Results 161 to 170 of about 64,867 (203)
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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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Proceedings of the Royal Society of London. A. Mathematical and Physical Sciences, 1972
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 E oo = 0. The breezes may be distinguished from one another by the value of the ratio, g
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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 E oo = 0. The breezes may be distinguished from one another by the value of the ratio, g
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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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2014
This chapter presents a general view of stellar winds, the main observational evidences and driving mechanisms. An estimate is made of the mass loss rates for hot and cool stars. The chapter ends with some comments on the interaction of the winds with the interstellar medium and the effects of winds on the evolution of the stars.
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This chapter presents a general view of stellar winds, the main observational evidences and driving mechanisms. An estimate is made of the mass loss rates for hot and cool stars. The chapter ends with some comments on the interaction of the winds with the interstellar medium and the effects of winds on the evolution of the stars.
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Global climatology of synoptically‐forced downslope winds
International Journal of Climatology, 2021John T. Abatzoglou +2 more
exaly