Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...167...61h&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 167, no. 1, Oct. 1986, p. 61-76.
Astronomy and Astrophysics
Astrophysics
91
B Stars, Hertzsprung-Russell Diagram, Neutron Stars, Stellar Evolution, Stellar Mass, Supergiant Stars, Abundance, Stellar Cores
Scientific paper
The evolution of single helium stars is calculated from the helium zero age main sequence up to neon ignition in the core for stellar masses of 2.2 M_sun;, 2.5 M_sun;, 2.9 M_sun;, 3.2 M_sun;, 3.5 M_sun;, and 4.0 M_sun;. For a 2.0 M_sun; helium star the evolution is calculated from the helium zero age main sequence, through ignition of carbon in the core (off-centre), up to the time when the convective carbon-burning shell reaches the centre. The aim of this investigation is: to determine the lower mass limit for neutron star formation by helium star evolution. This mass limit is found here to be most likely lower than the mass limit above which neon ignites in the core of a helium star (2.2 M_sun;). The evolutionary tracks in the pc, Tc plane and in the HR diagram are intercompared and are also compared with tracks calculated by other investigators.
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