Evolution of Iron Stars ---Gravitational Contraction and the Decomposition of Iron---

Details Evolution of Iron Stars ---Gravitational Contraction and the Decomposition of Iron--- Evolution of Iron Stars ---Gravitational Contraction and the Decomposition of Iron---

Feb 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970pthph..43..319n&link_type=abstract

Progress of Theoretical Physics, Vol. 43, No. 2, pp. 319-333

Physics

9

Scientific paper

The evolution of iron stars in the phases of gravitational contraction and collapse is studied with an automatic computation method for the stellar masses 2.6M&sun; and 10M&sun;. The computation is made for the two alternative cases with and without neutrino production by electron-neutrino interaction. For the stages before the stars become unstable because of the iron-helium phase transition, the features of evolution are essentially the same as those of carbon stars which have previously been computed by Murai, Sugimoto, Hōshi and Hayashi. Only for the cases with neutrinos, a further evolution has been computed until the central density becomes as high as 1 × 1011 g/cm^3. As soon as the iron-helium phase change occurs in the central region, the stars begin to collapse and the evolution becomes almost adiabatic. It is found that the collapse of the star of 2.6M&sun; is initiated not by the instability due to electron capture, contrary to the conclusion of Savedoff, Van Horn and Vila, but by the iron-helium transition.

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