V = 3, J = 1-0 SiO maser emission from evolved stars

Details V = 3, J = 1-0 SiO maser emission from evolved stars V = 3, J = 1-0 SiO maser emission from evolved stars

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...211..187a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 211, no. 1, Feb. 1989, p. 187-198. Research supported by CAICYT.

Astronomy and Astrophysics

Astronomy

33

Infrared Sources (Astronomy), Interstellar Masers, Mira Variables, Silicon Oxides, Supergiant Stars, Polarized Radiation, Radio Telescopes, Spectral Line Width, Stellar Atmospheres, Stellar Envelopes

Scientific paper

The 14-m radiotelescope at the Centro Astronomico de Yebes was used to search, from August 1986 to February 1988, for v = 3, J = 1-0 SiO maser line from numerous long-period variables, including 31 Mira variables, six supergiants, one semiregular, and one IR object. This maser line was detected in six new emitters, including RR Aql, V Cam, R Cas, microCep, U Her, and R LMi, as well as in seven that were previously reported. The SiO line was monitored for one and a half year in three sources, and the degree of linear polarization of the emission was estimated in two stars. The results of these observations indicate that the v = 3 line is about 35 times weaker in peak flux, 65 times weaker in profile area, and significantly narrower than the v = 1,2 lines. On the other hand, the variability and the degree of polarization are similar in these three lines. These results are compatible with the SiO masers being located in the circumstellar envelope.

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