Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254..454d&link_type=abstract
Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. 454, 1992
Astronomy and Astrophysics
Astrophysics
3
Accretion Discs, Cataclysmic Variables, Radiation Transfert
Scientific paper
We compute cooling functions for a hot and dense collisionally heated gas taking into account optical thickness effects. We show that these cooling functions depend strongly on the density and on the column density, and so are very different from the classical "optically thin" case (Cox & Tucker t969). In particular the well known maximum of the cooling function at a temperature of the order 105K disappears, owing to line collisional quenching, and the cooling function is smaller than the optically thin ones, even at very high temperatures (˜108 K), if the surface density is a few g cm-2. Computations are limited to a temperature and a density such that the bremstrahlung-compton process is negligible.
These computations are applied to accretion discs in close binary stars, and they show that the "hot" solution is thermally unstable. A grid of cooling functions and Rosseland mean opacities is given, and could be used for other purposes.
No associations
LandOfFree
Cooling Functions for Hot Dense Gas - Application to Accretion Discs in Close Binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Cooling Functions for Hot Dense Gas - Application to Accretion Discs in Close Binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Cooling Functions for Hot Dense Gas - Application to Accretion Discs in Close Binaries will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1044766