The structure and saturation of OH maser lines from long-period variable stars

Details The structure and saturation of OH maser lines from long-period variable stars The structure and saturation of OH maser lines from long-period variable stars

Jul 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...223l..25f&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 223, July 1, 1978, p. L25-L27. NSF-supported research.

Astronomy and Astrophysics

Astronomy

13

Hydroxyl Emission, Interstellar Masers, Masers, Radio Sources (Astronomy), Radio Spectra, Variable Stars, Radio Emission, Spectrum Analysis

Scientific paper

Detailed spectra of the 18 cm OH maser lines from about 20 long-period variable stars have been measured at the Arecibo Observatory. Examination of the main-line emission spectra from these stars reveals that most, if not all, of the sources have emission throughout the velocity interval between the two principal velocity groups. The relatively small values of maximum to minimum flux within the lines argue that the lines are produced in saturated or partially saturated masers. The striking similarity of the 1665 MHz and 1667 MHz line profiles for S CrB is a further indication that the main lines from that star are not produced by unsaturated masers.

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