Physical Processes in Astrophysics: Proceedings of a Meeting by Ian W. Roxburgh, Jean-Louis Masnou
By Ian W. Roxburgh, Jean-Louis Masnou
This quantity, in honour of Evry Schatzman, includes in-depth stories on vital subject matters of recent astrophysics, resembling stellar physics, masking stellar evolution, sunlight neutrinos, stellar rotation and spin down, convection shipping tactics, neutron stars, white dwarfs, and novae. the entire talks got through prime specialists who had time either to advance the fundamentals in their topic and to hide fresh paintings. the quantity is intended for either graduate scholars and researchers.
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Additional info for Physical Processes in Astrophysics: Proceedings of a Meeting in Honour of Evry Schatzman Held in Paris, France, 22 - 24 September 1993
Astrophys. : 1994, Mon. Not. R. : 1988, Mon. Not. R. , Julian. : 1970, Astrophys. : 1991, Astrophys. : 1993, Mon. Not. R. : 1955, Zeits. f. Astrophys. : 1967a, Mere. Soe. Roy. Sci. : 1967b, in Plasma astrophysics, ed. P. A. : 1968, Mon. Not. R. : 1984, Astron. : 1987, Mon. Not. R. : 1990, Mon. Not. R. : 1989, Mon. Not. R. : 1991, in The Sun and cool stars: activity, magnetism, dynamos, eds. I. Tuominen, D. Moss, G. : 1985, Astron. Astrophys. : 1962, Ann. Astrophys. : 1972, Astrophys. 171, 565 47 12 L.
The unit used for the three radiochemical experiments is a S N U = 10 -z6 events per target atom per second. The result for the Kamiokande water experiment is expressed, following the experimentalists, in terms of a ratio to the predicted event rate. The errors shown are, in all cases, effective lrr uncertainties, where I have combined quadratically the quoted statistical and systematic errors. I will use throughout this review the standard solar model results of Bahcall and Pinsolmeault (Bahcall 1992) since this is the only standard solar model published so far to take account of 22 Solar Neutrinos: What We Have Learned 5 helium diffusion.
Nucl. , 44, 544. I. , 1986, Soy. Phys. JETP, 64, 446. , 1978, Phys. Rev. D, 17, 2369. , 1979, Phys. Rev. D, 20, 2634. 36 A n g u l a r M o m e n t u m Loss M e c h a n i s m s and Stellar S p i n - d o w n L. Mestel Astronomy Centre, Division of Physics and Astronomy, University of Sussex, Falmer, Brighton BN1 9QH, England A b s t r a c t : The theory of magnetic braking by a thermo-centrifugal stellar wind is summarized. The basic result - "effective corotation" out to the Alfv6n surface yields approximate laws for the spin-down of late-type stars, if one adopts a simple phenomenological dynamo relation between magnetic flux and angular velocity, and a similar relation between mass loss and magnetic flux.