The life and times of an intermediate mass star - In isolation/in a close binary

Details The life and times of an intermediate mass star - In isolation/in a close binary The life and times of an intermediate mass star - In isolation/in a close binary

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985qjras..26....1i&link_type=abstract

Royal Astronomical Society, Quarterly Journal (ISSN 0035-8738), vol. 26, March 1985, p. 1-39.

Astronomy and Astrophysics

Astronomy

61

Binary Stars, Main Sequence Stars, Stellar Evolution, Asymptotic Giant Branch Stars, Capture Effect, Cepheid Variables, Hertzsprung-Russell Diagram, Nuclear Fusion, Planetary Nebulae, Stellar Envelopes, Stellar Oscillations, Stellar Winds, Supernovae, White Dwarf Stars

Scientific paper

A review is given of the properties of intermediate mass (1 < M/M_sun; < 9) single stars as they evolve through the initial stages of gravitational contraction on to the main sequence and then through various stages at rates controlled by hydrogen- and helium-burning reactions. Colourful events which punctuate the life of such stars include: the core helium flash (M ⪉ 2.3 M_sun;); acoustical pulsations as RR Lyrae or Cepheid stars during core helium burning; thermal pulses (also known as helium shell flashes) on the asymptotic giant branch where carbon and s-process isotopes are produced and thereupon brought to the surface whence they are expelled into the interstellar medium by a strong wind; ejection of a planetary nebula and excitation of this nebula by a final remnant which either (1) ultimately becomes a DA white dwarf exhibiting hydrogen at its surface (75 per cent of the time) or (2) experiences a final helium shell flash (25 per cent of the time), briefly becomes a born-again asymptotic giant branch star, re-excites the surrounding nebular shell, and loses the final vestiges of surface hydrogen to become ultimately a non-DA white dwarf.

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