A nonspherical thermal instability in young stars

Details A nonspherical thermal instability in young stars A nonspherical thermal instability in young stars

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979natur.278..625v&link_type=abstract

Nature, vol. 278, Apr. 12, 1979, p. 625, 626.

Physics

1

Stellar Evolution, Thermal Instability, Convective Heat Transfer, Heavy Elements, Inhomogeneity, Nuclear Reactions

Scientific paper

It is shown that in inhomogeneous young stars more massive than or as massive as the sun, a large scale nonspherical thermal instability can be excited at the stage when carbon has started to capture protons, but before convection has begun. The nonhomogeneous structure is considered to have formed from a dusty protocloud. For thermal instability to occur, the rate of nuclear energy generation must by highly sensitive to temperature. The onset of thermal instability leads to a large change in the mass fraction of heavy elements, and a negligible change in pressure and density distributions. The time of growth of the instability is found to be very short, usually on the order of 0.1 year, and large scale nonspherical spatial variations in temperature, which may survive the stage of hydrogen burning, are produced. The nonspherical thermal instability model may account for outbursts of FU Ori type stars.

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