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The nature of the radio emission from stellar winds in wolf-rayet binary stars
, 2012 Gabriela Montes
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Extreme energy in a relaxed galaxy group indicates the bursty nature of AGN feedback
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Science, 1980
The hottest and most luminous stars lose a substantial fraction of their mass in strong stellar winds. These winds not only affect the evolution of the star, they also carve huge expanding cavities in the surrounding interstellar medium, possibly affecting star formation. The winds are probably driven by radiation pressure, but uncertainties persist in
P S, Conti, R, McCray
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The hottest and most luminous stars lose a substantial fraction of their mass in strong stellar winds. These winds not only affect the evolution of the star, they also carve huge expanding cavities in the surrounding interstellar medium, possibly affecting star formation. The winds are probably driven by radiation pressure, but uncertainties persist in
P S, Conti, R, McCray
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Astrophysics and Space Science, 1997
The author surveys the basic theory of stellar winds with momentum input due to a force or with energy input. Five laws of stellar winds are formulated, and different wind mechanisms, line-driven model and dust-driven models are discussed.
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The author surveys the basic theory of stellar winds with momentum input due to a force or with energy input. Five laws of stellar winds are formulated, and different wind mechanisms, line-driven model and dust-driven models are discussed.
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Astrophysics and Space Science, 1974
Stellar winds from a binary star pair will interact with each other along a contact discontinuity. We discuss qualitatively the geometry of the flow and field resulting from this interaction in the simplest case where the stars and winds are identical.
G. L. Siscoe, M. A. Heinemann
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Stellar winds from a binary star pair will interact with each other along a contact discontinuity. We discuss qualitatively the geometry of the flow and field resulting from this interaction in the simplest case where the stars and winds are identical.
G. L. Siscoe, M. A. Heinemann
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Numerical Simulations of Stellar Winds
Space Science Reviews, 1999We discuss steady-state transonic outflows obtained by direct numerical solution of the hydrodynamic and magnetohydrodynamic equations. We make use of the Versatile Advection Code, a software package for solving systems of (hyperbolic) partial differential equations.
Keppens, R., Goedbloed, J.P.
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Journal of Geophysical Research: Space Physics, 1980
The theory of stellar winds as given by the equations of classical fluid dynamics is considered. The equations of momentum and energy describing a steady, spherically symmetric, heat‐conducting, viscous stellar wind are cast in a dimensionless form which involves a thermal conduction parameter E and a viscosity parameter γ.
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The theory of stellar winds as given by the equations of classical fluid dynamics is considered. The equations of momentum and energy describing a steady, spherically symmetric, heat‐conducting, viscous stellar wind are cast in a dimensionless form which involves a thermal conduction parameter E and a viscosity parameter γ.
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Stellar rotation effects on the stellar winds
Physics of Plasmas, 2020The purpose of this paper is to give detailed systematic considerations to clarify and provide insights and a qualitative guide into the role of the azimuthal wind flow in the stellar-rotation braking mechanism. For this purpose, we make use of the Weber-Davis [Astrophys. J. 148, 217 (1967)] magnetohydrodynamic (MHD) version of Parker's [Astrophys.
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