SiO isotopic maser emission from VY Canis Majoris

Journal Article · Sat Jan 15 04:00:00 EST 1983 · Astrophys. J., Lett. Ed.; (United States)

DOI:https://doi.org/10.1086/183945· OSTI ID:6269528

Deguchi, S; Good, J; Fan, Y; Mao, X; Wang, D; Ukita, N

We have detected strong maser emission from VY CMa in the /sup 29/SiO J = 2--1, v = 0 transition. The intensity of the /sup 29/SiO emission is about twice that of the ground-state /sup 28/SiO maser emission which we have also measured. We also looked for /sup 30/SiO emission, but none was detected. Both the /sup 28/SiO and /sup 29/SiO emission profiles have been measured on occasions separated by as much as 3 months, and no variability has been detected in the detailed structure of the lines above the level of the noise. The radial velocities of the masers in VY CMa are close to the central star velocity as derived from the OH 1612 MHz double-peaked maser emission and the broad /sup 28/SiO weak emission. One possible explanation for this is that the maser emission comes from a rotating disk around the central star.

• Research Organization: Five College Radio Astronomy Observatory, University of Massachusetts, Amherst
• OSTI ID: 6269528
• Journal Information: Astrophys. J., Lett. Ed.; (United States), Journal Name: Astrophys. J., Lett. Ed.; (United States) Vol. 264:2; ISSN AJLEA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
AMPLIFIERS
CHALCOGENIDES
ELECTRONIC EQUIPMENT
EMISSION
ENERGY LEVELS
ENERGY-LEVEL TRANSITIONS
EQUIPMENT
GROUND STATES
ISOTOPES
MASERS
MICROWAVE AMPLIFIERS
MICROWAVE EQUIPMENT
OXIDES
OXYGEN COMPOUNDS
RADIAL VELOCITY
SILICON COMPOUNDS
SILICON ISOTOPES
SILICON OXIDES
STARS
VELOCITY