X-ray emission in wind instability simulations

Details X-ray emission in wind instability simulations X-ray emission in wind instability simulations

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..427c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 427-435

Statistics

Computation

11

B Stars, Computational Astrophysics, Main Sequence Stars, O Stars, Shock Waves, Stellar Physics, Stellar Winds, Temperature Profiles, X Ray Astronomy, X Rays, Computerized Simulation, Density Distribution, Line Spectra, Shock Heating, Spectrum Analysis, Stellar Models, Time Dependence

Scientific paper

We estimate X-ray emission by shock-heated regions in hot star winds, using temperature and density profiles calculated by time-dependent dynamical models; the shocks result from the instability of the line scattering force that drives the wind. For main sequence late O and early B stars, the model X-ray flux is generally well below the observed flux, though the shape of the model spectrum is approximately consistent with observations. For the early O supergiant zeta Pup, the model spectral shape again agrees with observation; the total flux predicted by models is well above the observed flux, though significant uncertainties remain.

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