Hayashi limit is a constraint upon the maximum radius of a star for a given mass. When a star is fully within hydrostatic equilibrium—a condition where the inward force of gravity is matched by the outward pressure of the plasma—then the star can not exceed the radius defined by the Hayashi limit. This has important implications for the evolution of a star, both during the formulative contraction period and later when the star has consumed most of its hydrogen supply through nuclear fusion.[1]
A Hertzsprung-Russell diagram displays a plot of a star's surface temperature against the luminosity. On this diagram, the Hayashi limit forms a nearly vertical line at about 3,500 K. Low temperature stars are always fully convective, and models of stellar structure for fully-convective stars do not provide a solution to the right of this line where a star is in equilibrium (with lower surface temperatures). Thus stars are constrained to remain to the left of this limit during all periods when they are in hydrostatic equilibrium, and the region to the right of the line forms a type of "forbidden zone". Note, however, that there are exceptions to the Hayashi limit. These include collapsing protostars, as well as stars with magnetic fields that interfere with the internal transport of energy through convection.[2]
Red giants are stars that have expanded their outer envelope in order to support the nuclear fusion of helium. This moves them up and to the right on the H-R diagram. However, they are constrained by the Hayashi limit not to expand beyond a certain radius.[3]
The Hayashi limit is named after
See also
References
- ^ Martin Schwarzschild (May 27-29, 1975). "The Study of Stellar Structure". Theoretical Principles in Astrophysics and Relativity. University of Chicago: University of Chicago Press. pp. 1-14.
- ^ Clowes, Chris (July 3, 2005). "Hertzsprung-Russell Diagram". Peripatus. http://www.peripatus.gen.nz/Astronomy/HerRusDia.html. Retrieved 2007-05-04.
- ^ Hayashi, Chushiro; Hoshi, Reun (1961). "Outer Envelope of Giant Stars with Surface Convection Zone". Publications of the Astronomical Society of Japan 13: 442–449. http://adsabs.harvard.edu/abs/1961PASJ...13..442H. Retrieved 2007-05-03.
- ^ Tenn, Joe (June 8, 2004). "Chushiro Hayashi". Sonoma State University. http://www.phys-astro.sonoma.edu/BruceMedalists/Hayashi/. Retrieved 2007-05-03.
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