From wind to superwind - The evolution of mass-loss rates for Mira models

Details From wind to superwind - The evolution of mass-loss rates for Mira models From wind to superwind - The evolution of mass-loss rates for Mira models

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...375l..53b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 375, July 10, 1991, p. L53-L56.

Astronomy and Astrophysics

Astrophysics

169

Asymptotic Giant Branch Stars, Mira Variables, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Stellar Winds, Cosmic Dust, Metallicity, Stellar Atmospheres, Stellar Envelopes, Stellar Luminosity

Scientific paper

Dynamical atmosphere models were calculated for a large grid of variables with Mira-like properties satisfying the Iben radius-luminosity-mass relationship for evolving AGB stars. Their masses ranged from 0.7 to 2.4 solar masses, and their periods from 150 to 800 days. All were fundamental-mode pulsators, had solar metallicity, and included effects of dust. The mass-loss rate increases as an approximately exponential function of time, reaching 0.00001-0.0001 solar masses/yr. Further evolution is dominated by the powerful wind, which strips the star's envelope from the core. This 'superwind', a remarkably robust effect, occurs for all initial stellar masses and all modeling parameters that have been tested. Models with very low metallicity also show the effect, but at higher luminosities, which has intriguing implications for the number of supernovae in early low-metallicity populations and for the chemical evolution of galaxies.

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