SIMBAD references

2014MNRAS.438.3557K - Mon. Not. R. Astron. Soc., 438, 3557-3567 (2014/March-2)

Suppression of X-rays from radiative shocks by their thin-shell instability.

KEE N.D., OWOCKI S. and UD-DOULA A.

Abstract (from CDS):

We examine X-rays from radiatively cooled shocks, focusing on how their thin-shell instability reduces X-ray emission. For 2D simulations of collision between equal expanding winds, we carry out a parameter study of such instability as a function of the ratio of radiative versus adiabatic-expansion cooling lengths. In the adiabatic regime, the extended cooling layer suppresses instability, leading to planar shock compression with X-ray luminosity that follows closely the expected (L_X ∼{dot}M^2) quadratic scaling with mass-loss rate {dot}M. In the strongly radiative limit, the X-ray emission now follows an expected linear scaling with mass-loss (L_X ∼{dot}M), but the instability deforms the shock compression into extended shear layers with oblique shocks along fingers of cooled, dense material. The spatial dispersion of shock thermalization limits strong X-ray emission to the tips and troughs of the fingers, and so reduces the X-ray emission (here by about a factor 1/50) below what is expected from analytic radiative-shock models without unstable structure. Between these two limits, X-ray emission can switch between a high-state associated with extended shock compression, and a low-state characterized by extensive shear. Further study is needed to clarify the origin of this `shear mixing reduction factor' in X-ray emission, and its dependence on parameters like the shock Mach number.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): shock waves - hydrodynamics - instabilities - stars: mass-loss - X-rays: binaries - X-rays: stars

Status at CDS:  

Simbad objects: 2

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2020.06.03-22:51:36

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