[Previous] | [Session 74] | [Next]
T.A. Ostrowski-Fukuda, R.E. Stencel (University of Denver), A. Kemball (NRAO), P.J. Diamond (MERLIN/VLBI National Facility)
The Very Long Baseline Array (VLBA) has been used to monitor the 43-GHz SiO (v=1, J=1-0) maser emission in the supergiant star S Persei monthly since 1999. SiO masers act as probes of the gas motions and magnetic fields of this star allowing us to investigate its extended atmosphere. Here we report the continuing results of this on-going project. Many epochs of data have been reduced and pieced together in a time-lapse movie fashion, allowing us to follow the motions of the individual maser regions. The trajectories and velocities of the SiO masers are investigated. Our findings from S Per are compared to TX Cam, which has been studied in the same fashion. We are most interested in learning out about the structure, time evolution, mass-loss process, magnetic field structure, and the physical conditions in the inner regions of these types of stars. Just as in the case of TX Cam, we have found that our images reveal that the mass loss may not be the same for all regions of the star’s surface. This work is supported by the Menzel Scholarship Fund at the University of Denver, and in conjunction with the National Radio Astronomy Observatory, Socorro, NM.
If you would like more information about this abstract, please follow the link to http://www.du.edu/~tostrows/AASJune02.htm. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
The author(s) of this abstract have provided an email address for comments about the abstract: tostrows@du.edu
[Previous] | [Session 74] | [Next]
Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.