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Giant and supergiant stars with degenerate neutron cores
Eich, Chris; Zimmermann, Mark E.; Thorne, Kip S.; Zytkow, Anna N.
AA(California Institute of Technology, Pasadena), AB(California Institute of Technology, Pasadena), AC(California Institute of Technology, Pasadena), AD(Queen Mary College, London; Cambridge, University, England)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 346, Nov. 1, 1989, p. 277-283. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Degenerate Matter, Giant Stars, Neutron Stars, Nuclear Astrophysics, Stellar Cores, Supergiant Stars, Astronomical Models, Gravitational Effects, Neutrinos, Stellar Envelopes, Stellar Luminosity
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Two classes of Thorne-Zytkow (TZ) stellar models are investigated: the giant models with low-mass envelopes and gravitational energy generation, and the super giant ones with more massive envelopes and nuclear energy generation. Bisnovatyi-Kogan and Lamzin (1984) argue that there is a flaw in the TZ match of the giant star's envelope onto their cores, that no equilibrium giant models will be possible when this flaw is corrected, and that such giant stars will turn out to die quickly via runaway neutrino losses and catastrophic contraction. The paper shows that Bisnovatyi-Kogan and Lamzin are mistaken: there is no flaw in the match to the core; fully self-consistent equilibrium models do exist; and the structure of those models suggests that they will be stable against neutrino-loss-triggered contraction. By contrast, there are genuine difficulties with the TZ supergiant models because their hot CNO cycle nuclear reactions get hung up waiting for beta-decays and thus have difficulty generating enough energy for hydrostatic support. An unsuccessful attempt to build self-consistent supergiant models based on a nonequilibrium hot CNO cycle is described.

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Database: Astronomy
arXiv e-prints