# MySQL dump 6.0 # # Host: localhost Database: VSS #-------------------------------------------------------- # Server version 3.22.23b # # Table structure for table 'answers' # CREATE TABLE answers ( no int(11) DEFAULT '0' NOT NULL auto_increment, time int(11) DEFAULT '0' NOT NULL, category varchar(30) DEFAULT '' NOT NULL, subject varchar(50), questions text, answers text, PRIMARY KEY (no) ); # # Dumping data for table 'answers' # INSERT INTO answers VALUES (1,929488495,'Moons','Jupiter\'s moons','Dr. Shaw,\r\n\r\nSince I participated in the 90 min. interview for the research, I was wondering whether or not Jupiter\'s moons are comparable to a solar system. By the way, after being asked those questions, I have decided that you have your work cut out for you during the course of this class,.\r\n\r\nThank you,\r\nAmy Hamon \r\n','The formation and history of Jupiter\'s moons is one of those\r\nnice \'maybe it means somethings\'. See Seeds p509 for more.'); INSERT INTO answers VALUES (2,929488633,'moons','astronomy question','How many moons does Saturn have? \r\n','18 and counting'); INSERT INTO answers VALUES (3,929488707,'jupiter','Great Red Spot',' Dr. Shaw, \r\n\r\nWhat causes the Great Red Spot on the surface of Jupiter? I \r\nknow that the rotation of the planet might be one cause of the\r\nhuge storm, but what are some other ideas?\r\n','The Great Red Spot is a storm. Now if we just knew whay it was red....'); INSERT INTO answers VALUES (4,929488903,'eclipses','lunar eclipse','What is happening in the event of a lunar eclipse with respect to the position of the sun, Earth, and the moon? \r\n','I think you get a chance to answer that one yourself in Question 6. :-)'); INSERT INTO answers VALUES (5,929489082,'earth','EARTH\'S ROTATION','In what direction does the earth rotate? \r\n','The Earth\'s direction of rotation depends on which direction you look at it from. I could say prograde, but that would not be very informative. Counterclockwise as \r\nseen from the north. Of course, if you have a digital clock\r\nthat doesn\'t do you much good.'); INSERT INTO answers VALUES (6,929489365,'galaxies','Distance of nearest galaxy','How far away is the nesrest galaxy to us? \r\n','Of course we live in the Milky Way - but the next galaxies over are the Large and Small Magellanic Clouds. They\r\ncan be seen from the southern hemisphere. Quite a nice\r\nsight. They are about 150,000 light years away. Close\r\nby cosmic standards, but too far to walk.'); INSERT INTO answers VALUES (7,929489553,'tides','Class','Hello Dr. Shaw;\r\n\r\nHow does the moon affect the tides on Earth? WHat about on other planets? \r\n','Our moon is the major source of tides on the earth. Other\r\nmoons raise tides on other planets also and the planet raise\r\ntides on the moon. Of course, liquid and gas distorts\r\nmore easily than solid, so they show the tides better.'); INSERT INTO answers VALUES (8,929489666,'comets','Comets?',' \r\nAny coming by soon?','The current brightest comet is comet Lee. Soon maybe\r\na binocular object. A good souce for comet information is \r\nencke.jpl.nasa.gov'); INSERT INTO answers VALUES (9,929489829,'stellar evolution','random star stuff',' \r\nHow long until the star Antares explodes?\r\n','Ms. Russell, maybe you should be the one to answer this question. Less than a few hundred million years would be a \r\ngood guess.'); INSERT INTO answers VALUES (10,929489867,'solar system','How old is our solar system?',' \r\n','The solar system is 4.5 billion years old.'); INSERT INTO answers VALUES (11,929490068,'life off Earth','Astronomy','Do you think humans will be able to travel to and live on other planets in the next 20 years? \r\n','If we wanted to estabilsh a lunar base by 2020 we could.\r\nHowever, it would take a much bigger budget than NASA now\r\nhas, so I suspect it will be more like 50 years until\r\nwe are living anywhere off Earth but in space stations.\r\nI refer you to \'The Martian Chronicles\' for another view.'); INSERT INTO answers VALUES (12,929490132,'tides','tides vs phases of the moon','What actually causes the oceadntides to come and out?\r\nThank you... \r\n','Lunar gravity (mostly) solar gravity (some).'); INSERT INTO answers VALUES (13,929490184,'seasons','Earth\'s axis',' \r\nhow does the earth\'s axis effect the seasons? Does it?','You get to answer that one in Question 4.'); INSERT INTO answers VALUES (14,929490307,'Schedule','Observatory project question','How long will we have to observe the sky? Is \r\nthe observarory project a full semester project? \r\n','If the weather cooperates, I would like the observations turned in July 14. We will check them July 7th to see how it goes.'); INSERT INTO answers VALUES (15,929967976,'SS formation','How it all began.',' \r\nDr. Shaw,\r\nI understand how the universe got started in its formation with the\r\nsticking together of gas and dust particles, but what I wanted to know \r\nis how the nebula began to spin in the first place and \"stick\" together. You said in class that gravity pulled it all together, but where does that gravity come from in the first place? Thanks for your time...\r\n','Gravity is one of the four funadmental forces. All matter\r\nattracts every other piece of matter. WRT the solar nebula\r\nall the gas and dust attracts all the rest. Since there\r\nis a higher density in the center most of it \'falls\'\r\ntoward the center until it forms the sun. Some of it\r\nis swirling around and thsu has angular momentum. This\r\ncan opposed gravity and thus form a disk. It does not take much turbulence in a large cloud to give the amount of\r\nangular momentum in the solar system. Think of an ice\r\nskater with her arms out and how fast she \'spins up\'\r\nwhen she pulls them in. The could contracts from a few\r\n10 thousands of astronomical units to about 100. this \r\ncauses quite a bit of spin up.\r\n\r\nBTW be sure to use the terms solar system, Galaxy and universe correctly.\r\n'); INSERT INTO answers VALUES (16,930515248,'orbital elements','Question 5',' \r\nWe are having trouble finding the eccentricity of the moon. Where could we find that?\r\n\r\nAntares\r\n\r\n','http://csep10.phys.utk.edu/astr161/lect/time/moonorbit.html\r\nhas some information about the lunar orbit including\r\nthe eccentricity. I found it by searching on lunar orbit.'); # # Table structure for table 'notice' # CREATE TABLE notice ( no int(11) DEFAULT '0' NOT NULL auto_increment, time int(11) DEFAULT '0' NOT NULL, message text, PRIMARY KEY (no) ); # # Dumping data for table 'notice' # INSERT INTO notice VALUES (2,931350349,' \r\nWELCOME BACK!'); INSERT INTO notice VALUES (4,931782003,' \r\n7/12/99\r\n\r\nPlease write up all of your observations to be turned in by next MONDAY\r\n\r\nQuestion 6 (NEW)\r\n\r\nWhen and how do the solar and lunar eclipses occur?\r\n\r\nFirst: the current version of the software will NOT cast shadows! Therefore, you will have to investigate eclipses by observing when and how the sun is eclipsed and inferring that you are then in either full shadow (umbra) or partial shadow (penumbra.)\r\n\r\nYou may use the model from question 5 but make sure you have saved it to turn in.\r\nThis time you want to find waypoints very near the Earth [near E] looking back at the Sun and Moon and very near the Moon looking back at the Sun and the Earth (to see what the eclipse looks like) You might even find one above the Earth-Moon system [aboveEM] to be able to see how the eclipses occur over the entire year.\r\n\r\nRead up on the variety of lunar and solar eclipses.\r\n\r\nNote before starting: You will need a way to keep time, especially to determine the length of a year. One way to do this is to use the arrow texture on the object you are following (such as the moon) and set its rotation to one year (or 1/2 year or 1/4 year). You can then use the rotating image at the bottom right to tell time. Will this fake rotation effect any of your eclipse observations?\r\n\r\n1.\r\nInitially set the lunar orbit inclination to 0. \r\nBegin at the near Earth position and let the system move until you see an eclipse. Move back and forth during the eclipse and give a good description of what is going on. What do you see?\r\n\r\nSlowly let the Earth-Moon-Sun system move for a full year. How many eclipses do you see?\r\n\r\nMove the Moon\'s orbital inclination to its real value. Now what happens? How many eclipses do you see in one year? What type?\r\nTurn on \'orbital view\' [under view] describe the orbits during and eclipse. How often does the moon cross the ecliptic in one year? Why doesn\'t an eclipse occur every time the moon crosses the ecliptic? Hint: Back off and look at the entire lunar orbit.\r\n\r\nWhat is the line of nodes and what does it have to do with eclipses?\r\n\r\nChange the inclination of the lunar orbit to 60 degrees. Again, what happens to the number of eclipses per year and why?\r\n\r\nDoes the moon have to be exactly in the ecliptic to have an eclipse? What is the difference in the eclipse between \'almost\' and \'exactly\' in the ecliptic as we see it from Earth (or from the moon)?\r\n\r\nDuring the solar eclipse which direction is the Moon moving? Can you calculate how fast this is and therefore approximate how long an eclipse will take between first and fourth contact?\r\n\r\n2.\r\nNow move to the Moon and find an eclipse (you might want to go back to 0 inclination).\r\nWhat would you see from the Earth when you see a solar eclipse on the moon? Go through the same exercises from a lunar viewpoint as you did from the Earth.\r\nIn your comments emphasize the differences.\r\n\r\n3.\r\nStart with the official values of the Earth-Moon-Sun system. Now make the moon 10 time as large. How many eclipses do you see per year? What kinds? Why? \r\n\r\nMake the Sun 10 time as large. How many eclipses do you see per year? What kinds? Why?\r\nCan you make an annular eclipse of the Sun? [It is much easier to see this with the sizes exaggerated.]\r\n\r\nKeeping your lunar and solar sizes at 10 times, double the lunar distance. How many eclipses do you see per year? What kinds? Why? \r\n\r\n\r\n\r\n'); INSERT INTO notice VALUES (1,931375407,'This is a test message. This is used for test new function of daily message update. \r\n\r\nThe instructor\'s old messages will also be kept. The students can still see the old messages after the new message posts.\r\n\r\n\r\n'); INSERT INTO notice VALUES (3,931436102,' \r\nIn order to help you visualize the movement of the\r\nEarth and the Moon I have created a texture called\r\n\'arrow\'. Please get it from me via diskette. You can use this for seeing what you would see from a specific\r\nplace on the moon (or Earth). To change the direction of the arrow on the moon you can change the \'time of perihelion\' in its properties. (This does not work for the Earth and only works for the Moon it you have it moving correctly.)\r\n\r\nRemember, changing the size of an object can allow you to \r\nsee it better but does not change its orbital properties.\r\nIn order to compare synodic and sidereal periods of the Moon\r\nyou might watch the E-M system from new to new phase and\r\ncount the number of times the Earth rotates in that time.\r\n\r\nIf you did not show me your observations yesterday do so \r\ntoday\r\n'); INSERT INTO notice VALUES (5,931922186,' Talk to your group members an start thinking about\r\nwhich of the following projects you would like to do.\r\nOnly one project to a group. There are plenty to go around.\r\n\r\n***************************\r\nSome things to remember. Techniques which you used before:\r\n\r\n1. Start with real values\r\n2. Will changing a value to a fake on help you see something?\r\n A. Changing SIZE may change what you see but it will not effect orbital elements\r\n B. Changing rotation does not effect orbital elements\r\n C. You can use rotation rates as clocks (just as we do to keep time.)\r\n\r\nA new technique for seeing what something looks like as it moves through your sky.\r\n\r\nI t is based upon the same thing that allows you to have satellite TV reception. That is, if a TV company can orbit a satellite above the earth so that it stays stationary on the sky [a geosynchronous satellite] then we can put a false on in orbit and set a waypoint to track it and our view will move just as if we were looking at a fixed point in the sky.\r\n\r\nTo do this you will need to\r\n1. set a \'synchronous satellite around the planet from which you wish to view\r\n2. move close to the planet\r\n3. Set a waypoint, which follows the satellite.\r\n4. If you need to shift the satellite to another side of the planet just change its time of perihelion. (This should not be necessary.)\r\n5. It you need a planetary tilt, tilt the ORBIT of the satellite the same as the planet\'s tilt\r\n\r\nWhat are the orbital parameters of the satellite? To get them you will have to use Kepler\'s Third law relating the mass of the planet, the period of the orbit (= the planet\'s rotation to make the orbit synchronous) and the size of the orbit. Be careful. It you change the planet\'s mass you will change the orbit of every one of its other satellites!\r\n\r\n\r\n7. Model the retrograde motion of the sun as seen from Mercury. \r\nHow does the Sun seem to move in the Mercurean sky? How long is it between noon and noon on Mercury? (Count this in your model.) How is the motion different if the orbital eccentricity is 0.02 or .4?\r\n\r\nDescribe Mercury\' motion in the sky as seen from Earth. How far away from the Sun does it get (angular)? Be prepared to show how you measured this in your model. If you know how far away the Sun is, how can you convert this into the size of mercury\'s orbit?\r\n\r\n\r\n 8. Model the phases of Venus--geocentric and heliocentric orbits. \r\n\r\nGalileo used the changing phases of Venus to prove the heliocentric theory of the solar system. How does Venus change appearance as seen from Earth in a geocentric theory vs. a heliocentric one? Why did it take so long for this proof to be demonstrated? \r\n\r\n\r\n 9. Model the Martian moons.\r\n\r\nHow bright and how big would the Martian moons appear from the surface of Mars? Could you ever experience a total eclipse of the sun while standing on the surface of Mars? What is the difference between Earthly and Martian eclipses? Demonstrate the motion of the two moons across the Martian sky as seen from the (rotating) Martian surface\r\n\r\n\r\n 10. Model a mini solar system. \r\n\r\nSometimes Jupiter and the Galilean moons are said to resemble the solar system. To what extent is this true or untrue? Model the motion of the Galilean Moons as seen from Jupiter\'s surface (?) Can you get solar eclipses while on Jupiter? Do the Galilean moons ever eclipse each other as seen from the Earth?\r\n\r\n\r\n11. Model Uranus, Neptune and Pluto. \r\n\r\nWhy are Uranus\' seasons so vastly different than Earth\'s? How was the Uranian ring system discovered? Simulate this ring system using a fake satellite and its orbit painted in. Show how the discovery worked. \r\nWhen is Pluto closer to the sun than Neptune? When will this happen again? How close do these two planets come (real distance, not angular)?\r\n\r\n\r\n 12. Model Pluto\'s center of mass. \r\nWhy does Pluto \"wobble\" in its orbit? Can you set up the model to show this wobble? How do Pluto and its moon Charon orbit?\r\nHow, when and where do Plutonian eclipses occur? If so, when? What could we learn from such eclipses? Do they ever eclipse as seen from the Earth? \r\n\r\n\r\n\r\n 13. Model the newly discovered three-planet solar system. \r\n\r\nWhy/how is it different than our own? \r\n\r\n'); INSERT INTO notice VALUES (6,932041585,' \r\nQuestion 6 presentations today!\r\n\r\nI have tested the e-mail system for sending grades.\r\nIf you did not get a message on your private email let me know.\r\n\r\nThis weekend - Read Chapters 21-25. Be sure to look\r\nclosely at the planet(s) you might use in your project.\r\nTry to answer the handout questions. Come wih your own\r\nquestions Monday.'); # # Table structure for table 'questions' # CREATE TABLE questions ( no int(11) DEFAULT '0' NOT NULL, category varchar(18), subject varchar(30), content text, PRIMARY KEY (no) ); # # Dumping data for table 'questions' # INSERT INTO questions VALUES (1,'','','When you go home tonight, take a moment to look up into the night sky. Pick out a star. How big is that star? How do you conceive of a body so very far away from yourself? \r\nThe study of Astronomy introduces us to sizes, distances, and times far beyond our common, everyday experience. That star that you selected out of the night sky - let\'s say someone told you that it is roughly 1 million miles in diameter? How meaningful is that fact? Can you appreciate the size of that star any better? \r\n\r\nProbably not. In order to appreciate the size of the universe, we must understand the scale of the planets, the sun, and other bodies in relation to one another. \r\n\r\nWhat is the difference between the size of the sun, planets, the moon, asteroids, and comets? \r\nWith your team members, plan and build a model to illustrate the relative size of these bodies, demonstrating your comprehension of nature at its grandest scale. '); INSERT INTO questions VALUES (2,'','','Now that you have expanded your vision of the size of the sun, the planets, and other members of the universe, what about their distance? How far apart are the sun and the planets? \r\n\r\nIf you read in a book that the average distance of the planet Mercury from the sun is 0.387 AU, would you be able to picture that distance? Would you remember it? Of course not! \r\n\r\nBuild on the knowledge and skills gained through your first model-building experience. Join your teammates now in using the virtual reality tools available to you to represent the distance of the sun from the nine planets. '); INSERT INTO questions VALUES (3,'','','Astronomy is one of the oldest and most intriguing sciences. One needs only to look up on a clear night at the beauty of the star-filled sky to realize why this is so. \r\n\r\nThere are practical reasons for being drawn to the study of astronomy as well. For example, the Ancient Greeks knew about the connection between the seasons and the orientation of the Earth to the Sun. Furthermore, seafaring cultures were aware that the tides are influenced by the position of the Moon. For these and other reasons, a number of ancient civilizations placed great importance on astronomical observations, as is evidenced by the megalithic monuments they left behind. \r\n\r\nMost people, for example, are familiar with Stonehenge, an assembly of mammoth stones dotting the British Isles. These point to the locations where the Sun and the Moon rise and set at key times during the year, including the solstices and equinoxes. The great medicine wheel in Wyoming, constructed atop a windswept plateau by Native Americans, is another example. The wheel is a circular ring of stones which mark important astronomical events, such as the rising of bright stars and the Sun at the summer solstice. \r\n\r\nThese are but a few examples of how ancient astronomers, particularly those of Greece, handed down to us new and powerful way of thinking about the world. The Greeks, Native Americans, and others gave the first demonstrations that logic, reason, and mathematics can be used to discover and understand how the workings of the universe impact our experience of the world. This impact can be seen in the weather, the seasons, the tides and more. \r\n\r\nIn this section, your team mates and you will use the tools handed down to us by the ancients, plus some new ones, to examine relationships between the Earth, our Moon, and the Sun. First, let\'s take a closer look at how the relative positions of the Earth, Moon, and Sun effect our experience of the world as we progress through the calendar year. \r\n\r\nWith your team, plan for and build a model that answers the following question: Where are the earth, moon, and sun relative to each other on July 1, 1999 at 10 p.m.? \r\n'); INSERT INTO questions VALUES (4,'','','The seasons - winter, spring, summer, autumn - each of us probably has our favorite and that favorite may even change over time. Autumn treats us with a spectacle of colors, as the days grow shorter and temperatures cooler. To the delight of avid snow skiers, winter brings the cold, crisp air and, hopefully, a ton of fresh powder. \r\n\r\nAnd, so it goes, the change of the seasons, year after year. We become so accustomed to the cycle of seasons, we often forget to stop and think what is the cause for such dramatic changes in temperature, weather, and length of daylight? Where, when, and how are the seasons formed? '); INSERT INTO questions VALUES (5,'','','The Rubáiyát of Omar Khayyám\r\n\r\nFitzgerald, Edward (1809-1883) \r\n\r\nYon rising Moon that looks for us again- \r\n\r\nHow oft hereafter will she wax and wane; \r\n\r\nHow oft hereafter rising look for us \r\n\r\nThrough this same Garden-and for one in vain! \r\n\r\nThe excerpt from the poem above speaks to a phenomenon that continues to capture our attention today - the phases of our moon. How many times have you looked up into the night sky to admire the brilliance of the full moon or the seemingly perfect cut of a crescent? One does not have to be a poet to appreciate such a sight. \r\n\r\nOne does, however, have to be a bit of a scientist to understand it. What are the phases of the moon and how are they created? Does our planet earth have phases? If so, how are they formed? How about the sun? Does it have phases? How are they formed? \r\n\r\nAnswers to these questions are the impetus for your next model-building venture. '); INSERT INTO questions VALUES (6,'','','Solar and lunar eclipses have often been interpreted as bad omens. \r\n\r\nSeveral such eclipses, and the fear evoked by them, have actually had an impact on world history. A well-known Chinese example dates back to 1851 when the Manchu emperors were about to fall due to the Taiping Rebel Group. Western governments tried to support the Chinese Emperor, sending modern weapons and British and American officers. The General of this army was Charles Gordon, a military genius. \r\n\r\nOn a moonlit night in 1851, a rebel headquarter was to be attacked. Very unexpectedly, a lunar eclipse occurred shortly before the assault. The Chinese soldiers interpreted this event as a most evil sign and lost their fighting spirit. As a result, the attack failed, there were high casualties, and General Gordon suffered his first defeat. \r\n\r\nIf General Gordon could have predicted the occurrence of the eclipse in advance, would history have been rewritten? \r\n\r\nWhere, when, and how do solar and lunar eclipses occur? '); INSERT INTO questions VALUES (7,'','','Until as recently as the early 1960s, it was thought that Mercury\'s \"day\" was the same length as its \"year\" so as to keep that same face to the Sun much as the Moon does to the Earth. However, this belief was shown to be false by doppler radar observations. \r\n\r\nIt is now known that Mercury rotates three times in two of its years. To this day, Mercury is the only body in the solar system known to have an orbital/rotational resonance with a ratio other than 1:1. \r\n\r\nGiven this knowledge, an individual on the planet Mercury would observe some interesting movements of the Sun. How does the Sun seem to move in the Mercurean sky? '); INSERT INTO questions VALUES (8,'','','Born in Pisa in 1564, Galileo Galilei, although a student of medicine, was a mathematician at heart. In fact, he served as a professor of mathematics at the university at Padua for eighteen years. Through is work, Galileo introduced the world to a new way of knowing through the practice of science. \r\n\r\nIn the early 1600s, Galileo used the changing phases of Venus to support a heliocentric theory of the solar system. How does Venus change appearance as seen from Earth in a geocentric theory vs. a heliocentric one? \r\n\r\nModel the phases of Venus, geocentric and heliocentric orbits, to demonstrate this? \r\n\r\nWhy did it take so long for Galileo to demonstrate the phases of Venus and, thus, prove scientifically the Copernican universe? '); INSERT INTO questions VALUES (9,'','','Mars is the fourth planet from the Sun and the seventh largest. Though Mars is much smaller than Earth, its surface area is about the same as the land surface area of Earth. \r\n\r\nExcept for Earth,Mars has the most highly varied and interesting terrain of any of the terrestrial planets, some of it quite spectacular. For instance, Olympus Mons is the largest mountain in the Solar System rising 24 km (78,000 ft.) above the surrounding plain. Valles Marineris, a system of canyons, is approximately 4000 km long and from 2 to 7 km deep. \r\n\r\nIn addition to a dynamic terrain, Mars has two tiny satellites, Phobos and Deimos, which orbit very close to the surface. \r\n\r\nHow bright and how big would the Martian moons appear from the surface of Mars? \r\n\r\nCould you ever experience a total eclipse of the sun while standing on the surface of Mars? \r\n\r\nWhat is the difference between Earthly and Martian eclipses? \r\n\r\nModel Mars and its satellites to find out. '); INSERT INTO questions VALUES (10,'','','Jupiter has 16 known satellites-the four large Galilean moons and 12 small ones. Sometimes Jupiter and the Galilean moons are said to resemble the solar system. To what extent is this true or untrue? \r\n\r\nModel Jupiter and its major satellites to inform your answer. \r\n\r\nJupiter has a significant magnetic field, extending more than 650 million km in certain directions. The environment near Jupiter contains high levels of energetic particles trapped by Jupiter\'s magnetic field. This \"radiation\" is similar to that found within Earth\'s Van Allen belts.\r\n\r\nModel the Jovian radiation belts. How do the Jovian radiation belts differ from Earth\'s? '); INSERT INTO questions VALUES (11,'','','Uranus is the seventh planet from the Sun and has the third largest diameter. The character of its seasons is unique in the Solar System. Why are Uranus\' seasons so different? Model a comparison between the Earth and Uranus to determine how they differ. \r\n\r\nThe Uranian ring system was discovered in 1977. There are nine major rings surrounded by belts of fine dust. Working outward from the planet, they are named 6, 5, 4, Alpha, Beta, Eta, Gamma, Delta, and Epsilon. \r\n\r\nDemonstrate how the rings of Uranus were originally discovered. How much more difficult would this method of discovery have been for Jupiter\'s rings? \r\n\r\nThe eight planet, Neptune, has at least 10 moons and a set of rings. It is very similar in appearance to Uranus. Its discovery was predicted by observing inconsistencies in the orbit of Uranus as predicted by Newton\'s theory of gravity-a triumph for Newtonian physics! Neptune\'s outer neighbor, Pluto, has such an eccentric orbit that it is, at times, closer to the Sun. \r\n\r\nWhen is Pluto closer to the Sun than Neptune? When the two planets cross paths, how close do they come to one another? \r\n'); INSERT INTO questions VALUES (13,'','','Model the newly discovered three-planet solar system.\r\n\r\nWhy/how is it different than our own?'); INSERT INTO questions VALUES (12,'','','Pluto is named after the god of the underworld and, more indirectly, for the astronomer who predicted its existence-Percival Lowell. It is usually the farthest planet from the Sun, though its extremely elongated elliptical orbit sometimes places it inside the orbit of Neptune. \r\n\r\nThere is considerable debate about Pluto\'s status as a planet. There may be a number of large, ice-covered bodies similar to Pluto inhabiting the outer reaches of the solar system, and Pluto might be considered the largest of these, rather than the smallest of planets. Among its other eccentricities, its orbit is more inclined than the other planets and it \'wobbles\'. Why it wobbles is an interesting question. \r\n\r\nPluto has a recently discovered satellite, Charon. Some consider the Pluto/Charon system to b a double planet system rather than planet-moon one. \r\n\r\nHow do Pluto and its moon orbit? Do they ever eclipse as seen from the Earth? Is so, when? What could we learn from such eclipses? \r\n\r\nUse the virtual modeling software to answer these questions about Pluto and Charon. '); # # Table structure for table 'resources' # CREATE TABLE resources ( no int(11) DEFAULT '0' NOT NULL auto_increment, filename varchar(30) DEFAULT '' NOT NULL, size int(11) DEFAULT '0' NOT NULL, type varchar(30), category tinyint(4) DEFAULT '0' NOT NULL, question_no tinyint(4) DEFAULT '0' NOT NULL, owner_no tinyint(4) DEFAULT '0' NOT NULL, time int(11) DEFAULT '0' NOT NULL, PRIMARY KEY (no) ); # # Dumping data for table 'resources' # INSERT INTO resources VALUES (1,'1',46967,'',2,1,5,929545812); INSERT INTO resources VALUES (2,'Q1_SolarSystem_Size.ssf',5839,'',1,1,12,929717596); INSERT INTO resources VALUES (3,'Q2_SolarSystem_Dist.ssf',5839,'',1,1,12,929717615); INSERT INTO resources VALUES (4,'Group2-Q2.ssf',4874,'',1,2,8,929717776); INSERT INTO resources VALUES (5,'empty.html',129,'text/html',1,5,17,931292326); # # Table structure for table 'semail' # CREATE TABLE semail ( no int(11) DEFAULT '0' NOT NULL auto_increment, time int(11) DEFAULT '0' NOT NULL, name varchar(30), subject varchar(50), questions text, status char(1), PRIMARY KEY (no) ); # # Dumping data for table 'semail' # INSERT INTO semail VALUES (27,929718838,'Team 5','Question 1 report',' \r\nAstronomy 1010 6/18/99\r\n\r\nGroup 5\r\n\r\nQuestion 1:\r\n\r\n1. What is the difference between the size of the sun, planets, moons,\r\n asteroids, and comets?\r\n\r\nHow and why the sizes go to be the way they are. \r\nHow did Astronomers find the numbers?\r\n\r\nThe sun is the largest star in our solar system. Planets would be the next smaller in size ranging from the largest Jupiter at 71,494km (radius) to the smallest Pluto at 1151 km (radius). \r\n\r\nMoons are typically smaller than planets although there are several that are comparable in size to the smaller of the planets. \r\n\r\nAsteroids and comets are typically smaller than most moons and would be considered the smallest objects of the group in question. They have a wide range of size in their category.\r\n\r\nThe Terrestrial planets are made of heavier trace elements and thus were dense and had a low gravitational pull. They were also closest to the sun and this hotter temperature inhibited their growth by not allowing the gases to condense as rapidly as the outer cooler planets. The Jovian planets formed in the outer solar system where temperatures were much cooler. This allowed them to grow much more rapidly than the Terrestrial planets in size and mass. They were formed from the much more abundant hydrogen and helium gases. \r\n\r\nAstronomers looked at the planets through a telescope. They could determine the size of the planet relative to the lens size and power of magnification. By looking at the size of the planet through the telescope, they can use math equations to find the actual size.\r\n','R'); INSERT INTO semail VALUES (13,929454320,'heather Weekley','Earth\'s axis',' \r\nhow does the earth\'s axis effect the seasons? Does it?','R'); INSERT INTO semail VALUES (14,929454329,'Chris Edwards','tides vs phases of the moon','What actually causes the oceadntides to come and out?\r\nThank you... \r\n','R'); INSERT INTO semail VALUES (15,929454330,'Will Harrison','astronomy question','How many moons does Saturn have? \r\n','R'); INSERT INTO semail VALUES (16,929454333,'Melissa Womack','Astronomy','Do you think humans will be able to travel to and live on other planets in the next 20 years? \r\n','R'); INSERT INTO semail VALUES (17,929454337,'Matt Dockter','How old is our solar system?',' \r\n','R'); INSERT INTO semail VALUES (18,929454338,'Antares Russell','random star stuff',' \r\nHow long until the star Antares explodes?\r\n','R'); INSERT INTO semail VALUES (19,929454339,'susie hungerbuhler','Comets?',' \r\nAny coming by soon?','R'); INSERT INTO semail VALUES (20,929454339,'Natasha Brown','Observatory project question','How long will we have to observe the sky? Is \r\nthe observarory project a full semester project? \r\n','R'); INSERT INTO semail VALUES (21,929454342,'Irma Smith','Class','Hello Dr. Shaw;\r\n\r\nHow does the moon affect the tides on Earth? WHat about on other planets? \r\n','R'); INSERT INTO semail VALUES (22,929454342,'Julie Reitz','Distance of nearest galaxy','How far away is the nesrest galaxy to us? \r\n','R'); INSERT INTO semail VALUES (23,929454356,'Trey King','EARTH\'S ROTATION','In what direction does the earth rotate? \r\n','R'); INSERT INTO semail VALUES (24,929454370,'Brian Rawlings','lunar eclipse','What is happening in the event of a lunar eclipse with respect to the position of the sun, Earth, and the moon? \r\n','R'); INSERT INTO semail VALUES (25,929454380,'Jamie Dyer','Great Red Spot',' Dr. Shaw, \r\n\r\nWhat causes the Great Red Spot on the surface of Jupiter? I \r\nknow that the rotation of the planet might be one cause of the\r\nhuge storm, but what are some other ideas?\r\n','R'); INSERT INTO semail VALUES (26,929454958,'Amy Hamon','Jupiter\'s moons','Dr. Shaw,\r\n\r\nSince I participated in the 90 min. interview for the research, I was wondering whether or not Jupiter\'s moons are comparable to a solar system. By the way, after being asked those questions, I have decided that you have your work cut out for you during the course of this class,.\r\n\r\nThank you,\r\nAmy Hamon \r\n','R'); INSERT INTO semail VALUES (28,929718894,'Team 5','Question 2 report',' \r\nAstronomy 1010 6/18/99\r\n\r\nGroup 5\r\n\r\nQuestion 2:\r\n\r\n2. How far apart are the sun and the planets?\r\n\r\nHow and why the distances go to be the way they are. \r\n\r\nAnd how did astronomers find the numbers.\r\n\r\n\r\nThe first four planets are referred to as the Terrestrial planets. They are closest in distance to the sun and to one another. Mercury, the closest planet to the sun is 57.9 million km from the sun. As you pass the fourth planet (Mars) the distance to the next planet is great (approx. 500 million km). From the fifth planet (Jupiter) to the last planet (Pluto) the distances are much greater between the planets and also from the sun. This second group is called the Jovian planets. Pluto is 5.9 billion km from the sun.\r\n\r\nThe distances between planets is much greater in the Jovian planets than in the Terrestrial planets.\r\n\r\nWhen the planets formed, matter was spread equally outward from the sun. As this matter condensed into planets, each one pulled in as much surrounding matter as possible. As the objects grew in mass, their gravity increased, which in turn allowed them to pull in more matter. \r\n\r\nThe larger planets have a higher gravitational pull so they can pull in matter from farther away. This explains why the planets are far apart. One planet has an area of gravitational pull. The next planet must be outside of that to gather their own matter. The mass is directly responsible for the amount of gravitational pull a planet has, thus the larger, more massive planets are farther out and have more distance between them.\r\n\r\nAstronomers might measure the distance of a planet from Earth and then knowing the distance from the Earth to the Sun add the two together.\r\n','R'); INSERT INTO semail VALUES (29,929733338,'Chris Edwards','How it all began.',' \r\nDr. Shaw,\r\nI understand how the universe got started in its formation with the\r\nsticking together of gas and dust particles, but what I wanted to know \r\nis how the nebula began to spin in the first place and \"stick\" together. You said in class that gravity pulled it all together, but where does that gravity come from in the first place? Thanks for your time...\r\n','R'); INSERT INTO semail VALUES (30,929971193,'Team 3: Heather, Julie, Susan','Question summary for #1 and #2',' \r\n','R'); INSERT INTO semail VALUES (31,929972550,'Amy Hamon','Friday, June 18',' \r\nDr. Shaw,\r\nI apologize for missing class on June 18. I had a family emergency that required me to go home Thursday night and I did not get back in time for class. Again, I\'m sorry for the inconvenience dealing with the researchers, etc.\r\n\r\nThank you,\r\nAmy Hamon','R'); INSERT INTO semail VALUES (32,929973168,'Group 2','Q1-2-Report','How do astronomers find these numbers?\r\n -Astronomers find the size and distance numbers of planets, stars, moons, comets, and asteroids through science. Science is the process by which we look at data and search for relationships that tell us how nature works (Seeds 199). Science is based on evidence. Every theory and conclusion must be supported by evidence obtained from experiments or from observations (27). Hypothesis, theory, and natural law are key staples to the astronomer\'s diet. Hypotheses and theories are stories to help try to explain how nature works, but no scientific theory or hypothesis can be proved correct. The only way to arrive at facts is to consult nature and make direct measurements or observations; which is easy to say, but awful hard to accomplish. \"Measurement in astronomy is very difficult. It is impossible to measure directly simple parameters, like the diameter of a star. Simple observations that are possible, combined with the basic laws of physics are used to discover the properties of stars\" (167). To find the diameter of a star, you must first find the temperature and luminosity of a star. The astronomer\'s method, using the earth\'s orbit at two different points for the baseline, is also used. Another way to find the distance of stars is using the parallaxes for the closer stars and spectroscopic parallaxes for the more distant stars. If you can link the observable parameters step-by-step to the final conclusions, you will have gained a strong insight into the nature of science.\r\n\r\nHow accurate are these measurements?\r\n -\"Science is based on measurement, and whenever we make a measurement we should ask ourselves how accurate that measurement can be. The accuracy of the measurement is limited by the resolution of the measurement technique, just as the amount of detail in a photograph is limited by the resolution of the photo\" (109). Therefore, these numbers could never be 100% accurate unless we could travel to every place that we wanted to get a measurement from (minus the moon).\r\n\r\nWhy these distances, sizes, masses, rotation rates, etc.\r\n -Astronomer\'s use these numbers to build a model for us to better understand the universe we live in. \"A scientific model need not be right, but it must be useful. Scientist\'s use these models as mental crutches to help them think about nature. They are not so much searching for ultimate truths as they are trying to build better and better models of how nature works\" (15).\r\n\r\nHow arbitrary is all this?\r\n -Scientific explanations are attempts to describe how nature works based on fundamental rules of evidence. The power of science to shape our world can lead us to think that its explanations are unique. The process we call science depends on the use of evidence to test and perfect explanations, and the logical rigor of this process gives great confidence in the conclusions (581). This is very arbitrary to humans because we always want to know how and why something is. We can\'t seem to let nature run its course and just accept things for what they are.\r\n \r\n','R'); INSERT INTO semail VALUES (33,929973300,'Dr.Shaw','Question Description',' \r\n','R'); INSERT INTO semail VALUES (34,929973938,'Dr. Shaw','Group 1\'s project 1','In the first question we were asked to find the sizes of the sun, each of the planets, and two moons within our solar system. This we did by using the internet and the virtual reality software program called \"open skies\". After finding the masses, diameters, rotation rates, and tilts on astronomy internet sites, we plugged the values for each of these into the software program and were able to see the difference in the sizes. This was a truly amazing thing to be able to do. By using the open skies program we were able to see the amazing differences and similarities of the planets and the sun. We have always known that the sun was far larger in mass and diameter than any of the planets that orbit around it, but to virtually be able to see the difference made the concept more real to us. The only two problems we had with this project were learning how to use the software correctly and positioning the sun in the right place in relation to the rest of the planets. \r\n','R'); INSERT INTO semail VALUES (35,929973966,'Dr.Shaw','Question Description','As I go home to look at the star\'s they seem minute and ver insignificant to the moon. It is very hard to imagine that the very star that I am looking at might be ten times as big as the Earth beneath my feet. I can not really concieve of that star because to me it is just a little dot in the sky although I know in my mind it is actually a thousand times larger than what I percieve it to be. \r\nIf someone told me that the star was i million miles in diameter I would not, in fact, be able to really understand the true meaning of the in my mind, because even though I know a million is a big numebr, I can not see the image in my head. I can not appreciate the size of the star, because my eyes can only take in what it sees now, as opposed to what may be. Like you said, in order to appreciate the sixe of the universe, we must understand the scale of the planets, the sun, and other bodies in relation to one another.\r\nThe diffrence between the size of the sun, planets, the moon, asteroids, and comets vary. You find som ecomets tha are ever an astrnomical unit in length as well as some asteroids that are more than 100 kilometes (60 mi). The planets are a little bit easier to compare. The sun, compared to the rest of the planets, is quite larger than all of them.\r\n','R'); INSERT INTO semail VALUES (36,929975162,'Natasha Brown','Project 2','What struck us the most as we worked on the second question was the sheer grandeur of the model. In the first question, everything was close and the difference sizes were apparent. This did not seem as shocking until everything was to scale and Mercury was\'nt even visable next to the sun. We tried to get a feel for the distances and sizes by leaving Pluto and accelerating towards the sun, but we did\'nt take a path that showed us the other planets. Something else that was intersting was that Pluto and Charon were nearly on top of each other, while Earth and Luna were barley on the same screen. For the most part every other planet had its own screen and nothing else was visible. I think that\'s probably what impressed us the most, the vastness of space. Most things you see show the solar system on one page or screen, so seeing it to scale was elightening. \r\n','R'); INSERT INTO semail VALUES (37,929975374,'Group 1','grade','How exactly will we be graded on our projects and when can we expect our grades? I hope what we have is acceptable. Thanks for your time!\r\nGroup #1\r\n','R'); INSERT INTO semail VALUES (38,929976009,'Team #3','Question Summary #1 and #2',' \r\nFor question number one our team first decided to find the size, mass, orbit, and distance of each planet from the sun, and various moons. We collected the data from the resource pages under Nine Planets. We then entered the data into the template already provided for us in Open Skies.\r\n\r\nThrough many trial and errors, we were able to position the planets, sun, and moons all onto one screen. Our goal was to relate the size of each object with each other in an order. The order we chose was relative to the distance of each object from the sun. Therefore, Mercury, Venus, Earth, moon, Mars, Jupiter, Saturn, Uranus, Neptune, Pluto, and Charon; was the final order.\r\n\r\nAfrer creating each object, we found that the distances betweeen the planets was very important when attempting to view them on one screen. Some planets, for instance, Mercury, Venus, and Earth, appeared to be swallowed by the larger Jupiter. They disappeared in the screen when they were too close. To correct this problem we used a formula: \r\n distance from sun to planet + radius of planet + (arbitrary number)\r\nto create an appropriate distance between the planets. (see data below)\r\n\r\nIn order to consistantly view the final outcome of our project, we created a waypoint,\"view from the sun.\" When activated, the waypoint displays the sun and the nine planets from a diagonal vantage point of the sun. The sun appears in the far west of the screen with the planets trailing off northeasterly.\r\n\r\nWith the available data and software our group was able to create a model solar system that demonstrated the scale needed to appreciate the size of each planet.\r\n\r\n \r\nPLANETS MASS (kg) DIAMETER (km) ORBIT (km)\r\nMercury 1.99E+33 1390000 \r\nVenus 4.87E+24 12103.6 10820000\r\nEarth 5.97E+24 12756.3 149600000\r\nMoon 7.35E+22 3476 149984400\r\nMars 6.42E+23 6794 227940000\r\nJupiter 1.90E+27 142984 778330000\r\nSaturn 5.68E+26 120536 142940000\r\nUranus 8.68E+25 51118 2870990000\r\nNeptune 1.02E+26 49532 4504000000\r\nPluto 1.27E+22 2274 5913520000\r\nCharon 1.90E+21 1172 19640 (f. pluto)\r\nSun 1.99E+33 1390000 \r\n\r\nWhen we compared the sizes of the sun, moons, asteroids, and comets, we found the order to be: Sun, Jupiter, Saturn, Uranus, Neptune, Earth, Venus, Mars, Mercury, Large satellites i.e. Titan, Pluto, smaller satellites, asteroids, comets.\r\n\r\nWe hypothesized that the way scientists are able to derive the sizes and distances of the planets was through powerful telescopes, roaming probes, satellites, and basic knowledge of physic, mathmatics, light, and science. Tycho Brache was a scientist in the sixteenth century who observed the sky for 20+ years and determined arc and angular measure, which enabled him to begin thinking about relative distances and orientations. His data along with Galileo\'s (first to look through a telescope) aided Kepler and future scientists to create 3 laws of planetary motion (Principles of Astronomy, 174-7).\r\n\r\nQuestion Number 2\r\nWhen we constructed our 2nd solar system, we began with the our solar system from question 1 and simply changed the distances in volved to the accurate ones listed above. We once again created a waypoint (Sun?2) at the sun so one is able to view the planets in a straight line. We were only able to put a few of them on the screen. To view the farther out ones, it is necessary to back up farther or follow (with the F key) the outter most planets. The second system was much easier and faster to create based on previous knowledge of the software and having the planets and their masses already created. (See data sheet above for distances from sun.) We also found all of our distances through the Resource site, Nine Planets. ','R'); INSERT INTO semail VALUES (39,930057803,'Amy, Jamie, Melissa','Question 1 report',' \r\nAstronomy 1010 6/18/99\r\n\r\nGroup 5\r\n\r\nQuestion 1:\r\n\r\n1. What is the difference between the size of the sun, planets, moons,\r\n asteroids, and comets?\r\n\r\nHow and why the sizes go to be the way they are. \r\nHow did Astronomers find the numbers?\r\n\r\nThe sun is the largest star in our solar system. Planets would be the next smaller in size ranging from the largest Jupiter at 71,494km (radius) to the smallest Pluto at 1151 km (radius). \r\n\r\nMoons are typically smaller than planets although there are several that are comparable in size to the smaller of the planets. \r\n\r\nAsteroids and comets are typically smaller than most moons and would be considered the smallest objects of the group in question. They have a wide range of size in their category.\r\n\r\nThe Terrestrial planets are made of heavier trace elements and thus were dense and had a low gravitational pull. They were also closest to the sun and this hotter temperature inhibited their growth by not allowing the gases to condense as rapidly as the outer cooler planets. The Jovian planets formed in the outer solar system where temperatures were much cooler. This allowed them to grow much more rapidly than the Terrestrial planets in size and mass. They were formed from the much more abundant hydrogen and helium gases. \r\n\r\nAstronomers looked at the planets through a telescope. They could determine the size of the planet relative to the lens size and power of magnification. By looking at the size of the planet through the telescope, they can use math equations to find the actual size.\r\n','R'); INSERT INTO semail VALUES (40,930057856,'Amy, Jamie, Melissa','Question 2 report','Astronomy 1010 6/18/99\r\n\r\nGroup 5\r\n\r\nQuestion 2:\r\n\r\n2. How far apart are the sun and the planets?\r\n\r\nHow and why the distances go to be the way they are. \r\n\r\nAnd how did astronomers find the numbers.\r\n\r\n\r\nThe first four planets are referred to as the Terrestrial planets. They are closest in distance to the sun and to one another. Mercury, the closest planet to the sun is 57.9 million km from the sun. As you pass the fourth planet (Mars) the distance to the next planet is great (approx. 500 million km). From the fifth planet (Jupiter) to the last planet (Pluto) the distances are much greater between the planets and also from the sun. This second group is called the Jovian planets. Pluto is 5.9 billion km from the sun.\r\n\r\nThe distances between planets is much greater in the Jovian planets than in the Terrestrial planets.\r\n\r\nWhen the planets formed, matter was spread equally outward from the sun. As this matter condensed into planets, each one pulled in as much surrounding matter as possible. As the objects grew in mass, their gravity increased, which in turn allowed them to pull in more matter. \r\n\r\nThe larger planets have a higher gravitational pull so they can pull in matter from farther away. This explains why the planets are far apart. One planet has an area of gravitational pull. The next planet must be outside of that to gather their own matter. The mass is directly responsible for the amount of gravitational pull a planet has, thus the larger, more massive planets are farther out and have more distance between them.\r\n\r\nAstronomers might measure the distance of a planet from Earth and then knowing the distance from the Earth to the Sun add the two together.\r\n \r\n','R'); INSERT INTO semail VALUES (41,930149133,'matt dockter','concerns','sorry for all my questions regarding how you want things answered, i suppose i ought to know - but sometimes things seem so vague to me that i require some sort of clarification. i still don\'t know if my group members and i are on the right track as far as our projects go (what you want us to get out of them), it seems like all we do (gr. 2) is put things in - and most of the time we don\'t know the right reason(s) why they are that way. we cleared up the confusion on the write-ups, but we still might be struggling on the visual side. i am having a hard time switching my way of thought from the economics side of things to the astronomical side of things. any recommendations would be very helpful - i really do like your personality and teaching style and i think you would be a great instructor in any subject.\r\n\r\n sincerely,\r\n matt\r\n','R'); INSERT INTO semail VALUES (42,930238615,'GROUP 2 MATT,WILL,TREY','QUESTION 4',' \r\nQ4-2-Report (Trey, Will, and Matt)\r\n\r\n\r\nA.Where are the seasons formed?\r\n\r\n The locations of the seasons are formed because the earth is inclined to respect to the celestial equator. The sun spends half the year in the northern celestial hemisphere and half the year in the southern celestial hemisphere. If the sun\'s position is in the northern celestial hemisphere the northern celestial hemisphere is warmer. The seasons in the southern half of the earth are opposite of what the northern half is experiencing. \r\n\r\n \r\nB. When are the seasons formed ?\r\n\r\n The earth spins eastward on its axis once per day. While this motion is taking place, the sun is also moving slowly eastward along the ecliptic (the sun\'s apparent path around the sky) about 1 degree per day. The earth\'s axis of rotation is tipped 23.5 degrees from the ecliptic. The celestial equator is the projection of the earth\'s equator and the ecliptic is the projection of the earth\'s orbit. Because the earth is tipped 23.5 degrees, its equator is also tipped 23.5 degrees from the plane of the earth\'s orbit. Thus, the ecliptic and the celestial equator meet at an angle of 23.5 degrees. Due to this angle, the earth passes through a yearly cycle of seasons. Of the four systems, two of them begin when the ecliptic (sun\'s path through sky) crosses the celestial equator - this intersection of the two paths are called equinoxes (vernal and autumnal). The other two seasons begin when the ecliptic hits its most northerly and southerly points, called solstices (summer and winter). \r\n Viewed from North America, the vernal equinox (spring) is the point where the sun crosses the celestial equator moving northward - this happens around March 21. The summer solstice (summer) is the point in the sky where the sun is the furthest north on the ecliptic - this happens around June 22. The autumnal equinox (autumn/fall) is the point where the sun crosses the celestial equator moving southward - this happens around September 22. The winter solstice (winter) is the point in the sky where the sun is the furthest south on the ecliptic - this happens around December 22.\r\n\r\n\r\nC. How are the seasons formed?\r\n\r\n The cycle of the seasons occurs because Earth\'s axis is inclined 23.5 degrees from the perpendicular to its orbit. As earth orbits the sun, its axis remains pointing in the same direction in space. The seasonal temperature depends on the amount of heat we receive from the sun. The ecliptic is a major factor in determining the seasons. The motion of the sun around the ecliptic tips the heat balance one way in summer and the opposite way in winter. When the sun is in the northern celestial hemisphere, the northern half of earth receives more direct sunlight than the southern half. When the sun is in the southern celestial hemisphere, the northern half of earth receives more direct sunlight. The beginnings of the seasons are defined at four points along the ecliptic the vernal equinox, the summer solstice, the autumnal equinox, and the winter solstice. The seasons are not caused by changes by changes in the distance from the earth to the sun.\r\n\r\n\r\nObservation using Open Skies of the Earth at :\r\n\r\n1. 0 degrees - Sun light rays are parallel to the earth\'s equator. The seasons are the same for both northern and southern hemispheres.\r\n\r\n2. 60 degrees - The earth is now tilted with the pole at a greater angle. The seasons will now be more dramatic in the northern and southern hemispheres.\r\n\r\n3. 90 degrees - The sun\'s rays are now perpendicular the earth\'s equator. The north and south poles are now in the position of the equator at a 0 degrees tilt. The polar ice caps should melt and lead to flooding. \r\n\r\n\r\n**PLEASE NOTE: The texture used in our Solar Model was the \"earth4by8\" This gives greater definition to the project.\r\n\r\n\r\n1. How does the lighting change on the globe looking down from above on the earth ?\r\n\r\nThe visual image is half dark and half light.\r\n\r\n2. How does the lighting change viewed from North and South ?\r\n \r\nThe visual lighting image changes are the earth revoles as seen from the North pole.\r\n\r\n \r\n','R'); INSERT INTO semail VALUES (43,930317243,'Group 1','Question 4 discussion',' \r\nGroup 1\r\nAntares, Brian, and Natasha\r\nQuestion 4\r\n\r\nHow do seasons occur on Earth?\r\n Seasons depend on the amount of heat the Earth gets from the sun. Constant temperature occurs when the Earth receives and gives off an equal amount of heat. Because of the Earth’s tilt, the northern celestial hemisphere is in direct sunlight for six months; and the southern celestial hemisphere the other six months. There are four checkpoints on what we see as the sun’s path that determines the beginning of the seasons:\r\n *Vernal equinox-the sun moves northward across the celestial equator\r\n *Summer solstice-the northernmost point of the sun\r\n *Autumnal equinox-the sun moves southward across the equator\r\n *Winter solstice-the southernmost point of the sun\r\nDirect sun means the sun is hitting the Earth straight on and not at an angle. \r\n\r\nHow does lighting change over the year?\r\n At some points of the year the northern celestial hemisphere receives direct sunlight, at others the southern celestial hemisphere receives sunlight because of the angle of the Earth in comparison to the ecliptic path.\r\n\r\nWith texture and without, where is earth brightest and dimmest?\r\n The Earth is brightest whenever and wherever it is receiving direct sunlight, and dimmest where it is shadowed by the mass of the Earth. Normally the South Pole is in darkness and the equator is brightest and –45 degrees is in between. Therefore this area is in twilight, the place between brightness and darkness.\r\n\r\nThe Earth’s normal tilt is 23.45 degrees. When observed at a tilt of 90 degrees, there are still four seasons but day and night are different. The ecliptic path follows the poles vertically, that is, perpendicular to the equator. Both poles have a period of direct sunlight. At a tilt of 0 degrees, light follows the Earth’s rotation of the poles. At 50 degrees, both poles get more sunlight, and the ecliptic path crosses the equator.\r\n\r\nThe waypoint of our project is at 178 degree roll, 3.5 degree pitch, and .8 degree yaw. If you roll to 156.2 degrees roll, you will see the north and south pole aligned vertically. As you look from Earth the sun rotates 156.2 degrees and appears to move across the sky from northwest to southeast.\r\n\r\n\r\n','R'); INSERT INTO semail VALUES (44,930320587,'Group 3','project #4 questions',' \r\nGroup 3\r\nSusie, Heather, and Julie\r\nProject 4\r\n\r\nCreating the Solar System:\r\n When we created the Solar System for Project 4, we put the earth at its correct distance from the sun. If we focus on the earth we are able to see the sun rotate around it. This is the same view that we see from the earth. We created a waypoint at q4way1 which shows the sun moving around the earth; both sun and earth are on the same plane. In order to see what occurs when we change the tilt to 0 degrees, go under edit and change tilt from 23.5 to 0. With the tilt at 0 degrees, we conclude that all places on the earth would receive the same amount of sunlight all the time. The sunlight would hit most directly at the equator. As you went north or south it would become cooler. However as the sun spins around the earth the side of the earth that does not receive direct sunlight is in winter. As the sun moves into the area that is experiencing winter, the areas of milder temperature come into spring. As the sun leaves the area experiencing summer they enter into fall in the milder temperature regions. If we change the tilt 50 degrees we see that we would continue to have seasons except that it would be warmer during the summer at more northern latitudes, thus, ice caps would not exist. When it is summer in the Southern Hemisphere, the more southern latitudes are warmer than they would be today. The opposite is true during winter; the more northern and southern latitudes are colder than today. If the tilt is 90 degrees we see that the polar regions receive the direct sunlight. For example, if the North Pole is left and South Pole is right, and the sun is on the left, then the North Pole would have 6 months daylight and the South Pole would have 6 months darkness. As you go up and down longitude lines it would become cooler. \r\n The cycle of seasons occurs because earth\'s axis inclined at 23.5 degrees from the perpendicular to its orbit. It moves slowly but the axis is fixed in space for periods as short as a human lifetime. As earth circles the sun, its axis remains pointing in the same direction in space. On one side of the sun (left), earth\'s Northern Hemisphere is inclined toward the sun, and northern latitudes experience summer because they receive the most direct sunlight. 6 months later, earth is on the other side of the sun (right), and the Northern Hemisphere is inclined away, and northern latitudes experience winter. The seasons are reversed in southern latitudes. \r\n The length of daylight is based on the apparent rising and setting of the sun. As the earth spins eastward it appears that the sun moves in an east to west direction which is called the ecliptic. There are 4 locations along the ecliptic. They show the beginning of the seasons. They are the vernal equinox, summer solstice, autumnal equinox, and the winter solstice. During the equinox the sun is directly above the earth\'s equator and there is equal day and night. The vernal equinox occurs on March 20 or 21 and marks the beginning of spring (the sun begins to illuminate the side of the earth experiencing winter). The autumnal equinox occurs on September 22 or 23 and marks the beginning of fall. Because the earth\'s orbit is elliptical, the earth moves faster as it gets closer to the sun. Therefore the time interval between March and September is longer than between September to March. The distance between the sun and earth is shortest in January, meaning the earth completes its semicircle from September equinox to March equinox faster than March to September (www.worldbook.com). The solstices mark the most northerly and southerly points. The summer solstice is the point on the ecliptic where the sun is farthest north. The winter solstice is the place on the sky where the sun is farthest south . Average daytime temperature leads to the change in the seasons. \"The amount of heating that the earth receives in a single day throughout the year, and this depends on how many hours the sun is above the horizon and exactly how long it spends at its highest elevation above the horizon. The higher the sun gets, the less slanted the rays of light are that intercept each square meter, and so the efficiency with which these slanted rays can deliver energy to the surface gets better and better the higher up the sun gets.\" (Ask a NASA Scientist)\r\n The summer sun is above the horizon for more hours each day than the winter sun. Summer days are long and winter days are short. Because the sun is above the horizon longer in the summer, we receive more energy each day. The sun is highest in the sky at noon on a summer day. It shines almost straight down. On a winter day, the noon sun is low in the southern sky. The ground therefore, gains less heat from the winter sun because the sunlight hits the ground at an angle and spreads out. These two effects create the differences in the heat balance on the earth and cause the seasons (Foundations of Astronomy).\r\n Side note: Our textures were erased. The texture we used included the longitude,latitude, and equator (earth4x8). Please use this texture when refering to our solar system.\r\n','R'); INSERT INTO semail VALUES (45,930320723,'Team 5','Question 4 report',' Astronomy 1010 6/24/99\r\n\r\nGroup 5\r\n\r\nQuestion 4:\r\n\r\nWhere, when, and how are the seasons formed?\r\n\r\n\r\nWhere: The seasons are formed on the earth as the sun shines upon it from its various locations along the ecliptic. The seasons are most pronounced at the North and South Poles and become less pronounced as you near the equator. \r\n\r\nWhen: The change of season is noted by the movement of sunlight across each of the four points on the ecliptic. Spring is called the Vernal Equinox and is characterized by equal amounts of daylight and darkness. The sun is moving toward the Northern Hemisphere. Fall is called the Autumnal Equinox and is also characterized by equal amounts of daylight and darkness, but the sun is moving toward the Southern Hemisphere.\r\n\r\nSummer is called Summer Solstice and is characterized by the sun predominantly shining in the Northern Hemisphere creating more daylight and less darkness. Winter is called Winter Solstice and is characterized by the sun predominantly shining in the Southern Hemisphere creating more darkness than daylight.\r\n\r\nHow: The seasons are formed as the earth revolves around the sun. Due to the tilt of the earth, the seasons are formed as the sun shines on the Northern and Southern hemispheres from along the ecliptic. \r\n\r\nFollow the earth. How does the lighting change over the year? \r\n\r\n As stated above, the amount of light changes as the seasons change and also as we have day and night.\r\n\r\nWhere is the earth brightest and where dimmest and when?\r\n\r\nThe earth is brightest at any location that the time is 12:00 p.m. (noon). It is the dimmest at any location where the sun is rising (dawn) and setting (dusk). \r\n \r\nWhat about the \"in between\"?\r\n\r\nFor example: At sunrise, the sun is the most indirect and the dimmest. From this point until 12:00 noon the sun is getting more direct and brighter. This is the \"in between\" stage from dimmest to brightest.\r\n\r\nAt 0º the change is:\r\n\r\nThe sun shines equally in the northern and southern hemispheres.\r\n\r\n\r\nAt 50º the change is:\r\n\r\nMore noticeable at the north and south poles. At 23.5º they have mostly indirect sunlight. At 50º they have complete sunlight at various times. \r\n\r\n\r\nAt 90º the change is:\r\n\r\nDramatic. The equator is now straight up and down. The north and south poles are now the most direct point where sunlight hits when the sun is shining on their hemisphere. \r\n\r\n\r\nDescribe the motion of the sun in the Earth\'s sky when the Earth is aligned NS.\r\n\r\nThe sun shines most directly on the equator and diffuses equally into the northern and southern hemispheres\r\n\r\n','R'); INSERT INTO semail VALUES (46,930321475,'Antares Russell','Question 5',' \r\nWe are having trouble finding the eccentricity of the moon. Where could we find that?\r\n\r\nAntares\r\n\r\n','R'); INSERT INTO semail VALUES (47,931959146,'Team 5','Individual Group Project Choice',' \r\nNumber 10 is our first choice and number 13 is a second choice. ','R'); INSERT INTO semail VALUES (48,932046345,'group 3','project 7 choices','\r\nWe would prefer to choose from a) 9-pluto b)11-uranus c)10-jupiter.\r\nThanks.','R'); # # Table structure for table 'showcase' # CREATE TABLE showcase ( no int(11) DEFAULT '0' NOT NULL auto_increment, filename varchar(30) DEFAULT '' NOT NULL, size int(11) DEFAULT '0' NOT NULL, type varchar(30), question_no tinyint(4) DEFAULT '0' NOT NULL, team_no tinyint(4) DEFAULT '0' NOT NULL, time int(11) DEFAULT '0' NOT NULL, report text, PRIMARY KEY (no) ); # # Dumping data for table 'showcase' # INSERT INTO showcase VALUES (1,'1.ssf',4870,'',1,5,929717852,NULL); INSERT INTO showcase VALUES (2,'qst2.ssf',5967,'',2,5,930233966,NULL); INSERT INTO showcase VALUES (3,'Solar System#1.ssf',7388,'',1,3,929978035,NULL); INSERT INTO showcase VALUES (4,'Question2-2.ssf',6714,'text/plain',2,1,929976597,NULL); INSERT INTO showcase VALUES (5,'Solar System #2.ssf',6953,'',2,3,929974070,NULL); INSERT INTO showcase VALUES (6,'Group2-Q1.ssf',5529,'',1,2,929975613,NULL); INSERT INTO showcase VALUES (7,'Group2-Q2.ssf',5546,'',2,2,929975877,NULL); INSERT INTO showcase VALUES (8,'question 4.doc',46592,'application/msword',1,4,930235901,NULL); INSERT INTO showcase VALUES (9,'QUESTION1.SSF',6609,'',1,1,929976550,NULL); INSERT INTO showcase VALUES (10,'question 4.doc',46592,'application/msword',4,4,930236435,NULL); INSERT INTO showcase VALUES (11,'Group2-Q4.ssf',1942,'',4,2,930238105,NULL); INSERT INTO showcase VALUES (12,'Solar System#4.ssf',1783,'',4,3,930238151,NULL); INSERT INTO showcase VALUES (13,'Question4.ssf',1657,'',4,1,930317457,NULL); INSERT INTO showcase VALUES (14,'4.ssf',2352,'',4,5,930318812,NULL); INSERT INTO showcase VALUES (15,'astlab.gif',11382,'image/gif',5,6,931292241,' Astronomy 1010 6/24/99\r\n\r\nGroup 5\r\n\r\nQuestion 4:\r\n\r\nWhere, when, and how are the seasons formed?\r\n\r\n\r\nWhere: The seasons are formed on the earth as the sun shines upon it from its various locations along the ecliptic. The seasons are most pronounced at the North and South Poles and become less pronounced as you near the equator. \r\n\r\nWhen: The change of season is noted by the movement of sunlight across each of the four points on the ecliptic. Spring is called the Vernal Equinox and is characterized by equal amounts of daylight and darkness. The sun is moving toward the Northern Hemisphere. Fall is called the Autumnal Equinox and is also characterized by equal amounts of daylight and darkness, but the sun is moving toward the Southern Hemisphere.\r\n\r\nSummer is called Summer Solstice and is characterized by the sun predominantly shining in the Northern Hemisphere creating more daylight and less darkness. Winter is called Winter Solstice and is characterized by the sun predominantly shining in the Southern Hemisphere creating more darkness than daylight.\r\n\r\nHow: The seasons are formed as the earth revolves around the sun. Due to the tilt of the earth, the seasons are formed as the sun shines on the Northern and Southern hemispheres from along the ecliptic. \r\n\r\nFollow the earth. How does the lighting change over the year? \r\n\r\n As stated above, the amount of light changes as the seasons change and also as we have day and night.\r\n\r\nWhere is the earth brightest and where dimmest and when?\r\n\r\nThe earth is brightest at any location that the time is 12:00 p.m. (noon). It is the dimmest at any location where the sun is rising (dawn) and setting (dusk). \r\n \r\nWhat about the \"in between\"?\r\n\r\nFor example: At sunrise, the sun is the most indirect and the dimmest. From this point until 12:00 noon the sun is getting more direct and brighter. This is the \"in between\" stage from dimmest to brightest.\r\n\r\nAt 0º the change is:\r\n\r\nThe sun shines equally in the northern and southern hemispheres.\r\n\r\n\r\nAt 50º the change is:\r\n\r\nMore noticeable at the north and south poles. At 23.5º they have mostly indirect sunlight. At 50º they have complete sunlight at various times. \r\n\r\n\r\nAt 90º the change is:\r\n\r\nDramatic. The equator is now straight up and down. The north and south poles are now the most direct point where sunlight hits when the sun is shining on their hemisphere. \r\n\r\n\r\nDescribe the motion of the sun in the Earth\'s sky when the Earth is aligned NS.\r\n\r\nThe sun shines most directly on the equator and diffuses equally into the northern and southern hemispheres\r\n\r\n'); INSERT INTO showcase VALUES (16,'Q5Group4MoonPhases.ssf',4221,'',5,4,931445736,'Team 4\r\n07.08.1999 \r\n\r\n\r\n\r\nPhases of the Moon:\r\n The Moon rotates one revolution around the Earth every 27.321661 days, or one sidereal period. Sidereal periods are the complete rotations around the Earth as related to the background of the stars. In other words, one sidereal period is how long it takes the Moon to move from one point in the sky, through one revolution, and back to that same point in the sky. Every 24 hours the Moon moves about 13 degrees eastward in the sky, or about 0.5 degrees per hour. The orbit of the Moon is tilted 5 degrees 9 minutes in relation to the Earth\'s orbit around the Sun and it can never wander more than 5 degrees 9 minutes from the north or south of the ecliptic. During this sidereal period of the Moon the Earth also moves along it\'s orbit causing the Sun to move eastward along the ecliptic. Due to this movement the Moon actually needs a little over 2 days to get back to the same spot in the sky, with relation to the Sun, and begin the phases over again. This period, of 29.5305882 days, is known as one synodic period, which as opposed to the motion of the Moon with respect to the stars, is the motion of the Moon with respect to the Sun. \r\nAs the Moon moves through the sky night after night, we see the same side of it at all times. This is because the Moon rotates, on it\'s axis, in the same direction as the Earth, counter clockwise from the North Pole. At the same time the orbit around the Earth is in a counterclockwise direction, so that if a point on the Moon is facing the Earth it is always facing the Earth. This also explains the eastward movement through the sky. As the Moon orbits the Earth, with the same side always facing the same way, the light from the Sun is cast onto the Moon, thus causing the Moon to glow from the reflection of the light. Through one sidereal period, the amount of visible light cast onto the Moon changes. When the Moon is in the northern most sky, the side facing the Earth is the side directly behind the side facing the Sun, so that no glow is seen from Earth. As the Moon moves the amount of glow seen becomes greater and greater until the Moon moves into the southern most point in the sky which is when the side facing the Sun is also facing the Earth, causing what we call a full Moon. This is when the amount of glow begins to decrease until the Moon comes back to due North and no glow can be seen. These increases and decreases in the amount of glow is what causes the Moon to appear as a crescent. As the Moon goes from new, in the northern sky, to first quarter, in the eastern sky, the crescent is said to be a waxing crescent, and as it goes from first quarter to full, in the southern sky, it is said to be waxing gibbous. The Moon then begins to appear smaller each night and as it moves from full to third quarter, in the western sky, it is said to waning gibbous. Then as it goes back to new, it is said to be a waning crescent. This cycle from new back to new is known as the synodic period and it takes about 2 weeks to go from new to full. So as the sun moves from new to full it is said to be waxing and as it moves from full to new it said to be waning. The amount of glow determines whether or not it is said to be gibbous for more glow, or crescent for less glow. At new moon, the Moon is almost inline with the Sun so it sets in the west with the Sun and no Moon is seen. As it gets to full it begins to set later each night and when full it rises in the east at sunset and sets in the west at sunrise. At some phases the Moon is visible during the day. For example, when the Moon is in the waxing gibbous phase it rises just before sunset and at the waning gibbous phase it can be seen in the morning sky.\r\nAny object that reflects light has a phase. If you were standing on the Moon then the Earth would appear in phases due to the amount of light being reflected. The same effects that appear on the Moon, from Earth, would appear on the Earth from the Moon and if the Moon is full on Earth then the Earth is new on the Moon. If the Moon is new on Earth the Earth is full on the moon. The only difference is the Moon is always facing the same way towards the Earth so ( I think ) you could always see the Earth in the sky. The amount of glow would be different, but you could always see it if you were on the correct side of the Moon and the Earth would seem to rise, or would have more glow when your point on the Moon was a crescent ( or 90 degrees to the Sun\'s light ). This would give rise to the question of whether or not the Sun has phases. If the Sun has light cast onto it from another object then it has a phase in relation to that object. Though it might be hard to see since so much light is coming from the Sun. As I stated before any object that rotates and has light cast onto it by another object has phases.\r\n\r\n\r\n\r\nWaypoints\r\n\r\n Around-The-Moon:\r\nShows the Moon as seen from between the Earth and Moon. The Sun can be seen moving across the screen and the glow of the Moon changes as the moves around. Earth can also be seen.\r\n\r\n Earth-From-Moon:\r\nShows the phases of the Earth as seen from the Moon. It follows the Earth through the sky and the glow changes accordingly. When the Moon is full the glow on the Earth is the least and when the Earth has the most glow, or is full, the Moon is in its new phase. \r\n \r\n Moon:\r\n Same as Around-The-Moon only farther away.\r\n\r\n Moon-From-Earth:\r\nShows the Moon as it rotates around the earth. The Sun can be seen every new moon and as it moves eastward (from the Earth) the phases change. This is how the glow changes as the Moon makes a complete orbit. This shows the synodic period.\r\n'); INSERT INTO showcase VALUES (17,'group3project5.ssf',5567,'',5,3,931446765,'Group 3\r\nJulie, Susie, and Heather\r\nQuestion #5\r\nThursday, June 8, 1999\r\n\r\nHow are the phases of the moon created: The phases of the moon are created by the varying amounts of sunlight that reach the side of the moon facing the earth. The moon passes through eight phases in a counterclockwise motion around the Earth: New, Waxing Crescent, First Quarter, Waxing Gibbous, Full, Waning Gibbous, Third Quarter, Waning Crescent. When the moon is between the Earth and the Sun the far side of the moon is illuminated and the near side we see is dark. This is the New Moon. As the moon continue to move along its orbit around the earth, the sun illuminates a small sliver and we see a thin crescent. Every night the crescent grows a little bit larger or waxes until half of the Moon is illuminated by the Sun. This is the First Quarter Moon. As the moon rotates around to the far side of the earth the sunlight begins to hit more of the Moon. The Moon then grows larger into a Waxing gibbous. When the Moon is on the far side of the Earth (the Earth is between the Sun and the Moon), the near side is the totally illuminated side and the moon appears in the Full Moon stage. The second half of the of the lunar cycle is the reverse of the first. After the Moon is full it begins to shrink or wane through the waning gibbous phase. When the Moon is directly across the Earth from the First Quarter Moon is the Third Quarter Moon. The opposite half of the moon is illuminated here. As the moon continues around the earth toward the Sun it wanes into a crescent, or Waning Crescent Moon. The Moon again reaches the New Moon phase. \r\n\r\nThe actual times involved in the lunar cycle phases: the Moon orbits around the earth at an average distance of 384,440 km. The orbit is elliptical and moves (as seen from the North Pole) counterclockwise with a period of 27.321661 days. This is the sidereal period, that causes it to shift its position in the sky by an amount equal to just slightly more than 13 degrees, measured in relation to the stars. The formula for this is: 360 degrees/27.322 days =(approximately) 13degrees per day. The moon takes approximately 27 days to circle the sky once and return to its original position. However, the cycle of phases takes longer than the moon\'s sidereal period. The moon must travel a little over two more days to regain its position in line with the sun and come in to the new phase. Thus, the lunar phase is approx. 29.5305882 days. This is called the synodic period, the period with respect to the sun.\r\n\r\nWhen does the full moon rise: When the moon is full, it rises in the east as the sun sets in the west.\r\n\r\nHow long is the moon in the sky between rise and set: During a Full Moon, the moon rises at sunset and sets at sunrise, so it is visible in the night sky but not in the daytime. When the moon is at Waxing Gibbous , it rises a few hours before sunset and sets before sunrise. When the moon is in the Third Quarter it rises after midnight and sets at noon. It continues to rise later and later as it goes into the Waning Crescent, which can be seen just before dawn above the eastern horizon. A New Moon rises at Dawn and sets at Sunset; we can not this moon. At New Moon the Moon is in line with the Sun, and it sets in the west with the Sun, which is why we can\'t see it. A few days after the New Moon, the Crescent Moon rises above the western horizon right after sunset. Each day the Moon grows larger and is higher above the horizon. The First Quarter Moon stands high in the southern sky at sunset and does not set until around midnight. As the moon continues to grow fatter in the waxing gibbous phase we find it moves farther east among the stars and sets later and later.\r\n\r\nWhen are the Sun and the Moon in the sky at the same time:\r\n Sometimes the moon can be seen during the daytime also. It depends on what phase the noon is in. For example, when the moon is a waxing gibbous moon, it rises a few hours before sunset. It sets a few hours after sunrise. It is also possible to see the first or third -quarter moon in the daytime sky.\r\n Solar or lunar eclipses also appear with the sun and the moon in the same sky. A lunar eclipse occurs at full moon when the moon moves through the shadow of the earth. It darkens as it enters the shadow because the moon shines only by reflected sunlight. A solar eclipse occurs when the moon moves between the earth and the sun. It the moon covers the disk of the sun completely, the eclipse is a total solar eclipse, otherwise it is a partial eclipse.\r\n\r\nWhat phase is the moon at this time: The Moon is in the sky during the day when it is in these phases: New, First (the second half of the day), Waxing Gibbous (a few hours before sunset), Waning Gibbous (a few hours after sunrise), Third Quarter (the first half of the day) \r\n\r\nDoes Latitude on the earth change these answers: The latitude does not effect the phases of the moon. However, it does change the times at which we see the phases. If the moon is not in the sky at ten o\'clock in the evening, then it will appear twelve hours later at ten o\'clock in the morning. We will see the moon as it appears against a new horizon. \r\n\r\nDoes the earth have phases?\r\nThe earth would have phases according to the perspective of the viewer. For example, if astronauts were on the moon watching a total solar eclipse, they cold only see by standing on the side facing the earth. This would be a \'full earth.\" This is a long process. \r\n The phases of the earth as seen from the moon are as follows: 3rd quarter, waxing crescent, new earth, waning crescent, 1st quarter, waning gibbous, full earth, waxing gibbous.\r\n\r\nWhen does the earth rise: In order to see the earth from the moon you must be on the light side of the moon. At 0 degrees we will always be able to see the earth in the right-hand sky. At 90 degrees, you can not see the earth because the earth is directly behind us on the opposite side of the sky. At 180 degrees the earth will always be to the left, according to our model. At 270 degrees, the earth will always be overhead. \r\n \r\nHow long is the earth in the sky between rise and set: The earth is either constantly in the sky or never in the sky (depending on which side of the moon you are on.)\r\n\r\nWhen are the sun and the earth in the same sky: during the new and crescent phases. The sun is behind the earth and the moon.\r\n\r\nDoes the longitude on the moon have an effect earth\'s phases: Yes, it has an effect because at 0 degrees the earth is on the right, 90 degrees, the earth is behind, at 180 the earth is to the left, at 270 degrees always overhead.\r\n \r\nDoes the sun have phases: No, we can not see phases of the sun because there is no reflected light on the sun except from stars very far away. This light is too miniscule for the human eye to track.\r\n\r\n When does the sun set as seen from the moon: It takes about 12 earth days for the sun to rise and to set on the moon. \r\nDescription of waypoints:\r\nEarthmoon - We enlarged the moon to a 90,000-km in diameter in order to see the phases better.\r\nViewfromfront - Here we are looking at the earth, moon, and the sun on the same plane. We must accelerate to see the motion.\r\nMoonearth - Here we are on the moon looking at the earth. Here we can watch the earth phases and its rise and set. We changed the diameter of the earth to 90,000 and kept the moon normal.\r\nViewfromabove - Here we can see the orbit of the moon around the earth and follow its path.\r\n90degrees - We changed the angle of inclination of the moon to 90 degrees. The phases change with the angle of the sun. We enlarged the moon again to 90,000km to have a better view. This enables us to see the entire moon.\r\n\r\n*Way points may need to be adjusted with the + or - keys\r\n'); INSERT INTO showcase VALUES (18,'qst5.ssf',4518,'',5,5,931526956,''); INSERT INTO showcase VALUES (19,'Question5.ssf',6369,'text/plain',5,1,931534251,'Question 5\r\nGroup 1\r\nAntares, Brian, and Natasha\r\n\r\nWhat are the phases of the moon and how are they created?\r\n\r\nThe moon moves eastward across the sky at about .5 degrees every hour. It moves a total of 13 degrees every 24 hours. This happens because of the moon’s orbit around the Earth. The moon’s orbit is measured in comparison to its place among the stars. The sideral period is 27.321661 days; that is, the moon moves across the sky and back to its original placement in comparison to the stars during this period. The moon rotates on its axis in such a way that the same side always faces the Earth. We would only see different sides of the moon if it did not rotate. Therefore we always see the near side of the moon and never the backside. The shape of the moon seems to change because the sun illuminates the side we can see in different ways. The moon seems to shine because of sunlight that is reflected. The lunar cycle begins with new moon to full moon. As the moon passes between the earth and the sun, only the backside is in the sunlight, and the near side is dark. As the moon is illuminated it grows, or waxes. Therefore we first see the waxing crescent. The first quarter is when we see half of the near side illuminated. The moon then moves into its waxing gibbous phase, gibbous being the Latin word for hunchbacked. When the entire side is illuminated it is a full moon. After this point the moon reverses this process. The waning gibbous is when the moon begins to shrink. Half the moon is again illuminated in third quarter; just a sliver in the waning crescent, and then we are back to new moon. This process takes longer than the sideral period. The synodic period is the moon’s cycle in comparison to the sun. This takes 29.5305882 days for the moon’s phases to complete. \r\n\r\n\r\nDoes the earth have phases? If so, how are they formed?\r\n\r\nThe Earth has phases if viewed from the moon because different sides of the earth are illuminated. In our model, we enlarged the earth and the moon. Then we focused on the moon but followed the earth. With this procedure we were able to see the different phases of the earth, as the illumination of the surface changed. \r\n\r\nDoes the sun have phases? If so, how are they formed?\r\n\r\nThe sun does not have phases. It is the source of illumination for all objects in our solar system, and could therefore not be darkened unless it was in the form of an eclipse. Phases are a cycle of changes in illumination, so the sun could not be said to go through these changes. \r\n\r\nView the moon’s phases from the earth and from a waypoint above the Earth-moon system. Describe what you see. How long do the phases actually take?\r\n\r\nThe earth and moon appear to get the exact same amount of light from where we observed. If we roll to -.05 degrees pitch, 5.3 degrees and 85.1 degrees yaw, we notice that as they slowly rotate the side we observe appears to always get sunlight which draws us to believe we are looking at the side of the earth and moon which receives the most illumination. When the moon begins its phases, the earth appears to go though similar actions. The only reason we can say that the earth’s phrases are harder to see is because we often look at the moon and rarely at the earth.\r\n\r\nCan you fix yourself on the surface of the rotating earth? When does the full moon rise? How long is the moon in the sky between rise and set? When are the sun and moon in the sky at the same time? What phase is the moon in this time? Does the latitude on Earth change your answers to above questions?\r\n \r\nNo, we cannot fix ourselves on the surface of the rotating Earth. We must always adjust because of the rotation. The full moon rises when both the arrows on our model are receiving sunlight and the earth’s arrows are facing away from the moon. The moon is in the sky for twelve hours between rise and set. During the full moon phase the moon rises at sunset and sets at dawn. The sun and the moon are in the sky at the same time during the waxing gibbous and waning gibbous phases. In waxing gibbous it rises a few hours before sunset and you can see it in the late afternoon. The waning gibbous moon sets a few hours after sunrise, so you can see it in the morning. The phases of the moon stay the same, but our perceptions change because of our latitude.\r\n\r\nDescription of Waypoints\r\n\r\n2planet- Even though the planets are at similar angles and both are facing the sun, the moon receives less light when it’s in the crescent phase. At this time the earth is in the half phase. This waypoint is informative because you are looking down on the earth and you can see the moon’s rotation around earth.\r\n\r\n2planet1star- From this waypoint you can see the entire earth, moon, and sun system and see how the moon orbits the earth while the earth is orbiting the sun and how this affects the amount of illumination the earth and moon each get. \r\nPhases- From this waypoint you can observe the moon by itself and see the pattern of the phases and illumination. If you adjust the time you can see the relationships between the moon, earth, and sun; or you can observe the moon on its own.\r\n\r\nView the system as if you are living on the moon. Can you fix yourself on the surface of the moon? When does the earth rise? What phase is it? How long is the Earth in the sky between rise and set? When are the Sun and Earth in the sky at the same time? What phase is the Earth at this time? Does longitude on the Moon change your answers to the above questions?\r\n\r\nNo, you cannot fix yourself on the surface of the rotating moon. The moon will always rotate out from under you and you must constantly adjust. The earth does not rise or set if you are on the near side of the moon, that is, the side of the moon that always faces the earth. From this location the earth would always be in your sky. Therefore the earth is not in a specific phase when it rises since it does not rise. The earth is always in the sky from the near side of the moon, so there is no time difference between rise and set. The longitude on the moon would change your observations because you could be on the back side of the moon, and therefore not see earth at all. \r\n\r\nBefore you leave your model change the angle of inclination of the lunar orbit to 90 degrees. How does this effect the phases?\r\n\r\nWe cannot observe how this affects the phases because our computer has frozen us out of that option. \r\n'); INSERT INTO showcase VALUES (20,'Group2-Q5(2)',4048,'',5,2,931787949,''); INSERT INTO showcase VALUES (21,'Q6Group4MoonPhases.ssf',4221,'',6,4,931964514,'Question 6 by Team 4\r\nQuestion Report \r\nGroup 4, Will and Brian T. \r\nQuestion 6 \r\n \r\n An eclipse is the partial or total obscuration of the light from a celestial body as it passes through the shadow cast by another body. A body may be eclipsed by the passage of another body between it and the observer, as in a solar eclipse, or by the intervention of another body between it and the source of the light it reflects, as in a lunar eclipse. The eclipse of a star by the moon or by a planet or other Solar System body is called an occultation. \r\n A solar eclipse is an eclipse of the Sun by the moon. Since the Moon\'s orbital plane is inclined to the plane of the ecliptic, a solar eclipse can occur only when the Moon is at conjunction (i.e. at new Moon) and at the same time is at or near one of its nodes; the Sun, Moon, and Earth are then very nearly in a straight line. In addition, the Sun\'s angular distance from one of the Moon\'s nodes at conjunction will determine whether an eclipse can or cannot occur. \r\n The apparent diameter of the Sun and the Moon as seen in the sky are almost the same, but they do vary slightly, particularly the Moon\'s, whose maximum and minimum distances from the Earth differ by about 10%. A total solar eclipse is seen at places where the umbra of the Moon\'s shadow-cone falls on and moves over the Earth\'s surface; at the same time the eclipse will appear partial to observers on either side of the central track of totality. Shortly before and after totality the phenomena of shadow bands and Baily\'s beads are observable. During the brief period of totality, the corona and any prominent prominences become visible. When the Moon is near apogee, the tip of its shadow-cone does not reach to the earth and there is an annular eclipse, in which a rim of light is seen around the darkened disk of the Moon. \r\n The overall duration of a solar eclipse from first contact to fourth contact can last as long as 4 hours; totality, from second contact to third contact, lasts at most 7.5 minutes. There are from two to five solar eclipses each year; if there are five, they will all by partial. The total number of solar and lunar eclipse in a year varies from two to seven; if there are only two, they will both be solar. \r\n A lunar eclipse is an eclipse of the Moon by the Earth. Since the Moon\'s orbital plane is inclined to the plane of the ecliptic, a lunar eclipse can occur only when the moon is at opposition (i.e. at full Moon) and at the same time is at or near one of its nodes. The Sun, Earth and Moon are then very nearly in a straight line. Lunar eclipses are visible from anywhere on Earth where the Moon is above the local horizon. The Moon does not become completely invisible during an eclipse because it is partially lit by sunlight refracted by the earth\'s atmosphere, and it appears reddish because the blue component is removed from the sunlight by scattering. \r\n A total lunar eclipse occurs when the Moon is entirely within the umbra, the dark central part of the Earth\'s shadow. The eclipse is partial when the Moon is partly within the umbra, and penumbra when the Moon passes through the penumbra but completely misses the umbra. The overall duration of a total lunar eclipse, from first contact to fourth contact, can last for 3.5 hours; totality, from second contact to third contact, for1.66 hours. There are two or three partial or total lunar eclipses each year. \r\n In Question 6, we were able to see both solar and lunar eclipses, partial and total. At the start of this project, the sun-earth-moon model was used. Initially, the lunar orbit inclination was set at 0 degrees. Observations were made looking at the earth\'s orbit from the moon, and looking at the moon\'s orbit from the earth. During the lunar eclipses, we used the view from the moon and observed when the earth came between the sun and the moon. As viewed from the moon, the earth appeared to move from right to left over the sun; shortly, the entire sun was covered up by the earth causing a lunar eclipse. If we were viewing the moon from the earth during this event, the moon would slowly be covered up by the earth\'s shadow. Because the lunar orbit inclination is at 0 degrees, there are a total of 12 lunar eclipses each year--one each month. A total of 12 solar eclipses also occurred over the course of one year when the moon\'s orbital inclination was at 0 degrees. No partial eclipses occurred either; they were all total eclipses. \r\n Next, the moon\'s orbital inclination was changed to 5 degrees. Now, the chance of an eclipse occurring is decreased. Over the course of one year, there were a total of three lunar eclipses (2 total and 1 partial) and two solar eclipses (1 partial and 1 total). The occurrence of an eclipse varies each year. In the two different \"years\" that we observed in our model, there were a different number of solar and lunar eclipses each year. The number decreased drastically from when the moon\'s orbital inclination was at 0 degrees. The orbits during an eclipse cross each other at a node. In one year, the moon crosses the ecliptic 24 times--twice each month. An eclipse does not occur every time the moon crosses the ecliptic because the moon\'s orbital inclination is at 5. An eclipse occurs only if the sun is near a node; the moon must be crossing either the same node (solar eclipse) or the other node (lunar eclipse). After observing the eclipses when the moon\'s orbital inclination was at 5 degrees, we changed it\'s orbital inclination to 60 degrees. The chance for an eclipse occurring under these circumstances was greatly reduced. The moon has to be exactly in the ecliptic to have an eclipse. The difference in the eclipse between \'almost\' and \'exactly\' is: \'almost\' refers to a partial eclipse (when the earth, moon, and sun are almost lined up) while \'exactly\' refers to a total eclipse (when the earth, moon, and sun are exactly lined up). During a solar eclipse, the moon is moving from right to left as viewed from earth. Between first and fourth contact, a solar eclipse can last as long as four hours. \r\n For the next section, we moved to the moon and observed the earth during solar and lunar eclipses. When we saw a solar eclipse on the moon from earth, we saw the moon slowly be covered up by the earth\'s shadow. The eclipses are reversed. In this case, a solar eclipse on the moon occurs when the earth comes between the sun and the moon. The other eclipse occurs when the moon comes between the sun and the earth. \r\n In the last section, we experimented with different sizes of the moon and the sun, and observed the number of eclipses each year. First, we made the moon 10 times as large. Nine solar eclipses were witnessed over the course of one year: 4 total and 5 partial. Only three lunar eclipses occurred in one year: 1 total and 2 partial. The number of eclipses increased because the moon\'s size was greatly increased. Next, we made the sun 10 times as large. The number of eclipses increased even greater. We saw twelve solar eclipses in one year (2 total and 10 partial) and 6 partial lunar eclipses. We did not witness any total lunar eclipses because the earth is still at it\'s regular size. It wasn\'t big enough to cover up the sun. We were able to make an annular eclipse of the Sun by shrinking the moon\'s diameter only slightly so that when the moon moves in front of the sun, it can\'t cover up the whole sun. Finally, we doubled the lunar distance, while keeping our lunar and solar sizes at 10 times. We witnessed only 3 partial solar eclipses and 2 partial lunar eclipses. The moon only passes between the sun and the earth three times. The earth is too small for any total lunar eclipses to occur. \r\n \r\n'); INSERT INTO showcase VALUES (22,'Question6.ssf',7331,'text/plain',6,1,931964873,'Question Six\r\nGroup 1\r\nAntares, Brian R., Natasha\r\n\r\nWhen and how do the solar and lunar eclipses occur?\r\nSolar eclipses occur when the moon moves between the earth and the sun. A total solar eclipse occurs when the moon covers the sun completely. A partial solar eclipse results when only part of the sun is covered by the moon. A lunar eclipse occurs during a full moon, when the moon moves through the shadow of the earth. This occurs when the moon moves through the shadow caused by the earth’s relationship to the sun. A total lunar eclipse occurs when the moon completely enters the penumbra, where the light is dimmed but not extinguished. A partial lunar eclipse occurs when the moon only partially enters the umbra.\r\nWill this fake rotation affect any of your eclipse observations?\r\nNo, this fake rotation will not affect our observations, as it is merely imitating the actual rotation of the earth.\r\nBegin at the near Earth position and let the system move until you see an eclipse. Move back and forth during the eclipse and give a good description of what is going on. What do you see?\r\nWe are near the Earth and we have been following the orbit of the moon. We stopped the moon as it passed in front of the sun. This is a solar eclipse. A solar eclipse occurs when the moon moves between the earth and the sun resulting in either a partial or total solar eclipse. In our case, the eclipse is not total because the moon is not fully covering the sun. The reason why we can see these eclipses is because our moon has the same angular diameter as our sun so it can cover the sun almost exactly. As we move back and forth we observe the path of the moon as it covers and reveals the sun.\r\nSlowly let the Earth-Moon-Sun system move for a full year. How many eclipses do you see?\r\nWe first observed solar eclipses. Over the period of a year, we observed 12 solar eclipses with a lunar inclination of 0. There are also 12 lunar eclipses at a lunar inclination of 0.\r\nMove the Moon’s orbital inclination to its real value. Now what happens? How many eclipses do you see in one year? What type?\r\nWhen we change the moon’s actual orbital inclination to 5.15 degrees, there was one solar eclipse. In two years we saw three eclipses, two partial eclipses and one annular. With the actual inclination we saw two lunar eclipses in one year. One was a total lunar eclipse, and the other was partial. Because the program does not allow us to see shadows, we cannot see if it is a penumbral eclipse. \r\nTurn on “orbital view”. Describe the orbits during an eclipse. How often does the moon cross the ecliptic in one year? Why doesn’t an eclipse occur every time the moon crosses the ecliptic?\r\nIn our model we observed the orbits during a lunar eclipse. The moon’s orbit was red and the earth’s orbit was blue. As the earth passes between the moon and the sun, the orbits cross, causing a purple disc to appear. In a total lunar eclipse the lunar orbit is level to our viewpoint and the earth is coming across at an angle, causing the entire right side of the moon’s path to appear purple. For our solar eclipse the earth’s orbit was red and the moon’s orbit was blue. During a partial solar eclipse the earth’s orbit could not be seen since we were on the same level, and the moon’s orbit was at a slight angle. It was not possible to see the two orbits overlap. The moon crosses the ecliptic 12 times in one year. An eclipse does not occur every time the moon crosses the ecliptic because the moon does not always completely or partially cover the sun, it often bypasses the sun in the model depending on the inclination. \r\nWhat is the line of nodes and what does it have to do with eclipses?\r\nThe line of nodes is a line across an orbit connecting the nodes-the points where an object’s orbit passes towards the plane of the earth’s orbit. This is commonly applied to the orbit of the moon. The line of nodes are the markers of when an eclipse season occurs. The eclipse season occurs each time the line connecting these nodes points towards the sun.\r\nChange the inclination of the lunar orbit to 60 degrees. Again, what happens to the number of eclipses per year and why?\r\nWhen we changed the lunar inclination in our model to 60 degrees, there were no solar eclipses in a year. This is because the orbit of the moon puts it at such a different angle to the earth that it takes several years for the moon to come between the earth and the sun. As the inclination changes, there are fewer eclipses per year. The same is true of lunar eclipses. It would take the several years for the earth to pass between the moon and the sun with the moon’s inclination at 60 degrees. \r\nDoes the moon have to be exactly in the ecliptic to have an eclipse? What is the difference in the eclipse between “almost” and “exactly” in the ecliptic as we see it from Earth (or the moon)?\r\nNo, the moon does not have to be exactly in the ecliptic to have an eclipse. If the moon is exactly in the ecliptic it will be a total eclipse, whereas if it is “almost” in the ecliptic then only part of the sun would be covered and it would be a partial eclipse.\r\nDuring the solar eclipse which direction is the Moon moving? Can you calculate how fast this is and therefore approximate how long an eclipse will take between first and fourth contact?\r\nIn our model we changed the lunar inclination back to 5.15 degrees in order to see a solar eclipse. We then observed from earth. We also changed the rotation of earth back to 1 day in order to determine how long the eclipse would take. In our eclipse the moon was moving counterclockwise across the sun. In all our eclipses the arrows on our earth were facing back, but we finally found an eclipse that worked. It took about one eighth of a turn, or three hours for the total solar eclipse. \r\nNow move to the moon and find an eclipse. What would you see from the Earth when you see a solar eclipse on the moon? Go through the same exercises from a lunar viewpoint as you did from the earth.\r\nOnce we put our official values back we found a solar eclipse from the moon. The side of the earth nearest the moon would be in nighttime, but would not be able to see the moon because the moon is in the earth’s shadow. This event from the earth would be a lunar eclipse. This shows the difference in perspective, that a solar eclipse on the moon would be a lunar eclipse on the earth. The waypoint we used was luna180 looking at the sun. \r\nStart with the official values of the Earth-Moon-Sun system. Now make the moon 10 times as large. How many eclipses do you see per year? What kinds? Why?\r\nFrom the waypoint earth180 we looked at the moon-sun relationship with the moon ten times its normal size. In one year there were six solar eclipses. All of these eclipses were total solar eclipses. This is because the diameter of the moon is so much greater and it is much easier for it to cover the disc of the sun. We again looked at lunar eclipses from luna180. However, nothing changes from our original observations because only the size of the moon has changed. \r\nMake the sun 10 times as large. How many eclipses do you see per year? What kinds? Why?\r\nFor this experiment we changed the moon back to its official value. We then changed the size of the sun during what was formerly a total solar eclipse, to see the sun dwarf the moon. From this we can conclude that there can be no total eclipses with the sun this size. However, we did see four eclipses, two partial and two annular in one year. This is because the disc of the sun is so large that the moon cannot completely cover it. Next we looked at lunar eclipses. In one year we saw seven partial lunar eclipses, again because the earth in this model is too small to cover the disc of the sun. Once again, we cannot identify penumbral eclipses because of the lack of shadow.\r\nCan you make an annular eclipse of the Sun? \r\nYes, we can make an annular eclipse, that is, a solar eclipse in which the solar photosphere appears around the edge of the moon in a bright ring. The chronosphere and prominences cannot be seen at this time. We made an annular eclipse by positioning the moon completely in the center of the sun. \r\nKeeping your lunar and solar sizes at 10 times, double the lunar distance. How many eclipses do you see per year? What kinds? Why?\r\nWith our moon and sun at 10 times the size, we doubled the lunar distance. In doing this we saw three partial solar eclipses. This is because although the sizes are comparable, the increase in distance made annular eclipses more rare, and caused fewer eclipses in general. At this distance we only saw one partial lunar eclipse, since at this distance the moon is too far from the earth to be impacted by an eclipse. \r\n'); INSERT INTO showcase VALUES (23,'Group2.Q6.ssf',3884,'',6,2,931965355,'When and how do the solar and lunar eclipses occur?\r\n\r\nSolar: When the Moon moves between the Earth and the Sun. If the Moon moves to cover the Sun completely the eclipse is said to be a total solar eclipse, relative to the Earth. A partial solar eclipse occurs when only part of the Sun is covered by the Moon. Observers in the path of totality see a total solar eclipse when the umbra shadow sweeps over them. Those in the penumbra see a partial eclipse.\r\n \r\nLunar: Occurs at full Moon when the Moon moves through the shadow of the Earth. Because the Moon shines only by reflective sunlight it gradually darkens as it enters the shadow. A total lunar eclipse occurs when the Moon\'s orbit crosses the Earth\'s shadow. Not all the eclipses of the Moon are total if the Moon only partially enters the umbra the eclipse is termed a partial lunar eclipse. If the Moon does not enter the umbra at all, but only passes through the penumbra the eclipse is termed penumbral eclipse.\r\n\r\nDoes changing the rotation of the Earth from ½ year to ¼ year effect any of your eclipse observations?\r\n\r\nChanged the size of the Earth by a factor of 10 and the Moon by a factor of 10 to better see the observations. \r\nNo, changing the rotation rate of the Earth does not effect the frequency or characteristics, as they are functions of the Earth\'s orbital properties not the Moon\'s. If the revolution rate of the Moon around its orbit is increased, then the number of eclipses also increases.\r\n\r\nWith the lunar orbit inclination set to 0, what do you see?\r\n\r\nWith the lunar orbit inclination set at 0, we see that the Moon\'s path is no longer tipped to the plane of the ecliptic, therefore a solar eclipse occurs at every new moon and a lunar eclipse at every full moon. This is because with every lunar orbit it crosses at a node. A node is where an object\'s orbit passes through the plane of Earth\'s orbit. Since the lunar orbital plane is the same as the Earth\'s orbital plane every time the Moon is between the Earth and the Sun its shadow is on the Earth, and every time the Earth is between the Moon and the Sun the Moon is in the umbra of the Earth\'s shadow, or is a total lunar eclipse. In a total solar eclipse the Moon moves between the Sun and the Earth from the east and continues westward. At the first contact the Moon\'s West Side meets the Sun\'s East Side. At second contact the Moon\'s East Side meets the Sun\'s east. Next is third contact when the Moon\'s West Side meets the Sun\'s West Side. Last is the fourth contact where the Moon\'s East Side meets the Sun\'s West Side.\r\n\r\nAs the Earth-Moon-Sun system moves for a full year, how many eclipses do you see?\r\n\r\nWith the inclination of the lunar orbit set at 0, we would see about 12 solar eclipses a year and about 12 lunar eclipses per year. \r\n\r\nWith the present inclination, how many eclipses do you see in one year? What type?\r\n\r\nWith the present inclination of 5 degrees 9 minutes, we would see 1 to 2 lunar eclipses per year and 0 to 2 solar eclipses per year. Whether a partial or total eclipse is viewed is determined by the position of the observer on the Earth. One could potentially view 2 total solar, 1 total and 1 partial, 2 partials or no eclipses per year. On our model we counted 4 partial solar eclipses over five years and only 1 total eclipses over five years. We also counted 5 partial lunar eclipses over five years and 5 total lunar eclipses. \r\n\r\nHow often does the Moon cross the ecliptic in one year?\r\n\r\nThe Moon crosses the ecliptic at every new moon and at every full moon. Since there are about 12 full moon cycles per year the Moon crosses the ecliptic about 24 times per year. An eclipse does not occur every time the Moon crosses the Earth\'s ecliptic because for a solar eclipse to occur the Sun must be located on, or very close to for partial eclipse, to the node. A lunar eclipse occurs when the Moon enters the Earth\'s shadow and always follows the ecliptic exactly opposite of the Sun.\r\n\r\nWhat is the line of nodes and what does it have to do with eclipses? \r\n\r\nThe line of nodes is the line formed from the points of intersection of the Moon\'s orbit and the ecliptic. If a line connects all nodes that line is the same as the ecliptic. Solar eclipses only occur when the Sun is near a node. Lunar eclipses occur when the Moon enters the Earth\'s shadow, but the shadow always follows the ecliptic. \r\n\r\nWith the lunar orbit inclination at 60 degrees, what happens to the number of eclipses per year?\r\n\r\nPartial solar eclipses would occur less frequently because of the greater angle of inclination. The number of total solar eclipses is not affected because a total eclipse occurs when the Moon\'s orbit crosses the ecliptic and this is dependent on the Earth\'s rotation around the Sun. If the speed in which the Earth rotates the around the Sun is increased then the number of eclipses increases. Lunar eclipses are effected in the same way. \r\n\r\nDoes the Moon have to be exactly in the ecliptic to have an eclipse?\r\n\r\nNo, it does not need to be in the ecliptic, but it must be near the ecliptic to have a partial eclipse, but it does have to cross the ecliptic for a total eclipse, this point is known as a node. \r\n\r\nWhat is the difference in the eclipse between almost and exactly in the ecliptic as we see it from Earth or the Moon?\r\n\r\n\r\nA partial solar eclipse occurs when the Sun and Moon meet near a node. A total solar eclipse occurs when the Sun and Moon meet at a node. Lunar eclipses occur when the Sun and Moon are at opposite nodes.\r\n\r\nDuring a solar eclipse in which direction is the Moon moving\r\n\r\nThe Moon is moving from east to west, always. It Moon moves at a rate of 0.5 degrees per hour so an eclipse, from first to fourth contact, takes varying times because the exact size of the umbral shadow depends on the location of the Moon in its elliptical orbit and the angle at which the shadow strikes the Earth. The Moon\'s shadow moves across the Earth at speed at least 1700 kilometers per hour. A total solar eclipse takes from 2 to 7 minutes depending on your location. \r\n\r\n\r\nPart 2\r\n\r\nWhat is the difference between a total solar eclipse on the Earth and a total solar eclipse on the Moon?\r\n\r\nA total solar eclipse on the Moon is a total lunar eclipse on the Earth. Viewed from the Moon, a shadow would be seen cast onto the Earth. Since the Moon is between the Earth and the Sun (or a solar eclipse on Earth) both the penumbra and umbra are seen on the Earth because the Moon\'s shadow is still smaller than the Earth. In a lunar eclipse from Earth the Moon fits totally inside the umbra.\r\n\r\nPart 3\r\n\r\nWith the Moon 10 times as large, How many eclipses do you see per year? What kinds and why? \r\n \r\nWe would see more total eclipses and less partial eclipses per year because of the size of the Moon\'s shadow. More often than not the Moon would cover the Sun and the Earth would move into the larger umbra of the Moon\'s shadow. Lunar eclipses would now appear as solar eclipses appear from the Moon. There would be no total lunar eclipses because the Moon would no longer fit inside the Earth\'s umbra.\r\n\r\nWith the Sun also 10 times larger, How many eclipses do you see per year? What kinds and why?\r\n\r\nWe would see a partial solar eclipse every new moon. We did not count any total eclipses, but if there were a total eclipse it would be an annular eclipse. \r\n\r\nCan you make an annular eclipse of the Sun? \r\n\r\nThis would be possible if the Moon is near the farther part of its slightly elliptical orbit and the umbral shadow does not reach the Earth. With the sizes exaggerated, by a factor of 10, we could see an annular eclipse if we set the lunar orbit inclination to 0. At every new moon we would see the eclipse as annular. \r\n\r\nWith the distances doubled, How many eclipses do you see per year? What kinds and why?\r\n\r\n We would not see any total eclipses because any time the Moon moves in front of the Sun it is not sufficiently large and only an annular eclipse occurs. In our model, we counted 7 partial and 2 annular eclipses over one year.\r\n\r\n\r\nTeam 2\r\n07.14.1999\r\nQuestion 6 - Eclipses \r\n'); INSERT INTO showcase VALUES (24,'group3project6.ssf',5159,'application/x-unknown-content-',6,3,932044829,'Susie, Julie, Heather\r\nGroup 3 Project 6\r\n7/12/99\r\nWhen and how do the solar and lunar eclipses occur?\r\n\r\nLunar Eclipse: a Lunar Eclipse occurs at full moon when the moon moves through the shadow of the earth. The moon shines only by reflected light so it darkens as it enters the shadow of the Earth. The Earth\'s shadow has two parts: the umbra and the penumbra. The umbra is the region of total shadow and the penumbra is the region of partial shadow. If the moon totally enters the umbra we see a total eclipse of the moon. A total lunar eclipse occurs gradually. The moon moves eastward a distance equal to its own diameter each hour, and therefore, takes about an hour to completely enter the outer edges of the penumbra. As the moon moves deeper into the penumbra, it dims. After about an hour in the penumbra, it enters into the outer edges of the umbra. The moon then takes an hour to enter the umbra and become totally eclipse. The moon does not disappear completely though. Sunlight is bent by the earth\'s atmosphere and leaks into the umbra producing a reddish glow on the moon. If we were on the moon during a total lunar eclipse, we would not see any part of the sun behind the earth, but we would see a reddish \'sunset\' of the atmosphere surrounding the earth. It is this glow that gives the moon its coppery color. Not all eclipses of the moon are total; this is a partial lunar eclipse and occurs when the moon only partially enters the umbra. These eclipses don\'t have the reddish glow because of the light reflected by the part of the moon not totally in the umbra. There also can be a penumbral eclipse, which occurs when the moon only passes through the penumbra. It is very difficult to see the dimming of the moon during a penumbral eclipse.\r\n\r\nSolar Eclipse: solar eclipses occur when the moon moves between the earth and the sun. If the moon covers the disk of the sun completely, the eclipse is a total solar eclipse. A partial solar eclipse occurs when the moon does not completely cover the disk of the sun. During a solar eclipse, location is important. On one point of the earth a person may see a total solar eclipse, while only a few hundred kilometers away a person would see only a partial eclipse. A total solar eclipse begins when we see the moon encroaching on the sun, or when the edge of the penumbra of the moon sweeps over our location on earth. Through the partial phases of the eclipse, the moon gradually covers the disk of the sun. Totality occurs when the sun is completely behind the moon, or when the umbra sweeps over our location on earth. Totality cannot last longer than 7.5 min. but they typically last only 2 to 3 min. Totality ends when the sun\'s bright surface peeks out from behind the moon or the trailing edges of the moon\'s umbra pass over the observer. During a total eclipse, we can see the corona (the sun\'s faint outer atmosphere) glowing a pale white color. Above the photosphere (disk of sun), we can also see chromosphere. The chromospere is the bright thin layer of gas with frequent eruptions, which glow a pale pink color. Not all solar eclipses are total. Since the moon follows an elliptical orbit, sometimes the moon is too far from the earth and the umbral shadow of the moon does not reach the earth\'s surface. This may be called an annular eclipse: the moon is in front of the sun, and the sun is visible in a bright ring from behind the moon. \r\n\r\nConditions for an Eclipse: For each month the moon crosses the earth\'s ecliptic at two points or nodes. Eclipses can occur only went the sun is near a node. A solar eclipse is caused by the moon passing in front of the sun, and this must happen when the sun is at a node. A lunar eclipse occurs when the moon enters the earth\'s shadow, but that shadow always follows the ecliptic exactly opposite the sun. Thus, the moon can enter the shadow only when the shadow is at a node, and that must mean that the sun is in the opposite side of the sky at the other node. There are two conditions for an eclipse: the sun must be crossing a node and the moon must be crossing the same node or the opposite node. Therefore, solar eclipses occur when the moon is new and lunar eclipses occur when the moon is full.\r\n\r\nAn eclipse season, the line of nodes: an eclipse season occurs when the sun is close enough to a node for an eclipse to occur. As the Earth orbits the sun, the moons orbit remains fixed in direction. The nodes of the moon are points where the moon crosses the plane of the earth\'s orbit. An eclipse season occurs each time the line connecting these nodes points toward the sun. It is only at this time the shadows produce eclipses. The line of nodes rotates every 18.6 years. On earth people see the nodes slipping westward along the ecliptic 19.4 degrees per year. The sun takes only 346.62 days to return to a node. Thus, the eclipse season begins 19 days earlier every year. Any new moon during the eclipse season will cross in front of the sun, causing a solar eclipse. Any full moon will enter the earth\'s shadow and cause a lunar eclipse.\r\n\r\nThe Saros Cycle: after one saros cycle of 18 years and 11 1/3 days, the pattern of eclipses repeats. After one saros cycle the moon and the nodes of its orbit return to the same place with respect to the sun. One saros is nearly equal to 19 eclipse seasons. If an eclipse occur in a place one day, it will occur there again 18 years and 11 days later. The saros cycle is 1/3 a day longer than 18 years 11 days. So the eclipse will not occur at the same spot on the earth\'s location. After 3 saros cycles (54 years) the eclipse will occur at the same location.\r\n\r\nHow many eclipses, lunar and solar at 0 inclination, occur during 1 year: 12 solar and 12 lunar\r\n\r\nHow many eclipses lunar and solar occur per year with the real value of the moon\'s orbital inclination (5 degrees) and what type: 2 solar and 2 lunar\r\n\r\nHow many lunar and solar eclipses occur when the inclination of the lunar orbit is 60 degrees: no solar or lunar eclipses occur when the moon is at 60 inclination. \r\n\r\nHow often does the moon cross the ecliptic per year: the moon crosses the ecliptic 2 times per month. So for an entire year, the moon crosses the ecliptic approximately 24 times.\r\n\r\nWhy doesn\'t an eclipse occur every time the moon crosses the ecliptic: The sun is not always near a node when the moon crosses the ecliptic. For an eclipse to occur, the sun and moon and earth need to be lined up. If the sun is not near a node or on the ecliptic when the moon crosses the ecliptic, these three bodies will not be in line and no eclipse will occur.\r\n\r\nDoes the moon have to be exactly in the ecliptic to have an eclipse: no, but it must be close. There can be a partial lunar eclipse, when the moon only partially goes in the umbra, or simply passes through the penumbra. If we were on the moon we would see part of the earth over imposing the sun. If it were a solar eclipse and the three bodies were not lined up. The moon would cover only part of the sun. If we were on the moon, looking at the earth, we would see a partial eclipse of the earth as we passed into the moon\'s umbra or penumbra, but we would not see much darkening because the sun would illuminate most of the earth.\r\n\r\nDuring a solar eclipse, which direction is the moon moving: the moon always moves counterclockwise around the earth. During a solar eclipse the moon moves counterclockwise in front of the sun.\r\n\r\nWhat would you see from the earth when you see a solar eclipse on the moon: if we were on the moon during a solar eclipse of the sun, we would see the earth superimposed over the sun, blocking the sunlight to the moon. \r\n\r\nDifferences of eclipses as seen from the moon: if we stood on the moon, we would see a solar eclipse of the sun, as the earth crossed over the sun. If the sun and earth were at opposite nodes with the moon in the middle, we would see an eclipse as the earth passed into the moon\'s shadow. So it is opposite of what we would see from the earth. If we were on the earth during the first senerio, we would see a lunar eclipse of the moon, instead of a solar eclipse of the sun. If we were on the earth during the second senerio, we would see a solar eclipse of the sun instead of an eclipse of the earth.\r\n\r\nHow many eclipses are seen per year if we make the moon 10 times as large: 2 lunar eclipses (one partial, one total), 4 total solar eclipses and the moon barely crosses over the outside of the sun 2 other times as well. However, we believe that during lunar eclipses, part of the moon will be in the earth\'s shadow while the upper and lower parts may not be (since the moon is so large). For example the center of the moon may be in the umbra, while the northernmost and southernmost regions may be exposed to light in the penumbra. \r\n\r\nWhy: The number of lunar eclipses remains the same, because to view a lunar eclipse on the computer we stood on the moon and watched for the earth to cross in front of the sun. The moon\'s increased size does not effect this. However, with the moon ten times as large, it covers more surface area in the sky, and therefore, is able to cross in front of the sun more times than at regular size. That is why we have 4 solar eclipses occurring (as seen from earth) instead of 2. \r\n\r\nHow many eclipses occur per year if the sun was 10 times as large: we see no lunar and 9 partial solar, 1 annular eclipse, and 1 total eclipse.\r\n\r\nWhy: The sun and the moon are fairly equal in size when seen from the earth. We therefore see many partial solar eclipses as the moon crosses over the sun. We see one total eclipse as the moon covers the sun, and we see an annular eclipse when the moon is slightly smaller than the sun (relative to the earth\'s orbit). We see no lunar eclipses because the larger sun shortens the earth\'s shadow and the moon does not cross into it.\r\n\r\nCan you make an annular eclipse of the sun: yes, we created an annular eclipse when we increased the moon and sun\'s sizes by 10. The outer most edges of the sun were seen with the moon superimposed in front of it. We also could see annular eclipses of the sun when we stood on the moon and watched the earth cross in front of the enlarged sun.\r\n \r\nHow many eclipses do you see per year when doubling the lunar distance: we see no lunar and 2 partial solar eclipses.\r\n\r\nWhy: we see no lunar eclipses because the earth\'s shadow is too short for the moon to cross into it. We still see 2 solar eclipses of the sun as the far away, tiny looking moon crossed in front of it.\r\n\r\nWaypoints: EM-the waypoint EM puts you on the earth looking at the moon\r\n MS-the waypoint MS puts you on the moon looking at the sun\r\n Earthmoon-normal view\r\n Neare-close to the earth\r\n Nearm-near moon\r\n'); INSERT INTO showcase VALUES (25,'qst6.ssf',6081,'',6,5,932046123,'Astronomy 1010\r\n\r\nGroup 5\r\n\r\nQuestion 6:\r\n\r\n1. When sitting on the earth, a solar eclipse occurs when the moon travels directly in front of the sun. If we set the lunar inclination to 0, a total solar eclipse will occur every time the moon makes an orbit about the earth. During an eclipse in this ideal system, the moon goes directly through the sun-earth line casting a full shadow (umbra) over the earth. From the earth\'s perspective, the sun is completely blocked out by the moon because the relative sizes of the sun and the moon are nearly equal at this distance. As the moon begins to eclipse the sun, we don\'t actually see the moon approaching the sun, because the illuminated side of the moon is opposite our viewpoint, facing the sun. Because of this, we view a solar eclipse from the earth as the sun \"disappearing\" from the sky from right to left, and then \"reappearing\" in the same fashion. Likewise, a lunar ec