Henyey track
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The Henyey track is a path taken by protostars with masses >0.5 Solar mass in the Hertzsprung-Russell diagram after the end of Hayashi track. The astronomer Louis G. Henyey and his colleagues in the 1950s, showed that the proto-star can remain in radiative equilibrium throughout some period of its contraction to the main sequence. The Henyey track is characterized by a slow collapse in near hydrostatic equilibrium. They are approaching the main sequence almost horizontally in the HR diagram (i.e. the luminosity remains almost constant).
[edit] References
- Henyey, L. G., Lelevier, R., Levée, R. D. (1955), The Early Phases of Stellar Evolution, Publications of the Astronomical Society of the Pacific, Vol. 67, No. 396, p.154-160
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