Detection of H I emission in the circumstellar envelope of Omicron Ceti (Mira)

Details Detection of H I emission in the circumstellar envelope of Omicron Ceti (Mira) Detection of H I emission in the circumstellar envelope of Omicron Ceti (Mira)

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...332..299b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 332, Sept. 1, 1988, p. 299-304. Navy-supported research.

Astronomy and Astrophysics

Astrophysics

46

Giant Stars, H I Regions, Stellar Envelopes, Carbon Monoxide, Density Distribution, Hydrogen Atoms, Line Spectra, Stellar Mass, Stellar Winds, Velocity Distribution, Very Large Array (Vla)

Scientific paper

High-sensitivity 21 cm VLA observations of Mira (Omicron Cet), have resulted in the detection of H I in its circumstellar envelope. The central velocity is +46.4 + or - 0.3 km/s, and the expansion velocity is 4.6 + or - 0.3 km/s, in excellent agreement with values from CO observations. At a distance of 77 pc, the envelope radius is 160 arcsec or 1.8 x 10 to the 17th cm, the age (crossing time) is 1300 yr, and the total H I mass 0.0006 solar mass. The envelope appears to be roughly spherically symmetric, and the density gradient is shallower than 1/r2, the most plausible explanation appears to be photoproduction of H I from H2 by interstellar ultraviolet radiation. The observations then suggest that the total hydrogen loss rate from Omicron Cet is about 10 to the 7th solar mass/yr and that the wind is appproximately one-third atomic as it leaves the star. Consideration of the interaction between the wind and the interstellar medium suggests that the local interstellar density is about 0.03/ cu cm.

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