The dusty envelopes of FU Orionis variables

Details The dusty envelopes of FU Orionis variables The dusty envelopes of FU Orionis variables

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...383..664k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 383, Dec. 20, 1991, p. 664-673.

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79

Accretion Disks, Cosmic Dust, Pre-Main Sequence Stars, Spectral Energy Distribution, Stellar Envelopes, Variable Stars, Computational Astrophysics, Infrared Astronomy Satellite, Infrared Photometry, Stellar Evolution, Stellar Mass Accretion, Stellar Models

Scientific paper

The spectral energy distributions of five FU Orionis variables are discussed using new ground-based infrared photometry and IRAS Addscan measurements. V1057 Cyg, V1515 Cyg, and Z CMa have much larger far-infrared fluxes than can be explained by the simple accretion disk models that match their spectral energy distributions less than 10 microns. The 10-20-micron excess emission in V1057 has decreased proportionately with the decline in optical light, which demonstrates that the far-infrared flux arises in a dust shell reprocessing light from the central object. It is suggested that the far-infrared excesses arise in somewhat flattened dusty envelopes with a covering factor in a solid angle of roughly one-half, which is consistent with the fraction of FU Orionis variables that are heavily embedded. It is proposed that the dusty envelope falls onto the outer disk at a rate of about 5 x 10 exp -6 solar mass/yr. The rate is sufficient to replenish disk material accreted during a FU Orionis outburst and allow repetitive eruptions on time scales of several thousand years.

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