Bibcode
DOI
Crivellan, L.; Simonneau, E.
Referencia bibliográfica
The Astrophysical Journal, vol. 428, no. 2, pt. 1, p. 753-759
Fecha de publicación:
6
1994
Revista
Número de citas
2
Número de citas referidas
2
Descripción
In view of more general applications, we have developed a new approach
to render explicit the temperature both in the source function of the
radiative transfer equation and in the constraint of radiative
equilibrium. This is a necessary step in the iterative temperature
correction when computing stellar atmosphere models. Our method consists
of a proper factorization of the Planck function through a normalized
frequency profile bnu=bnu(T), computed from a
trial temperature, and B(T), the integral over frequencies of the Planck
function itself. It holds that B(sun nu)(T) = bnu B(T);
integral bnu d nu=1. The quantity B(T) is proportional to the
fourth power of the temperature required. Such an approach, which works
exactly as the customary linearization method, can easily be applied
also to correcting a trial radiation field, within a class of more
general radiative transfer problems.