X-Ray Emission from Colliding Winds in Pre-Main Binary Systems

Details X-Ray Emission from Colliding Winds in Pre-Main Binary Systems X-Ray Emission from Colliding Winds in Pre-Main Binary Systems

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.271..667z&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 271, NO. 3/DEC1, P. 667, 1994

Astronomy and Astrophysics

Astronomy

12

Scientific paper

We present model calculations of the X-ray emission in the range 0.1-2.5 keV from colliding supersonic winds in young binary systems. For typical winds, with velocities between 300 and 500 km s- and mass-loss rates between 10-8 and 10-6 M0 , we find that the X-ray luminosity of the interaction region amounts to erg s- for binary separations less than 50 au. While the luminosity is in accordance with the observed range for pre-main-sequence stars, the bulk of the emission occurs in the soft part of the spectrnm below 1 keV. We have considered the effects of the interaction of winds with different velocities. In this case, the X-ray emission consists of a `soft' component, due to the slower wind, and a `hard' component from the fast one. Such a double-peaked spectrnm is also found in the case where, in addition to the shocked emitting gas, a stellar component with typical temperature 1 keV is present. Thus the soft X-ray excess represents the signature of interacting stars and can be used as an effective diagnostic to search for binary systems. Key words: shock waves - binaries: close - stars: mass-loss - stars: pre-main-sequence - X-rays: stars.

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