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| {{Multiple issues|refimprove=August 2010|one source=August 2010|citation style=August 2010}}
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| [[File:PMS evolution tracks.svg|thumb|Stellar evolution tracks (blue lines) for the pre-main-sequence. The nearly-horizontal curves are called Henyey tracks.<br />
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| High-mass stars have nearly horizontal evolution tracks from their birth until they arrive on the main sequence. Lighter stars, first follow the nearly-vertical [[Hayashi track]] before bending left into the Henyey track. <br />
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| The end (leftmost point) of every track is labeled with the star's mass in solar masses, and represents its position on the main sequence.
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| The red curves labeled in years are isochrones at the given ages. In other words, stars <math>10^5</math> years old lie along the curve labeled <math>10^5</math>, and similarly for the other 3 isochrones.]]
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| The '''Henyey track ''' is a path taken by [[pre-main-sequence star]]s with masses >0.5 [[Sun|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 pre-main-sequence star can remain in radiative equilibrium throughout some period of its contraction to the main sequence.
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| The Henyey track is characterized by a slow collapse in near hydrostatic equilibrium. They are approaching the [[main sequence]] almost horizontally in the Hertzsprung–Russell diagram (i.e. the [[luminosity]] remains almost constant).
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| ==References==
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| *{{Cite journal |last=Henyey |first=L. G. |last2=Lelevier |first2=R. |last3=Levée |first3=R. D. |year=1955 |title=The Early Phases of Stellar Evolution |journal=Publications of the Astronomical Society of the Pacific |volume=67 |issue=396 |pages=154–160 |doi= 10.1086/126791|bibcode = 1955PASP...67..154H }}
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| {{Star}}
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| [[Category:Stellar evolution]]
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| [[Category:Hertzsprung–Russell classifications]]
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| {{astronomy-stub}}
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Latest revision as of 01:54, 7 January 2015
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