A hot, low mass-loss rate inner envelope in IRC + 10216

Details A hot, low mass-loss rate inner envelope in IRC + 10216 A hot, low mass-loss rate inner envelope in IRC + 10216

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...318..809s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 15, 1987, p. 809-822.

Astronomy and Astrophysics

Astrophysics

46

Hot Stars, Infrared Stars, Mass Flow Rate, Stellar Envelopes, Stellar Mass Ejection, Stellar Models, Carbon Monoxide, Line Spectra, Optical Thickness

Scientific paper

Detailed models of CO excitation in the circumstellar envelope of the late-type, carbon-rich Mira IRC + 10216 have been made in order to infer its physical properties. The best-fit model matches the intensities and shapes of all observed rotational CO lines from the object, including the J = 1-0, 2-1, 3-2, and 6-5 lines. From this model, it is determined that the gas kinetic temperature in the inner envelope is significantly larger than that predicted from a thermodynamic model which describes the extended outer envelope. The mass-loss rate in the inner envelope is significantly lower than in the outer envelope. A value of 3.2 x 10 to the -5th solar mass/yr is inferred compared to a value of 4.8 x 10 to the -5th for the extended envelope. These results indicate that the inner envelope represents a phase of reduced mass loss in the object.

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