Early pre-main-sequence evolution with deuterium burning

Details Early pre-main-sequence evolution with deuterium burning Early pre-main-sequence evolution with deuterium burning

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...235..955m&link_type=abstract

Astrophysical Journal, Part 1, vol. 235, Feb. 1, 1980, p. 955-959.

Astronomy and Astrophysics

Astrophysics

41

Deuterium, Early Stars, Main Sequence Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Structure, Combustion, Hertzsprung-Russell Diagram, Numerical Integration, Stellar Luminosity, Stellar Temperature, T Tauri Stars

Scientific paper

Theoretical evolutionary histories of pre-main-sequence Population I stars of mass between 0.2 and 5 solar masses have been computed using the hypothesis of quasi-static equilibrium contraction. Since deuterium is present in the interstellar clouds in which stars are born, the D(P, gamma)3He reaction has also been included in the models. The results show that the evolutionary lifetimes in the region of T Tau stars are nearly doubled for an initial D-abundance equal to 2.5 x 10 to the -5th power. Some possible correlations among mass accretion, D-burning, and T Tau outbursts are also briefly discussed.

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