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Mathematical Proceedings of the Cambridge Philosophical Society, 1939
Difficulties associated with the evolution of stars by radiation alone are briefly discussed. It is clear that some other process is also affecting the stars and it is shown that the stars are capable of adding to their mass by the process of accretion of the cosmical cloud.
R. A. Lyttleton, Fred Hoyle
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Difficulties associated with the evolution of stars by radiation alone are briefly discussed. It is clear that some other process is also affecting the stars and it is shown that the stars are capable of adding to their mass by the process of accretion of the cosmical cloud.
R. A. Lyttleton, Fred Hoyle
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On Stars, Their Evolution and Their Stability
Science, 1984The Nobel lecture of Chandrasekhar is printed in which he describes the basic processes that determine the life history of a star with particular emphasis on the roles of stellar mass and radiation pressure. (AIP)
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2002
After seminal studies [229], the calculations of stellar evolution have been performed by various groups of researchers in a wide mass range with use of increasingly more powerful computers. There is presently (2001) a general understanding of the nuclear evolution of a star from the main sequence to a white dwarf, neutron star or black hole formation.
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After seminal studies [229], the calculations of stellar evolution have been performed by various groups of researchers in a wide mass range with use of increasingly more powerful computers. There is presently (2001) a general understanding of the nuclear evolution of a star from the main sequence to a white dwarf, neutron star or black hole formation.
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1989
The term massive star is not very precise, and in the following we shall use it for stars with zero age main sequence (ZAMS) masses M ZAMS above approximately 15 M ⊙. Note, however, that these abjects may achieve actual masses well below 15 M ⊙ during their evolution, as a consequence of mass loss due to stellar winds, pulsations, or other processes. M
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The term massive star is not very precise, and in the following we shall use it for stars with zero age main sequence (ZAMS) masses M ZAMS above approximately 15 M ⊙. Note, however, that these abjects may achieve actual masses well below 15 M ⊙ during their evolution, as a consequence of mass loss due to stellar winds, pulsations, or other processes. M
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2004
Supernovae are of wide interest to the astronomical community because they play a key role in the nucleosynthetic evolution of galaxies, stellar remnant populations, the energetics and phase balance of the interstellar medium (ISM), the interpretations of observations of distant galaxies, models of galaxy formation and evolution, the physics of star ...
David Arnett, Patrick A. Young
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Supernovae are of wide interest to the astronomical community because they play a key role in the nucleosynthetic evolution of galaxies, stellar remnant populations, the energetics and phase balance of the interstellar medium (ISM), the interpretations of observations of distant galaxies, models of galaxy formation and evolution, the physics of star ...
David Arnett, Patrick A. Young
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1984
The formation of a nebula is one stage in the evolution of most stars. If the evolution of a star from its formation to the time when its energy sources are exhausted were completely understood, it might be possible to show why a nebula is ejected and under what conditions a star produces this nebula.
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The formation of a nebula is one stage in the evolution of most stars. If the evolution of a star from its formation to the time when its energy sources are exhausted were completely understood, it might be possible to show why a nebula is ejected and under what conditions a star produces this nebula.
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