Models for IRAS observations of circumstellar dust shells around late-type stars

Details Models for IRAS observations of circumstellar dust shells around late-type stars Models for IRAS observations of circumstellar dust shells around late-type stars

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..273r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Sept. 15, 1986, p. 273-286.

Astronomy and Astrophysics

Astronomy

114

Cosmic Dust, Infrared Astronomy Satellite, Late Stars, Spaceborne Astronomy, Stellar Envelopes, Stellar Models, Carbon Stars, Grain Size, M Stars, Molecular Clouds, Spectrum Analysis, Stellar Atmospheres

Scientific paper

IRAS observations of circumstellar dust shells around late-type stars are compared with the models of Rowan-Robinson and Harris (1982, 1983). IRAS data at 12 and 25 μm agree well with previous observations and with the models. A discussion of the environment of late-type stars shows that one should expect the outflow to be halted at a distance r2 ≡ 1717to 1018cm from the star. A value for the ratio of the inner to outer radii of the dust shell, r1/r2 = 0.001, has therefore been adopted for most of the theoretical models discussed. For carbon stars the IRAS data at 60 and 100 μm agree reasonably with the predictions of the models. For M stars the IRAS data at 60 and 100 μm require that the grain absorption efficiency Qν ∝ ν between 20 - 30 and 100 μm. A few stars show excess 100 μm radiation, which probably arises from a shell of dust at the zone where the wind from the star runs into the interstellar gas.

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