Origin and propagation of shocks in the atmospheres of Mira-type stars

Details Origin and propagation of shocks in the atmospheres of Mira-type stars Origin and propagation of shocks in the atmospheres of Mira-type stars

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..283..137r&link_type=abstract

In: Mass-losing pulsating stars and their circumstellar matter. Workshop, May 13-16, 2002, Sendai, Japan, edited by Y. Nakada, M

Astronomy and Astrophysics

Astrophysics

Mira Variables, Shocks, Extrasolar Planets

Scientific paper

In Mira-type stars the optical emission lines and molecular maser lines (SiO, H2O, OH) probe different layers of the stellar atmospheres and circumstellar envelopes, affected by shock waves. Balmer emission appears slightly above the stellar photosphere. As the shock reaches the masering region in the circumstellar envelope, the SiO and H2O maser intensity grows. The lack of the radio continuum, expected to accompany the Hα emission in Miras, probably indicates that the source of the Balmer emission lines is small, e.g., connected with an active region on the star or with a shock generated by a close low-mass companion.

Affiliated with

Also associated with

No associations

Rating

Origin and propagation of shocks in the atmospheres of Mira-type stars 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 Origin and propagation of shocks in the atmospheres of Mira-type stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Origin and propagation of shocks in the atmospheres of Mira-type stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-920540