Circumstellar Dust in Mira Variables and the Mass Loss Mechanisms

Details Circumstellar Dust in Mira Variables and the Mass Loss Mechanisms Circumstellar Dust in Mira Variables and the Mass Loss Mechanisms

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...273..570a&link_type=abstract

Astronomy and Astrophysics, Vol.273, NO. 2/JUNII, P. 570, 1993

Astronomy and Astrophysics

Astrophysics

13

Catalogs: Iras, Circumstellar Matter, Stars: Mass Loss, Stars: Asymptotic Giant Branch, Dust, Stars: Infrared

Scientific paper

IRAS data on 92 oxygen-rich Mira variables are analysed to evaluate the role of pulsations in mass loss among these stars. Using a radiative model, equilibrium temperature, size, mass, and optical depth of circumstellar dust shells have been estimated. A two-component dust shell model was found necessary for fitting the photometric data. The LRS data required only a single shell which agrees very well with the inner hotter shell obtained from the photometric data. The mass of the inner shell shows a positive correlation with the pulsation period while that of the outer shell shows no such correlation. We suggest that the outer shell is a result of the mass loss during the pre-AGB stage while the inner shell represents AGB mass loss caused by pulsation with the possible support of radiation pressure. Dust was estimated to condense at ˜3-10R* lending support to the two-step process of mass loss involving the pulsations and radiation pressure. The recently reported variability of far infrared fluxes during pulsation period does not seem to alter these results significantly.

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