Stellar winds in binary X-ray systems

Details Stellar winds in binary X-ray systems Stellar winds in binary X-ray systems

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..267m&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 267-281.

Astronomy and Astrophysics

Astrophysics

42

Binary Stars, Radiation Effects, Stellar Mass Accretion, Stellar Winds, X Ray Sources, B Stars, Early Stars, Gas Ionization, Magnetohydrodynamic Flow, O Stars, Photoionization, Radiative Heat Transfer, Stellar Luminosity, Stellar Mass Ejection, Wind Velocity

Scientific paper

It is thought that accretion from a strong stellar wind by a compact object may be responsible for the X-ray emission from binary systems containing a massive early-type primary. To investigate the effect of X-ray heating and ionization on the mass transfer process in systems of this type, an idealized model is constructed for the flow of a radiation-driven wind in the presence of an X-ray source of specified luminosity, Lx. It is noted that for low values of Lx, X-ray photoionization gives rise to additional ions having spectral lines with wavelengths situated near the peak of the primary continuum flux distribution. As a consequence, the radiation force acting on the gas increases in relation to its value in the absence of X-rays, and the wind is accelerated to higher velocities. As Lx is increased, the degree of ionization of the wind increases, and the magnitude of the radiation force is diminished in comparison with the case in which Lx = 0. This reduction leads at first to a decrease in the wind velocity and ultimately (for Lx sufficiently large) to the termination of radiatively driven mass loss.

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