Results 151 to 160 of about 17,712 (190)

Turbulent Transport in Stellar Interiors

Theoretical and Computational Fluid Dynamics, 1998
The authors consider differential rotation as a major cause of turbulence in stably stratified stellar interiors. It is shown that for an anisotropy \(A\) of horizontal to vertical velocities, the vertical diffusivity is a factor \(A^2\) less than the horizontal diffusivity. Transport by meridional circulation is also reduced, as well as the efficiency
Michaud, G., Zahn, J.-P.
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GAIA AND PHYSICS OF STELLAR INTERIORS

EAS Publications Series, 2002
Understanding the stellar interiors is an important issue for astrophysics, but also for fundamental physics. The physical description of the stellar material implies statistical physics as well as hydrodynamics. We give examples of unsolved physical problems and their consequences for predictions of stellar properties and evolution.
Lebreton, Yveline, Baglin, Annie
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Opacity in Stellar Interiors

Publications of the Astronomical Society of the Pacific, 1931
marks that the "discrepancy" in Eddington's theory regarding the opacity of stellar interiors can be removed by assuming that the star is almost entirely of hydrogen. I have been for some time past engaged in an accurate evaluation of the opacitycoefficient (which is defined as the Rosseland mean) and the absorption-coefficient (which is defined as the
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Neutrino Processes in Stellar Interiors

Annual Review of Astronomy and Astrophysics, 1975
This review is a discussion of the role of neutrinos in different relevant epochs of stellar evolution. Section one outlines the basic theoretical and experimental work. Section two is devoted to the effects of neutrino losses on late stages of stellar evolution in general.
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Magnetic monopoles in stellar interiors

Lettere Al Nuovo Cimento Series 2, 1985
We study the energy loss of magnetic monopoles in a hot plasma and discuss the trapping of magnetic monopoles in the interior of the Sun. We find that magnetic monopoles inpinging onto the Sun with V ∼ 10−3 c are trapped if their mass is M ≲10−16 GeV. Bounds on the flux of such particles are derived from data on the Sun magnetic field, luminosity and ...
L. Bracci, G. Fiorentini
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Supersonic convection in stellar interiors

Chinese Astronomy and Astrophysics, 2006
According to the result of the numerical simulation on stellar convective envelopes by the traditional mixing length theory, supersonic convection would occur on the top of the convective regions of the yellow-and-red giants and supergiants. This, however, is not self-consistent with the local convection theory itself.
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Physical Processes in Stellar Interiors

Physics Bulletin, 1964
By D. Frank-Kamenetskii London: Oldbourne Book Co. Ltd. 1963. Pp. xi + 337. Price $14. This edition from the Russian is produced by the Israel Program for Scientific Translation at Jerusalem. The original is dated from Moscow in 1959, and acknowledges help from British and American as well as Russian authorities in the appropriate field.
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Beta Decay in Stellar Interiors

Physical Review, 1962
A study is made of the temperature and density dependence of beta-decay rates as they are affected by electron capture from continuum orbits, the absence of atomic binding energies, screening, and the exclusion principle. The rate of allowed electron capture from continuum orbits in a Fermi gas is calculated using the $V\ensuremath{-}A$ law; Coulomb ...
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Nuclear Burning in Stellar Interiors

1992
The nuclear reactions in the stellar interior do not only produce the energy to make the star shine but also transform elements into others, like chemical reactions transform molecules into other molecules. As an example, we can consider the reaction $$ {}^{12}{\rm{C}} + {}^{{\rm{16}}}{\rm{O}} \to {}^{24}{\rm{Mg}} + {}^4{\rm{He}} $$ One 12C ...
C. W. H. De Loore, C. Doom
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The Physics of Stellar Interiors

Physics Bulletin, 1975
V C Reddish Edinburgh: Edinburgh University Press 1974 pp vii + 107 price £3 Written at an undergraduate/postgraduate level, this book is based on a course of lectures given by Dr Reddish to astronomy students at the Case-Western Reserve University, Cleveland, Ohio, in the spring of 1969. Part one of the book deals with the structure, energy generating
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