Kinematic structure of OH/IR stars

Details Kinematic structure of OH/IR stars Kinematic structure of OH/IR stars

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...185..258s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 185, no. 1-2, Oct. 1987, p. 258-266. NSERC-supported research.

Astronomy and Astrophysics

Astrophysics

26

Infrared Stars, Late Stars, Masers, Planetary Nebulae, Stellar Mass Ejection, Stellar Structure, Asymptotic Giant Branch Stars, Cosmic Dust, Gravitational Collapse, Red Shift, Shock Waves, Stellar Mass Accretion, Very Large Array (Vla), Very Long Base Interferometry

Scientific paper

A kinematic model is constructed for 1612 MHz OH maser emssion in OH/IR stars. The spatial distributions of OH maser intensity are calculated from a model of spherically-symmetric uniformly-expanding circumstellar shell. By comparing VLA/VLBI maps of OH/IR stars with model results, the acceptable range of combination of physical parameters M/Ve, (nH2)max, (nH2)min, fOH = [nOH]/[nH2] are derived. The theoretical relations between OH shell radius R0 and mass loss rate Mand between OH maser luminosity LOH and Mare also obtained. These relations are in good agreement with empirical relations established by Bowers et al. (1983) and Baud et al. (1983). The ranges of (nH2)max and (nOH)min under different Mrequired for operating saturated 1612 MHz OH masers are also discussed. The authors find that the OH emission phase can last over 1000 years after the termination of the asymptotic giant branch and many protoplanetary nebulae may have the characteristics of OH/IR stars.

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