Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...215..781k&link_type=abstract
Astrophysical Journal, Part 1, vol. 215, Aug. 1, 1977, p. 781-787.
Astronomy and Astrophysics
Astrophysics
119
Carbon Stars, Infrared Stars, Late Stars, Molecular Spectra, Stellar Envelopes, Stellar Mass Ejection, Abundance, Carbon Monoxide, Gas Temperature, Hydrocyanic Acid, Molecular Excitation, Momentum Transfer, Stellar Models, Temperature Distribution
Scientific paper
The circumstellar envelope of IRC +10216 is modeled by assuming steady spherically symmetric mass loss from the star. The mass outflow is presumed to be due to radiation pressure on grains formed in the stellar atmosphere and momentum-coupled to the gas, and the temperature of the expanding gas is determined by taking account of cooling due to free expansion and molecular emission as well as heating resulting from gas-dust collisions. The excitation of molecular emission from CO, (C-13)O, HCN, and H(C-13)N is computed and compared with observations in order to obtain information about the mass-loss rate and the molecular abundances. For a distance of 200 pc, a mass-loss rate of 0.00002 solar mass per yr is derived along with a CO/H2 abundance ratio of 0.0008, a CO/(C-13)O isotope ratio of 35, and a momentum-transfer efficiency factor (averaged over the continuum energy distribution) of 0.013. Uncertainties in these results and their dependence on the assumed distance are discussed.
Hill F. F.
Kwan Juliana
No associations
LandOfFree
The circumstellar envelope of IRC +10216 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The circumstellar envelope of IRC +10216, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The circumstellar envelope of IRC +10216 will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1880185