Volume 381, Number 2, JanuaryII 2002
|Page(s)||491 - 499|
|Section||Interstellar and circumstellar matter|
|Published online||15 January 2002|
Nature of OH maser and SiO thermal emission towards carbon star: IRAS 05373–0810 (V1187 Ori)*
N. Copernicus Astronomical Center, Rabiańska 8, 87–100 Toruń, Poland
2 Yunnan Astronomical Observatory, National Observatory, CAS, Kunming 650011, PR China
3 Toruń Centre for Astronomy, Nicolaus Copernicus University, Gagarina 11, 87–100 Toruń, Poland
4 Institut d'Astrophysique, 98bis boulevard Arago, 75014 Paris, France
Corresponding author: R. Szczerba, firstname.lastname@example.org
Accepted: 23 October 2001
We present observational evidence that IRAS 05373–0810 is a genuine carbon star with an ISO SWS spectrum closely resembling that of R Scl. Modelling of the spectral energy distribution of IRAS 05373–0810 suggests that the star has luminosity of order of 8000 and loses mass at a rate of about yr-1. The detected OH maser emission at 1612, 1665 and 1667 MHz and SiO thermal emission at 86.85 GHz towards IRAS 05373–0810 is not associated with this source. The available observations imply that these lines, typical for O–rich sources, come from the molecular cloud L 1641 in the Orion star forming region (OH) and, very likely, from the NGC 2149 molecular complex (SiO).
Key words: stars: AGB and post–AGB, carbon, individual: IRAS 05373–0810 / ISM: dust, extinction
© ESO, 2002
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