Accretion Disks and Eruptive Phenomena
Abstract
Description
This paper describes eruptive phenomena in pre-main sequence stars. The eruptions of FU Orionis stars have much in common with outbursts in other accreting systems, such as dwarf novae and some symbiotic stars. These common features are best understood as increases in the rate material flows through an accretion disk. The spectroscopic properties, decay of the light curves, and outflow phenomena suggest that these outbursts arise from thermal instabilities in the disk. Available data and estimates for recurrence times indicate that young stars can accrete much, perhaps all, of their mass in FU Ori accretion events. Future observations can test this notion and place better constraints on the importance of eruptive events in the early life of a low mass star.
to appear in The Physics of Star Formation and Early Stellar Evolution, edited by C. J. Lada and N. Kylafis (30 pages, 11 figures) This version corrects several typos and a mistaken impression left in the derivation of the disk radial temperature profile
to appear in The Physics of Star Formation and Early Stellar Evolution, edited by C. J. Lada and N. Kylafis (30 pages, 11 figures) This version corrects several typos and a mistaken impression left in the derivation of the disk radial temperature profile