منابع مشابه
Stellar Winds in Interaction
WR140 (WC7pd + O5) is often considered to be the archetype of hot, luminous colliding-wind binaries, with strong cyclic high-energy and dust-formation events. The challenge is that this system is quite extreme, with a long period (nearly an integral 7.94 years) and high eccentricity (e = 0.88). Most of the action thus occurs during the relatively short several-month interval of close periastron...
متن کاملStellar Winds from Massive Stars
We review the various techniques through which wind properties of massive stars – O stars, AB supergiants, Luminous Blue Variables (LBVs), Wolf-Rayet (WR) stars and cool supergiants – are derived. The wind momentum-luminosity relation (e.g. Kudritzki et al. 1999) provides a method of predicting mass-loss rates of O stars and blue supergiants which is superior to previous parameterizations. Assu...
متن کاملTurbulence in Line-Driven Stellar Winds
Hot, luminous OB stars have strong stellar winds driven by the line-scattering of the star's continuum radiation. This line-driving mechanism is understood to be highly unstable to smallscale perturbations. I review e orts to simulate the nonlinear evolution of this instability using radiation hydrodynamics simulation codes. Because the usual local, Sobolev treatment for the line-force does not...
متن کاملProbing Clumpy Stellar Winds in SFXTs
Quantitative constraints on the wind clumping of massive stars can be obtained from the study of the hard X-ray variability of SFXTs. In these systems, a large fraction of the hard Xray emission is emitted in the form of flares with typical duration of 3 ksec, frequency of 7 days and luminosity of 10 ergs/s. Such flares are most probably emitted by the interaction of a compact object orbiting a...
متن کاملSpectrum formation in clumpy stellar winds
Modeling expanding atmospheres is a difficult task because of the extreme non-LTE situation, the need to account for complex model atoms, especially for the iron-group elements with their millions of lines, and because of the supersonic expansion. Adequate codes have been developed e.g. by Hillier (CMFGEN), the Munich group (Puls, Pauldrach), and in Potsdam (PoWR code, Hamann et al.). While ear...
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ژورنال
عنوان ژورنال: Astronomy & Astrophysics
سال: 2019
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/201732020