Photoionization and Dynamical Evolution of Pregalactic Clouds

Details Photoionization and Dynamical Evolution of Pregalactic Clouds Photoionization and Dynamical Evolution of Pregalactic Clouds

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.606s&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

We investigate thermal and hydrodynamical evolution of collapsing pancake in the era of galaxy formation. We solve detailed chemical rate equations for six species, e, H, H^+, H^-, H^+_2 and H_2. We compute photoionization and photodissociation rates by the UV radiation field. We integrate the radiation transfer equation for the ionizing photons (h nu >= 13.6eV) strictly. When the pancake is irradiated by the UV background radiation field (J21 = 0.1, J_nu propto nu^{-alpha}, alpha = 1), we find a critical thickness with a given initial averaged density bar{n}_ini. It is lambda_cool = 1.1 Mpc (bar{n}_ini/1.0 times 10^{-4} cm^{-3})^{-0.8} that determines whether the sheet will cool or not. If the initial thickness of the sheet is larger than lambda_cool, the sheet collapses and cool below 5 times 10^3K by H_2 rovibrational line emission. Otherwise, the temperature of the sheet is high (T > 10^4 K) throughout the evolution, even if it collapse.

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