Vibrational Instability of Population III Low-Mass Stars due to the ɛ-Mechanism

Details Vibrational Instability of Population III Low-Mass Stars due to the ɛ-Mechanism Vibrational Instability of Population III Low-Mass Stars due to the ɛ-Mechanism

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011pasj...63...95s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.63, No.1, pp.95--104

Astronomy and Astrophysics

Astronomy

4

Instabilities, Stars: Abundances, Stars: Evolution, Stars: Interiors, Stars: Oscillations

Scientific paper

The linear vibrational instability of population III low-mass stars due to the ɛ-mechanism was investigated against g modes by using the quasi-adiabatic approximation. Since, contrary to the case of population I stars, such stars (M ≳ 1Modot) have no convective envelope, a definite conclusion of the stability is obtained. It is found that stars with M ≲ 5Modot become unstable during the main-sequence stage against the dipole g1, g2, and g3 modes due to the ɛ-mechanism of3He-3He reaction. The e-folding time of the instability is on the order of 107 yr, and is much shorter than the evolutionary timescale. It is thus expected that the instability grows to a finite size and induces material mixing, which has a significant influence on the later evolution of these stars.

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