Doctor of Philosophy in Astronomy
Physics and Astronomy
First Committee Member
Stephen Lepp, Chair
Second Committee Member
Third Committee Member
Graduate Faculty Representative
Number of Pages
The implications of H+H2 cooling in astrophysics is important to several applications. One of the most significant and pure applications is its role in cooling in the early universe. Other applications would include molecular dynamics in nebulae and their collapse into stars and astrophysical shocks. Shortly after the big bang, the universe was a hot primordial gas of photons, electrons, and nuclei among other ingredients. By far the most dominant nuclei in the early universe was hydrogen. In fact, in the early universe the matter density was 90 percent hydrogen and only 10 percent helium with small amounts of lithium and deuterium. In order for structure to form in the universe, this primordial gas must form atoms and cool. One of the significant cooling mechanisms is the collision of neutral atomic hydrogen with a neutral diatomic hydrogen molecule. This work performs calculations to determine collisional cooling rates of hydrogen using two potential surfaces.
Astrophysics; Bkmp2; Dominant nuclei; Hydrogen; Interstellar hydrogen; Ion recombination; Mielke; Pure sciences; Rate coefficients; Recombination
Astrophysics and Astronomy | Chemistry | Cosmology, Relativity, and Gravity | Stars, Interstellar Medium and the Galaxy
Kelley, Matthew, "Molecular Processes in Astrophysics: Calculations of H + H2 Excitation, De-Excitation, and Cooling" (2012). UNLV Theses, Dissertations, Professional Papers, and Capstones. 1521.