Results 11 to 20 of about 1,742 (119)
, 2004 Neutrino-driven winds are thought to accompany the Kelvin-Helmholtz cooling phase of nascent protoneutron stars in the first seconds after a core-collapse supernova. These outflows are a likely candidate as the astrophysical site for rapid neutron-capture nucleosynthesis (the r-process).
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The Astrophysical Journal, 1981 Models are calculated for stellar winds driven by radiation pressure in spectral lines. The line transfer equation in the fluid frame is solved in order to evaluate the radiation pressure force, and the hydrodynamic structure is constructed to be consistent with this force. This technique avoids use of the Sobolev approximation, which is not applicable
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Star-Driven Wind and Jet Models
Astrophysics and Space Science, 2003 We outline some main results from recent analytical modelling of axisymmetric jets from the coronae of young stars and compare them to disk-wind and X-wind models. We emphazise the roles of the magnetic rotator and the disk in the formation and the evolution of the jet.
Sauty, C. +3 more
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Accretion of supersonic winds on boson stars [PDF]
Physical Review D, 2016 We present the evolution of a supersonic wind interacting with a Boson Star (BS) and compare the resulting wind density profile with that of the shock cone formed when the wind is accreted by a non-rotating Black Hole (BH) of the same mass. The physical differences between these accretors are that a BS, unlike a BH has no horizon, it does not have a ...
Gracia-Linares, M., Guzman, F. S.
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Theory of Winds from Hot Stars [PDF]
Symposium - International Astronomical Union, 1987 Mass loss from hot stars was first established by Morton (1967). He observed 3 OB supergiants, δ, ε and ζ Orionis, with an ultraviolet spectrograph sent up with a rocket. In the wavelength range of 1200 A to 2000 A he observed 6 resonance lines of highly ionized atoms such as C III, C IV, N V and Si IV.
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Winds of hot stars in the Magellanic Clouds [PDF]
Symposium - International Astronomical Union, 1991 The Magellanic Clouds provide a unique laboratory in which to study the metallicity dependence of stellar winds. If proved by observations, such a dependence would have important consequences for stellar evolution, nucleosynthesis, energy balance of the ISM, star formation and so on.
R. P. Kudritzki +3 more
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Parameters and winds of hot massive stars [PDF]
, 2009 Over the last years a new generation of model atmosphere codes, which include the effects of metal line-blanketing of millions of spectral lines in NLTE, has been used to re-determine the properties of massive stars through quantitative spectral analysis methods applied to optical, IR and UV spectra.
Kudritzki, R. -P., Urbaneja, M. A.
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Wind Variability in O-Type Stars [PDF]
Symposium - International Astronomical Union, 1994 The search for the cause of the discrete absorption components (DACs) in P Cygni profiles in UV spectra of O stars continues: pulsation, rotation and magnetic fields are probably all in various degrees important. We highlight some key observations which show that DACs start close to the stellar surface, and emphasize the possible role of localized ...
Henrichs, H.F. +2 more
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The evolution of supernovae in the winds of massive stars [PDF]
, 2004 We study the evolution of supernova remnants in the circumstellar medium formed by mass loss from the progenitor star. The properties of this interaction are investigated, and the specific case of a 35 $\msun$ star is studied in detail. The evolution of the SN shock wave in this case may have a bearing on other SNRs evolving in wind-blown bubbles ...
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Wind variations of wolf-rayet stars [PDF]
International Astronomical Union Colloquium, 1999 AbstractWhat distinguishes WR stars from most of their progenitor phases is their dense winds, that often completely hide their small hydrostatic cores. Thus, to learn about these cores, which are especially important in an evolutionary context, we are generally limited to studying the winds only.
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