Computational Atomic and Molecular Physics and Computational Astrophysics
All of the information we receive about the universe comes to us in the form of photons (except for a handful of neutrinos). These photons are emitted by atoms and molecules which reside in the various astronomical environments. The character of this emission (e.g., the intensity) is related to the environmental parameters (e.g., density, temperature, radiation field, distribution of atoms, molecules, and electrons, etc.) that the emitting species finds itself. Therefore, there is a fundamental connection between astronomy and atomic and molecular physics.
In my research group, we are engaged in two main efforts: 1) the calculation of various atomic and molecular parameters, using modern computational techniques, which are relevant to astrophysics and 2) modeling of astrophysical environments using the results obtained in 1). Our interests include many types of astronomical objects and environments including the early Universe, the formation of the first stars, x-ray emission from comets and planets, extrasolar giant planets, cool stellar atmospheres, supernovae, and planetary nebulae.
Students working in my research group will receive hands-on exposure to atomic and molecular physics, computational physics and numerical methods, and theoretical molecular astrophysics. For students taking the PHYS 8990 course, I offer two original projects:
- Photodestruction of atoms and molecules in astrophysical radiation fields. In the majority of astrophysical plasmas, the abundances of the atomic and molecular species are not in equilibrium and therefore must be determined by a balance of formation and destruction processes. An important destruction process is that due to the absorption of photons which however, is very sensitive to the local radiation environment. In this project, the student will explore the differences in photodestruction rates for various environments including the interstellar medium, stellar atmospheres, quasars, the extragalactic medium, and the early Universe including the effect of recombination distortion photons. As an example, we will consider H-. Some experience with Unix and Fortran, or C++, would be helpful, but is not a requirement.