Stellar mass loss and pulsation

Details Stellar mass loss and pulsation Stellar mass loss and pulsation

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988stia...8945268w&link_type=abstract

IAU, Colloquium on the Use of Pulsating Stars in Fundamental Problems of Astronomy, 111th, Lincoln, NB, Aug. 15-17, 1988, Paper.

Astronomy and Astrophysics

Astronomy

Asymptotic Giant Branch Stars, Mira Variables, Stellar Evolution, Stellar Mass Ejection, Stellar Oscillations, Cepheid Variables, Late Stars, Planetary Nebulae, Pre-Main Sequence Stars, Stellar Winds

Scientific paper

Mass loss at rates sufficient to alter the evolution of stars is known to occur during the pre-main sequence evolution of most stars; on the main sequence for massive stars; and during advanced evolutionary phases when the luminosity is high and the effective temperature is low. While most investigations of the effects of mass loss on stellar evolution have assumed continuous (parameterized) mass loss laws apply, there is increasing evidence that mass loss rates are substantially higher for stars that are pulsating with large amplitude and/or in selected modes. Some new insights into the mass loss that terminates the AGB evolution of intermediate mass stars, and leads to the formation of planetary nebulae, come from recent detailed studies of the mass loss process from the Mira variables.

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