The structure of H2O masers associated with late-type stars

Details The structure of H2O masers associated with late-type stars The structure of H2O masers associated with late-type stars

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230..449s&link_type=abstract

Astrophysical Journal, Part 1, vol. 230, June 1, 1979, p. 449-455.

Astronomy and Astrophysics

Astrophysics

45

Infrared Stars, Late Stars, Radiant Flux Density, Stimulated Emission, Variable Stars, Water Masers, Emission Spectra, Maser Outputs, Stellar Magnitude, Thermal Emission

Scientific paper

The H2O maser emission features for each of the stars, RT Vir, W Hya, RX Boo, and RR Aql, have been found to lie in a region of no more than about 10 to the 14th cm. The masers are probably located in a shell surrounding the star. There have been order-of-magnitude variations in the flux densities of these H2O masers since 1973, and variations in the infrared flux of these stars should have been expected if the masers are pumped by IR photons. Weak, broad, quasi-thermal features are found to underlie the narrow features in W Hya, RX Boo, and R Aql.

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