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Wind asymmetries in massive stars
Space Science Reviews, 1994We are in the process of surveying the linear polarization in luminous, early-type stars. We here report on new observations of the B [e] stars S 18 and R 50, and of the Luminous Blue Variables HR Car, R 143, and HD 160529. Together with previously published data, these observations provide clear evidence for the presence of intrinsic polarization in 1
R. E. Schulte-Ladbeck +6 more
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Astrophysics and Space Science, 1990
The CIV and SiIV resonance doublets of 43 Be stars are investigated. Measurements of the equivalent widths seem to reveal a correlation between the strenght of the lines and the projected rotational velocity (v sini). it is discussed whether this result indicate that the wind region is not spherically symmetric.
F. X. De Araujo +1 more
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The CIV and SiIV resonance doublets of 43 Be stars are investigated. Measurements of the equivalent widths seem to reveal a correlation between the strenght of the lines and the projected rotational velocity (v sini). it is discussed whether this result indicate that the wind region is not spherically symmetric.
F. X. De Araujo +1 more
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Astrophysics and Space Science, 1994
The magnetic Bp stars, i.e., the helium-strong and helium-weak/silicon-strong stars, have well ordered, global magnetic fields and are hot enough to have weak, radiatively driven stellar winds. They are the only stars where we can study magnetic winds for which the approximate magnetic field structure is known.
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The magnetic Bp stars, i.e., the helium-strong and helium-weak/silicon-strong stars, have well ordered, global magnetic fields and are hot enough to have weak, radiatively driven stellar winds. They are the only stars where we can study magnetic winds for which the approximate magnetic field structure is known.
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Publications of the Astronomical Society of Japan, 1983
Abstract The structure of a spherically symmetric, stationary mass-losing shell on a neutron star is calculated. Mass loss occurs just afetr a nuclear flash, because the energy flux at the bottom of the shell exceeds the local Eddington luminosity near the photosphere, where the Eddington luminosity decreases outward due to the ...
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Abstract The structure of a spherically symmetric, stationary mass-losing shell on a neutron star is calculated. Mass loss occurs just afetr a nuclear flash, because the energy flux at the bottom of the shell exceeds the local Eddington luminosity near the photosphere, where the Eddington luminosity decreases outward due to the ...
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1988
The present state of knowledge about winds and chromospheres of G, K, and M giants and supergiants has been reviewed.
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The present state of knowledge about winds and chromospheres of G, K, and M giants and supergiants has been reviewed.
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Effects of Wind-Wind Collision in Close Binary Stars
Astrophysics and Space Science, 2000Various observational appearences of the effects of wind-wind collision for binary stellar systems have been discovered recently in X-ray, UV, optical, IR and radio ranges. Recent 3D gas-dynamic simulations of the wind-wind collision regions in WR+O, O+O and symbiotic binary systems allow to understand the physics of wind-wind collision effects ...
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Rotationally modulated winds of O stars
International Astronomical Union Colloquium, 1999AbstractThe stellar wind diagnostics of some well-studied O stars exhibit cyclical variations with periods that are probably related to the rotational period of the underlying star. This rotational modulation is usually attributed to large scale, persistent structures in the wind, which are thought to be generated and maintained by photospheric ...
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Shocks and shells in hot star winds
Astrophysics and Space Science, 1995Radiation-driven winds of hot, massive stars show variability in UV and optical line profiles on time scales of hours to days. Shock heating of wind material is indicated by the observed X-ray emission. We present time-dependent hydrodynamical models of these winds, where flow structures originate from a strong instability of the radiative driving ...
A. Feldmeier +5 more
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Consequences of Clumping in Hot-Star Winds
Astrophysics and Space Science, 1994It seems more and more likely that one will have to abandon the paradigm of smooth outflows from (hot) stars in favour of a clumpy structure, possibly in a fractallike hierarchy on all scales. Observationally, this is best established for Wolf-Rayet star winds (e.g.
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Effects of rotation on hot star winds
Astrophysics and Space Science, 1994We discuss the structure of a radiatively-driven wind from a rapidly rotating hot star. When the rotation rate is large, there is a region at low latitudes near the stellar surface where the force of gravity is larger than the radiation pressure. Within this region, the streamlines “fall” toward the equator, and if the rotation rate is large enough ...
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