On the formation of stars from disk accretion

Details On the formation of stars from disk accretion On the formation of stars from disk accretion

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..363m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 1, 1984, p. 363-366.

Astronomy and Astrophysics

Astrophysics

52

Accretion Disks, Hertzsprung-Russell Diagram, Pre-Main Sequence Stars, Stellar Evolution, Stellar Mass Accretion, T Tauri Stars, Deuterium, Gravitational Collapse, Open Clusters, Stellar Cores

Scientific paper

Models of stars which form by accretion from a disk have been constructed. Accretion and pre-main-sequence tracks have been calculated for a range of initial parameters which spans the physically reasonable modes for accretion. It is found that the models agree with the observed positions of T Tauri stars in the H-R diagram and avoid some of the problems which are endemic to traditional pre-main-sequence evolution. No evidence is found to indicate that the formation of high- and low-mass stars in young open clusters is noncoeval. A problem is pointed out that arises when attempting to use an H-R diagram of T Tauri stars to distinguish between various models of star formation.

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