The structure of radiative shock waves. IV. Effects of electron thermal conduction
Abstract
We consider the structure of steadystate radiative shock waves propagating in partially ionized hydrogen gas with density rho_{1} = 10^{10} gm cm^{3} and temperature 3000 Kle T_{1}<=8000 K. The radiative shock wave models with electron thermal conduction in the vicinity of the viscous jump are compared with pure radiative models. The threshold shock wave velocity above which effects of electron thermal conduction become perceptible is found to be U_{1}^{*}~ 70 km s^{1} and corresponds to the upstream Mach numbers from M_{1}~ 6 at T_{1}=8000 K to M_{1}~ 11 at T_{1}=3000 K. In shocks with efficient electron heat conduction more than a half of the hydrogen atoms are ionized in the radiative precursor, whereas behind the viscous jump the hydrogen gas undergoes the full ionization. The existence of the electron heat conduction precursor leads to the enhancement of the Lyman continuum flux trapped in the surroundings of the discontinuous jump. As a result, the partially ionized hydrogen gas of the radiative precursor undergoes an additional ionization (deltax_{H} <~ 5%), whereas the total radiave flux emerging from the shock wave increases by 10%le delta (F_{R}) <=25% for 70 km s^{1}le U_{1} <=85 km s^{1}.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 September 2002
 DOI:
 10.1051/00046361:20020995
 arXiv:
 arXiv:astroph/0206240
 Bibcode:
 2002A&A...392..735F
 Keywords:

 shock waves;
 hydrodynamics;
 radiative transfer;
 stellar atmospheres;
 Astrophysics
 EPrint:
 6 pages, 5 figures, LaTeX, accepted for publication in AA