Accretion disc flows around FU Orionis stars

Details Accretion disc flows around FU Orionis stars Accretion disc flows around FU Orionis stars

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.236..495c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 236, Jan. 15, 1989, p. 495-503. Research sponsored by N

Astronomy and Astrophysics

Astronomy

32

Accretion Disks, Early Stars, Pre-Main Sequence Stars, Stellar Mass Accretion, Stellar Spectrophotometry, Heat Transfer, Ionization, Protostars, Thermal Stability, Time Dependence

Scientific paper

The accretion disk model of FU Orionis systems in outburst is investigated by examining the time-dependent behavior of a disk around a low-mass protostar that accretes at 0.00001-0.0001 solar masses/yr. It is found that the disk may be stabilized against the thermal ionization instability by the effect of advective heat transport and that it may therefore exist in the quasi-steady-state observed in post-outburst FU Orionis systems. The disk models are used to discuss the cosmochemical consequences of possible FU Ori events during the evolution of the primordial solar nebula.

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