Results 251 to 260 of about 65,066 (300)
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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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Publications of the Astronomical Society of the Pacific, 1980
The effect of the radiative cooling on the steady-state transonic wind model is calculated. It happens that there exists a maximum limit to the mass-loss rate such that if the limit is exceeded, the wind will no longer be in the steady state and turbulence may occur, giving rise to a possible source of X rays in T Tauri objects.
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The effect of the radiative cooling on the steady-state transonic wind model is calculated. It happens that there exists a maximum limit to the mass-loss rate such that if the limit is exceeded, the wind will no longer be in the steady state and turbulence may occur, giving rise to a possible source of X rays in T Tauri objects.
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Radiation Driven Stellar Winds
AIP Conference Proceedings, 2009Stellar winds are ubiquitous among massive stars. They play a crucial role in stellar evolution, and strongly affect observed spectra. While it is generally accepted that the winds are driven by radiation pressure, acting through bound‐bound transitions, many details remain unclear.
D. John Hillier +4 more
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2018
The tidally influenced secondary stars in interacting binaries are rapidly rotating and possess convective envelopes or are fully convective. This makes the generation of large-scale magnetic fields in such stars very likely, and magnetically influenced wind flows from the stellar surface would then lead to magnetic braking. The secondary would be spun
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The tidally influenced secondary stars in interacting binaries are rapidly rotating and possess convective envelopes or are fully convective. This makes the generation of large-scale magnetic fields in such stars very likely, and magnetically influenced wind flows from the stellar surface would then lead to magnetic braking. The secondary would be spun
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Circumstellar Shocks: Colliding Stellar Winds
Astrophysics and Space Science, 1995In this paper I will review some recent developments in the field of circumstellar shocks, particularly as they relate to colliding stellar winds. I shall review the basic physics of colliding winds and shocks, and discuss recent developments in hydrodynamic modelling of colliding winds.
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2007
I present here some ideas on how jets from low mass stars may evolve as the star evolves from class 0 to the main sequence through classes I, II, III. Analytical models and simulations suggest that the ejection start very early in the life of a low mass star from the edge of the disk.
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I present here some ideas on how jets from low mass stars may evolve as the star evolves from class 0 to the main sequence through classes I, II, III. Analytical models and simulations suggest that the ejection start very early in the life of a low mass star from the edge of the disk.
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