Advanced stages in the evolution of the sun

Details Advanced stages in the evolution of the sun Advanced stages in the evolution of the sun

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...246..118j&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 246, no. 1, June 1991, p. 118-136. Research supported by Carlsberg Foundation.

Astronomy and Astrophysics

Astrophysics

22

Red Giant Stars, Stellar Evolution, Stellar Luminosity, Stellar Mass Ejection, Stellar Models, Stellar Temperature, Helium, Planetary Nebulae

Scientific paper

The method of analytical fits to numerical results of stellar evolutionary tracks is used to estimate the effects of using different codes and input physics, as well as to gauge the effects of uncertainties in the knowledge of the sun's chemical composition, mixing-length parameter, and mass-loss parameter. The sun is found to be in a region of parameter space where solar models with only slightly different input will lead to widely different evolutionary ends, spanning from the end of nuclear burning before the helium core flash can occur, to evolution until enough nucleosynthesized material has been dredged up to turn the sun into a carbon star with C/O approximating 1.6. The most likely final stage is an oxygen-rich red giant Mira variable with a period of around 250 days and a luminosity and temperature of around 5000 solar luminosities and 3000 K, respectively, at an age of 11.6 x 10 to the 9th yr. Between 35 and 55 percent of the mass will be lost via wind during the solar lifetime, primarily shortly before the helium core flash and at the asymptotic giant branch.

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