Results 121 to 130 of about 1,093 (161)
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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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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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Analysis of a Magnetohydrodynamic Stellar Wind
Astrophysics and Space Science, 1986Characteristic features of solutions are analysed around the Alfvenic point. There are three types of solutions through the point.
Yasumichi Saito, Mamoru Saitō
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Proceedings of the Royal Society of London. A. Mathematical and Physical Sciences, 1972
Abstract Steady stellar winds are generally divided into two classes: (i) the winds proper, for which the energy flux per unit solid angle, E∞, is non-zero, and (ii) the breezes, for which Eoo = 0. The breezes may be distinguished from one another by the value of the ratio, g, of kinetic to thermal energy of the particles in the limit
Paul Harry Roberts +1 more
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Abstract Steady stellar winds are generally divided into two classes: (i) the winds proper, for which the energy flux per unit solid angle, E∞, is non-zero, and (ii) the breezes, for which Eoo = 0. The breezes may be distinguished from one another by the value of the ratio, g, of kinetic to thermal energy of the particles in the limit
Paul Harry Roberts +1 more
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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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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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2014
Exposure to stellar winds can have significant long term consequences for planetary atmospheres. Estimating the effects of these winds requires knowledge of how they evolve with time. Determining this empirically requires the ability to study the winds of stars of various ages and activity levels, but this is not easy to do as the coronal winds of ...
Wood, Brian E. +2 more
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Exposure to stellar winds can have significant long term consequences for planetary atmospheres. Estimating the effects of these winds requires knowledge of how they evolve with time. Determining this empirically requires the ability to study the winds of stars of various ages and activity levels, but this is not easy to do as the coronal winds of ...
Wood, Brian E. +2 more
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Physica Scripta, 1984
The mass loss phenomenon in hot luminous stars is discussed and models for the structure of the wind, two component models and shock models are described. The constraints on models by X-ray observations are analysed. Hot stars return considerable amounts of matter and energy to the interstellar medium; the importance of this flow of energy and matter ...
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The mass loss phenomenon in hot luminous stars is discussed and models for the structure of the wind, two component models and shock models are described. The constraints on models by X-ray observations are analysed. Hot stars return considerable amounts of matter and energy to the interstellar medium; the importance of this flow of energy and matter ...
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Astrophysics and Space Science, 1998
The different methods for the study of stellar winds are discussed: (1) P Cygni profiles (2) atomic emission lines (3) infrared and radio free-free emission (4) molecular emission lines (5) infrared radiation by dust. For each of these methods we describe some characteristic observations and we discuss the way in which these data can be used to derive ...
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The different methods for the study of stellar winds are discussed: (1) P Cygni profiles (2) atomic emission lines (3) infrared and radio free-free emission (4) molecular emission lines (5) infrared radiation by dust. For each of these methods we describe some characteristic observations and we discuss the way in which these data can be used to derive ...
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1999
This long-awaited graduate textbook, written by two pioneers of the field, is the first to provide a comprehensive introduction to the observations, theories and consequences of stellar winds. The rates of mass loss and the wind velocities are explained from basic physical principles.
Henny J. G. L. M. Lamers +1 more
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This long-awaited graduate textbook, written by two pioneers of the field, is the first to provide a comprehensive introduction to the observations, theories and consequences of stellar winds. The rates of mass loss and the wind velocities are explained from basic physical principles.
Henny J. G. L. M. Lamers +1 more
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