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Radio and Infrared Observations of OH/IR Stars

Sargent, Anneila I. and Baud, Boudewijn (1985) Radio and Infrared Observations of OH/IR Stars. In: Mass Loss from Red Giants. Astrophysics and Space Science Library. No.117. Springer Netherlands , Dordrecht, pp. 213-214. ISBN 9789401088961.

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Combined infrared and OH spectral line observations are essential to understanding the nature of OH/IR stars, the properties of their circumstellar envelopes and the OH maser pump mechanism. We have used the Very Large Array of the National Radio Astronomy Observatory to determine very precise radio positions for a selection of such objects near the tangential point and at the galactic center and have subsequently made simultaneous infrared and OH observations of both samples. From the infrared measurements, luminosities of these stars and masses of the thick dust shells which surround them have been derived, while the double-peaked OH emission line profiles have yielded both the stellar radial velocities, v_R, and the expansion velocities of the envelopes, v_e, as well as the maser luminosities. The selection criteria and the observations are described in detail elsewhere (Baud et al. 1984). The results are consistent with these stars lying at the top of the Asymptotic Giant Branch (AGB) of the Hertzsprung-Russell diagram; the dense circumstellar shells suggest that these objects are evolving rapidly through a phase of high mass loss.

Item Type:Book Section
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URLURL TypeDescription ReadCube access
Sargent, Anneila I.0000-0002-4633-5098
Additional Information:© D. Reidel Publishing Company 1985.
Subject Keywords:Mass Loss Rate; Galactic Center; Expansion Velocity; Asymptotic Giant Branch; High Mass Loss
Series Name:Astrophysics and Space Science Library
Issue or Number:117
Record Number:CaltechAUTHORS:20201001-145811098
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105733
Deposited By: George Porter
Deposited On:02 Oct 2020 15:24
Last Modified:16 Nov 2021 18:45

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