On flow phenomena that emit X-rays in hot star winds.

Details On flow phenomena that emit X-rays in hot star winds. On flow phenomena that emit X-rays in hot star winds.

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996rftu.proc...29f&link_type=abstract

International Conference on X-ray Astronomy and Astrophysics: Röntgenstrahlung from the Universe, p. 29 - 30

Astronomy and Astrophysics

Astrophysics

Stellar Winds: X Rays, Stellar Winds: Numerical Simulations, Stellar Winds: O Stars

Scientific paper

The X-ray emission from O stars may originate from instability-generated shocks in their stellar winds. Previous numerical simulations that assumed the wind to be isothermal could only draw limited conclusions concerning this emission. The authors present new calculations including the energy transfer in the wind. They confirm that up to a few stellar radii, radiative cooling is efficient, i.e., shock cooling zones are short compared with dynamical lengths. At larger radii, however, the wind structure changes drastically because all shocks are destroyed quickly due to a broadening of their cooling zones. The authors discuss the following flow phenomena as possible sources of X-rays: (1) inner radiative shocks; (2) shock merging; (3) outer adiabatic shocks; (4) leftover hot gas from shock destruction; and (5) an outer corona.

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