Astronomy and Astrophysics – Astronomy
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.6402d&link_type=abstract
American Astronomical Society, AAS Meeting #212, #64.02; Bulletin of the American Astronomical Society, Vol. 40, p.255
Astronomy and Astrophysics
Astronomy
Scientific paper
It has been suggested that the steady-state approximation for determining NLTE occupation numbers is not sufficient in Type II supernovae and thus the time-dependent rate equations must be solved (Utrobin and Chugai 2005). This is because the recombination time increases due to Lyman alpha trapping causing the recombination time to become comparable to the age of the supernova. The calculations are based on the Sobolev approximation and a simple two-level hydrogen atom. We calculate the recombination time for hydrogen using our general radiative transfer code PHOENIX. We use a known density, temperature and velocity structure consistent with the observed spectrum of SN 1999em, 20 days after maximum light. Since PHOENIX does exact radiative transfer, we can determine whether the approximations of Utrobin and Chugai (2005) hold. We study four different systems: a simple two-level hydrogen atom and a complete multilevel hydrogen atom in both pure hydrogen and solar compositions to explore the relevance of time dependence in the rate equations.
Baron Eddie
De Soma
Hauschildt Paul
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