Positions of the radio recombination line masers in MWC 349

Details Positions of the radio recombination line masers in MWC 349 Positions of the radio recombination line masers in MWC 349

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...386l..23p&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 386, Feb. 10, 1992, p. L23-L26. Research supported by CICYT.

Astronomy and Astrophysics

Astrophysics

52

Interstellar Masers, Line Spectra, Radiative Recombination, Radio Stars, Ionized Gases, Optical Thickness, Red Shift, Stellar Winds

Scientific paper

The Owens Valley Millimeter Interferometer has been used at 232 GHz to measure the relative positions of the strongest H30-alpha maser features toward MWC 349. Maser emission appears to originate from two positions 0.065 +/- 0.005 arcsec (80 AU) apart, located in an almost east-west direction (P.A. 107 +/- 7 deg), approximately perpendicular to the bipolar ionized wind structure observed in low-frequency radio continuum maps. It is argued that the maser features originate in two positions associated with a nearly edge-on, neutral disk which is the source of high-density ionized gas. The maser spots probably arise from clumps located in the near part of the disk surface.

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