Accretion disc flows around FU Orionis stars⋆

We investigate the accretion disc model of FU Orionis systems in outburst by examining the time-dependent behaviour of a disc around a low-mass protostar that accretes at 10−5 to 10−4M⊙ yr−1. We find that the disc 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. We use our disc models to discuss the cosmochemical consequences of possible FU Ori events during the evolution of the primordial solar nebula.

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