Mass loss from evolved stars. VII - OH maser shell radii and mass-loss rates for OH/IR stars

Details Mass loss from evolved stars. VII - OH maser shell radii and mass-loss rates for OH/IR stars Mass loss from evolved stars. VII - OH maser shell radii and mass-loss rates for OH/IR stars

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...323..734n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 323, Dec. 15, 1987, p. 734-748.

Astronomy and Astrophysics

Astrophysics

96

Interstellar Masers, Photodissociation, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Cool Stars, Hydroxyl Emission, Late Stars, Stellar Models, Stellar Winds

Scientific paper

The equations of photodissociation and radiative transfer are solved for the photochemical chain H2O yields OH + H yields O + H + H in the circumstellar envelopes produced by steady mass loss from cool evolved stars. The solution is performed for a large range of mass-loss rates, outflow velocities, and interstellar UV radiation field densities. Comparison with observations shows that, over a wide range of mass-loss rates, the radius at which the OH density peaks coincides with the radius defined by maser emission in the 1612 MHz line. This allows the use of these models, together with observations of OH maser shell radii and wind outflow velocities, to measure mass-loss rates. A simple power-law function relating mass-loss rate to OH shell radius and wind outflow velocity is developed from these models and is applied to the existing measurements of OH shell radii to derive mass-loss rates for 42 stars.

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