OH/IR star color mimics

Details OH/IR star color mimics OH/IR star color mimics

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...396..251l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 396, no. 1, Sept. 1, 1992, p. 251-266. Research supported by National Astro

Astronomy and Astrophysics

Astronomy

30

Hydroxyl Emission, Infrared Stars, Interstellar Masers, Stellar Color, Stellar Envelopes, Astronomical Catalogs, Companion Stars, Infrared Astronomy Satellite

Scientific paper

IR color criteria are used to select potential OH/IR stars from the IRAS Point Source Catalog. These OH/IR star color mimics, despite often having thick and demonstrably O-rich dust shells to shield their molecules against interstellar UV, have no 1612 MHz masers. The most likely reason for this is that these stars have degenerate companions, which collect an accretion disk from the red giant wind, which in turn provides them with a local source of UV to dissociate molecules from within their dust shells. In some cases this self-generated UV is sufficient to excise all molecules from a shell, as happens with symbiotic novae; in some cases it merely reduces their number and the ability of a shell to support a maser. It is suggested that D-type symbiotic stars can be identified among sources with thick opaque dust shells by a persistent absence of appropriate masers: these are the OH/IR color mimics.

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