Detection of the H92-alpha radio recombination line from the symbiotic star H1-36 Arae

Details Detection of the H92-alpha radio recombination line from the symbiotic star H1-36 Arae Detection of the H92-alpha radio recombination line from the symbiotic star H1-36 Arae

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387l..77b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 387, March 10, 1992, p. L77-L80.

Astronomy and Astrophysics

Astronomy

4

H Alpha Line, Planetary Nebulae, Radio Astronomy, Recombination Reactions, Symbiotic Stars, Very Large Array (Vla), Bremsstrahlung, H Ii Regions, Milky Way Galaxy, Optical Thickness, Photoionization, Stellar Winds

Scientific paper

The H92-alpha radio recombination line at 8309.383 MHz has been detected from the symbiotic star H1-36 Arae by the VLA. The continuum flux density is 73.5 mJy and the observed line-to-continuum ratio is Tl/Tc greater than about 1 percent. The line width is 46 km/s. Since the photoionized nebula may account for as little as one-half of the continuum radio flux, the true line-to-continuum ratio may be as high as 2 percent. If this is the case, and if pressure broadening is negligible, the electron temperature is between 10 exp 4 and 2 x 10 exp 4 K. If pressure broadening is marginally significant, the expansion velocity of the wind is consistent with vexp = 10 km/s, and the electron temperature drops to a range comparable to that found for certain planetary nebulae.

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