Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.6304b&link_type=abstract
American Astronomical Society, 189th AAS Meeting, #63.04; Bulletin of the American Astronomical Society, Vol. 28, p.1352
Astronomy and Astrophysics
Astronomy
Scientific paper
SiO maser emission provides a unique probe of both the kinematics and magnetic field structure in the extended atmospheres of late-type stars. Recent Very Long Baseline Interferometry (VLBI) observations of the SiO masers towards several late-type stars show that they are confined to a narrow ring-like morphology and typically lie within 2--4 stellar radii of the center of the star. Using NRAO's Very Long Baseline Array (VLBA), we have obtained 5 epochs of full-polarization observations of the v=1, J=1-0 SiO maser emission towards the Mira variable in the symbiotic binary R Aqr. These observations occurred at various phases in the stellar pulsation cycle allowing us to monitor variations in both the structure and the polarization of the maser emission with time. We find the SiO masers towards R Aqr lie in a ring-like distribution with a radius of ~ 3.5 AU ( ~ 2 R_{*}). In addition, both the polarization and the structure of the maser emission vary significantly over timescales of ~ 1--2 months.
Boboltz David A.
Diamond Phil J.
Kemball Athol J.
No associations
LandOfFree
Observations of the 43-GHz SiO Maser Emission in the Atmosphere of R AQR does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Observations of the 43-GHz SiO Maser Emission in the Atmosphere of R AQR, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Observations of the 43-GHz SiO Maser Emission in the Atmosphere of R AQR will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-817443