Spectral evolution of the H2O maser in late-type stars

Details Spectral evolution of the H2O maser in late-type stars Spectral evolution of the H2O maser in late-type stars

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..629t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 6, p. 629-642

Astronomy and Astrophysics

Astronomy

31

Astronomical Models, Interstellar Masers, M Stars, Mira Variables, Silicon Oxides, Stellar Envelopes, Stellar Physics, Water Masers, Data Bases, Emission Spectra, Infrared Astronomy Satellite, Line Spectra, Radio Telescopes, Red Shift, Stellar Evolution

Scientific paper

We have carried out almost simultaneous observations of H2O and SiO (J = 1-0, v = 1) masers for 171 known late-type maser stars with the 34 m radio telescope at Kashima. We found a systematic change in the H2O maser spectra related to the evolution of the stars. Typically, H2O maser spectral profiles are singly peaked in Mira variables, but doubly peaked in IRC/AFGL objects and OH/IR stars. The expansion velocity of H2O masers increases with decreasing IRAS color temperature. This is explained by the shock excitation model proposed by Cooke and Elitzur (1985). The blue shifted peak in the profiles is more prominent than the red shifted peak in most of the IRC/AFGL objects and OH/IR stars. A blocking model of the redshifted peak is introduced.

Affiliated with

Also associated with

No associations

Rating

Spectral evolution of the H2O maser in late-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 Spectral evolution of the H2O maser in late-type stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Spectral evolution of the H2O maser in late-type stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1414273