A long-term study of SiO (v = 1, J = 2-1) maser emission from evolved stars and Orion A

Details A long-term study of SiO (v = 1, J = 2-1) maser emission from evolved stars and Orion A A long-term study of SiO (v = 1, J = 2-1) maser emission from evolved stars and Orion A

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...158...67n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 158, no. 1-2, April 1986, p. 67-82.

Astronomy and Astrophysics

Astrophysics

70

Late Stars, Maser Outputs, Orion Nebula, Silicon Dioxide, Variable Stars, Average, Mira Variables, Radial Velocity, Temporal Distribution, Water Masers

Scientific paper

General characteristics of eight late-type stars and Orion A in the SiO (v = 1, J = 2-1) maser line are reported based on observations made with the 20-m Onsala telescope between 1977 and 1984. Five stars show periodic maser flux variations that are well correlated with the infrared light curve, and the maximum SiO intensity and the dynamic range vary significantly between different periods and sources. Some long-term variations in the center velocity of the maser emission have been noted, with Omicron Cet possibly being a member of a binary system. Grand averages have been used to study the general velocity structure, and a global SiO (v = 1, J = 2-1) profile for Mira variables shows that the strongest emission is blueshifted with respect to the stellar velocity, while as a whole the emission is redshifted. The analysis places the SiO masers in a region between the pulsating stellar atmosphere and the expanding circumstellar envelope, where the velocity structure bears no relation to the expansion velocity of the shell.

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