Calculation involving hydrogen-hydrogen(2) collisional cooling processes for use in astrophysics

This thesis will calculate the H-H2 cooling processes used in astrophysics. Cooling is critical to the formation of the first objects formed in the early universe, and other diverse phenomenon of interest to astrophysics. For instance, in order to collapse into objects, the gravitational potential energy of primordial density fluctuations must be radiated away. The most abundant element in the universe is hydrogen, and cooling processes involving hydrogen are important in several contexts. To calculate the cooling, the cross section for collisional excitation at constant energy were integrated over a Maxwellian velocity distribution to determine a rate coefficient. Then the equilibrium level populations will be solved for a given temperature and H density. Finally, the cooling and spectra are calculated from these equilibrium populations.

Name thesis:degree_name

Master of Science (MS)

Level thesis:degree_level

Thesis

Discipline thesis:degree_discipline

Physics

Grantor dc:publisher

University of Nevada, Las Vegas

Year

2002

Author dc:creator

• Archer, David Michael

Contributors dc:contributor

• Stephen Lepp

Statement dc:rights

• IN COPYRIGHT. For more information about this rights statement, please visit http://rightsstatements.org/vocab/InC/1.0/

Language dc:language

English

Identifier

https://oasis.library.unlv.edu/rtds/1448

OAI identifier oai:identifier

oai:oasis.library.unlv.edu:rtds-2447