Physics
Scientific paper
Aug 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991anpcs..16..459m&link_type=abstract
Ann. Phys. (Paris) Colloq., Vol. 16, No. 4, p. 459 - 479
Physics
White Dwarfs: Stellar Evolution, Formation: Black Holes, Formation: Neutron Stars, Stellar Evolution: Stellar Masses
Scientific paper
As is well known a star may end its nuclear lifetime as a white dwarf, neutron star, black hole or many, in certain circumstances, leave no remnant at all. The main question to be addressed in this review is the following: what are the progenitors of these different final stages? After a brief review of the major physical principles governing stellar evolution, the author presents the different evolutionary scenarios resulting from numerical calculations. Particular attention will be paid to the effect of mass loss on theoretical determinations of the mass limits MWD and MBH which are respectively the maximum initial mass leading to the formation of a white dwarf and the minimum initial mass for the formation of a black hole. The author terminates this review by the presentation of some relevant observational results. The bulk of this paper is devoted to the discussion of the evolution of single Population I stars.
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