Interferometric observations of non-maser SiO emission from circumstellar envelopes of AGB stars - Acceleration regions and SiO depletion

Details Interferometric observations of non-maser SiO emission from circumstellar envelopes of AGB stars - Acceleration regions and SiO depletion Interferometric observations of non-maser SiO emission from circumstellar envelopes of AGB stars - Acceleration regions and SiO depletion

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105..595s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 2, p. 595-607.

Astronomy and Astrophysics

Astronomy

35

Asymptotic Giant Branch Stars, Image Resolution, Interferometers, Mira Variables, Silicon Oxides, Stellar Envelopes, Brightness Distribution, Interstellar Masers, Radiative Transfer, Stellar Mass Ejection

Scientific paper

High- and medium-resolution images of SiO J = 2-1(V = 0) from the circumstellar envelopes (CSEs) of three oxygen-rich stars, Chi Cyg, RX Boo, and IK Tau, were obtained. The SIO images were found to be roughly circular, implying that the CSEs are spherically symmetric on angular-size scales of about 3-9 arcsec. The observed angular half-maximum intensity source radius is nearly independent of the LSR velocity for all three CSEs. Chi Cyg and RX Boo are argued to be less than 450 pc distant, and have mass-loss rates larger than about 10 exp -6 solar mass/yr. In Chi Cyg and RX Boo, the line profiles at the peak of the brightness distribution are rounded, typical of optically-thick emission from a spherical envelope expanding with a constant velocity. In the IK Tau line profiles, an additional narrower central component is present, probably a result of emission from an inner circumstellar shell with a significantly smaller expansion velocity than the extended envelope.

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