Non-radial instability of WR models

Details Non-radial instability of WR models Non-radial instability of WR models

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...161..125n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 161, no. 1, June 1986, p. 125-129.

Astronomy and Astrophysics

Astrophysics

24

Stellar Evolution, Stellar Oscillations, Supermassive Stars, Wolf-Rayet Stars, Adiabatic Conditions, Stellar Mass Ejection, Stellar Models, Vibration Mode

Scientific paper

The development of a H burning shell in a massive star evolving with mass loss triggers a phase of vibrational instability towards g+ modes of non radial oscillations. The e-folding time is of the order of 1000 yr but the unstable phase lasts only about 5 times more. Although the periods seem in accordance with those observed in some WR stars, it is still not clear that such a short unstable phase could be responsible for the observed variability.

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