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• W2024148061 startingPage "32" @default.
• W2024148061 abstract "A star acquires much of its mass by accreting material from a disk. Accretion is probably not continuous but episodic. We have developed a method to include the effects of episodic accretion in simulations of star formation. Episodic accretion results in bursts of radiative feedback, during which a protostar is very luminous, and its surrounding disk is heated and stabilized. These bursts typically last only a few hundred years. In contrast, the lulls between bursts may last a few thousand years; during these lulls the luminosity of the protostar is very low, and its disk cools and fragments. Thus, episodic accretion enables the formation of low-mass stars, brown dwarfs, and planetary-mass objects by disk fragmentation. If episodic accretion is a common phenomenon among young protostars, then the frequency and duration of accretion bursts may be critical in determining the low-mass end of the stellar initial mass function." @default.
• W2024148061 created "2016-06-24" @default.
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• W2024148061 date "2011-03-01" @default.
• W2024148061 modified "2023-10-16" @default.
• W2024148061 title "THE IMPORTANCE OF EPISODIC ACCRETION FOR LOW-MASS STAR FORMATION" @default.
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• W2024148061 doi "https://doi.org/10.1088/0004-637x/730/1/32" @default.
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