Other
Scientific paper
Oct 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.282.1359h&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 282, Issue 4, pp. 1359-1371.
Other
37
Hydrodynamics, Masers, Stars: Variables: Other
Scientific paper
A hydrodynamic pulsation model for long-period M-type Mira variables is used to estimate the physical conditions of number density, temperature and velocity field in the circumstellar envelope of a model star of 1M_solar, 332-d period, surface temperature 3000K and mass-loss rate 1.8x10^-7 M_solar yr^-1. These conditions have previously been used in a model of SiO masers to establish, for a single stellar phase, the nature and location of the zone in which SiO masers should form. Using Monte Carlo techniques, a synthetic image of 43-GHz emission is generated, showing that masers are predicted to form in an approximate ring 1 to 2 stellar radii from the photosphere, in agreement with the results of recent very long baseline interferometry (VLBI) observations. A new image of SiO masers around TX Cam, obtained using the Very Long Baseline Array (VLBA), is presented, which shows these characteristics. Models show that masers do not form in the region in which the stellar wind is fully developed. Amplification is dominated by tangential paths through the limbs of the circumstellar envelope. Synthetic lineshapes for a variety of maser transitions show structure and linewidths that are typical of observed lineshapes.
Bowen Garry
Diamond Phil J.
Field David
Gray Malcolm D.
Humphreys E. M. L.
No associations
LandOfFree
SiO masers in Mira variables at a single stellar phase 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 SiO masers in Mira variables at a single stellar phase, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and SiO masers in Mira variables at a single stellar phase will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1137699