Dust shells around Miras and OH/IR stars - Interpretation of IRAS and other infrared measurements

Details Dust shells around Miras and OH/IR stars - Interpretation of IRAS and other infrared measurements Dust shells around Miras and OH/IR stars - Interpretation of IRAS and other infrared measurements

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...186..136b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 186, no. 1-2, Nov. 1987, p. 136-152.

Astronomy and Astrophysics

Astrophysics

207

Infrared Stars, Interstellar Matter, Mira Variables, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Density Distribution, M Stars, Stellar Models

Scientific paper

It is shown that the locus of optical M-type Miras and OH/IR variables in the IRAS two-color diagram can be modelled by a sequence of single-shell dust shells of varying optical depth (mass loss rate) with inner radii such that the dust temperature at the inner boundary is the same for all models. The dependence of a theoretical two-color sequence on model parameters is investigated. Also, fits to the spectrum of OH 26.5+0.6 are given which might indicate an observable increase of the mass loss rate for this source during the past evolution. It is demonstrated that the position of the non-variable sources in the IRAS two-color diagram can be understood in terms of a sequence of dust shells, whose inner radii are progressively larger than those of the models mentioned above. It is suggested that these sources therefore represent an evolutionary phase shortly after the cessation of pulsation and of mass loss of the central star and before the formation of a planetary nebula. A model fit to the spectrum of OH 17.7-2.0 indicates that the mass loss does not stop "abruptly".

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