Results 331 to 340 of about 409,343 (365)

Mass Loss and Stellar Evolution

1979
The available observational evidence about stellar winds and mass loss is briefly reviewed, and its implications for stellar evolution are discussed. Particular emphasis is placed on post-main sequence evolution of low-mass and intermediate-mass stars, including the final evolution from red giant to the white dwarf stage.
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Mass Loss in Young Stellar Objects

Astrophysics and Space Science, 1998
Various aspects of mass loss associated with Young Stellar Objects are reviewed. The classification of the driving sources of the outflows is presented, and the properties of the youngest sources, the Class 0 protostars, are given. The observed properties of the molecular, atomic, and neutral components of the bipolar flows are discussed and critically
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Mass loss in early stages of stellar evolution

Nature, 1976
IT has been known for some time that stars lose mass between their birth on the main sequence and their death as white dwarfs (or as neutron stars or black holes for more massive stars), and the existence of the solar wind shows that not all the mass loss occurs in a last gasp to form a planetary nebula.
D. S. P. DEARBORN, M. KOZLOWSKI, D. SCHRAMM   +2 more
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Stellar winds and mass loss of a rotating star

Astrophysics and Space Science, 1972
The mass loss to be expected from the corona of a rotating F2-star is calculated. The rotation is supposed to be rigid up to a certain distances, as if it were maintained by a strong magnetic field. Dependent on the values of the rotational velocity the mass loss can increase to 26–40% forvrot up to 200 km s−1.
J. P. De Grève, C. De Loore, C. De Jager   +2 more
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Nucleosynthesis, Mass Loss and Stellar Evolution

1969
Stars are formed from material of the interstellar medium with a given composition: X (the fraction of hydrogen), Y (the fraction of helium), Z (the fraction of the sum of the heavy elements, which can be splitted in Z1, Z2, Z3,... representing these heavy elements).
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Mechanisms of Solar (and Stellar) Mass Loss

1996
The fundamental theory for mass loss from late-type stars such as our Sun was developed by Gene Parker in the 1950’s (Parker 1958), and has been largely understood since then; refinements since then have largely focused on physically more realistic fluid equations (which take into account, for example, the effects of multi-component fluids and ...
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Effects of Mass Loss on Stellar Evolution

1981
Session I - Winds From Early Type Stars: Observations.- Observations of stellar winds in early type stars (invited lecture).- The dependence of mass loss on the basic stellar parameters. (invited paper).- The velocity characteristics of WR stellar winds.- The iron curtain of the WC 9 star HD 164270..- Is a stellar wind inherent in WR-stars throughout ...
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The Influence of Photospheric Turbulence on Stellar Mass Loss

1987
We show that the stellar rate of mass loss is positively correlated with the average microturbulent photospheric velocity, and that the energy contained in the microturbulent motions is of the same order of magnitude as the wind energies.
Cornells de Jager, Hans Nieuwenhuijzen
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Stellar Mass Loss by Turbulent Alfvén Waves

1988
In the present study, we analyze the effect of the change in the opening angle of the magnetic field on mass loss and terminal velocity of the “typical” K5 supergiant (Model 6 of Hartmann and MacGregor (1980)). We use a flux of turbulent Alfven waves as the acceleration mechanism of the wind, with non-linear and surface Alfven wave absorption.
Reuven Opher, Vera J. S. Pereira
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Stellar pulsation, atmospheric structure, and mass loss

2008
Pulsation in one or many radial and/or non-radial modes may be a universal characteristic of stars. The possible consequences of pulsation include an increase in the atmospheric scale height (“levitation”), the heating of a region of the atmosphere to a temperature well in excess of the radiative equilibrium temperatur, and the driving of substantial ...
L. A. Willson, G. H. Bowen
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