Observations of OH and H2O microwave maser emission from VY Canis Majoris

Details Observations of OH and H2O microwave maser emission from VY Canis Majoris Observations of OH and H2O microwave maser emission from VY Canis Majoris

May 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222..132r&link_type=abstract

Astrophysical Journal, Part 1, vol. 222, May 15, 1978, p. 132-139.

Astronomy and Astrophysics

Astronomy

40

Hydroxyl Emission, Microwave Emission, Supergiant Stars, Water Masers, Infrared Astronomy, Power Spectra, Stellar Envelopes, Stellar Mass Ejection, Time Response, Very Long Base Interferometry

Scientific paper

VLBI observations of the H2O emission from VY CMa made in 1974 and 1976 show the diameter of the masing region to be about 5 times 10 to the fifteenth power cm, and the diameters of the individual components to be about 5 times 10 to the thirteenth power, and the density is about 10 to the ninth power per cu cm. The H2O and main-line OH maser spectra from single antenna measurements show substantial changes within a few months. These changes may be correlated with changes in the optical spectrum. Expanding-shell models, with emission from both the limbs and the direction along the line of sight to the star, can explain the observations.

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