Other
Scientific paper
Jan 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...312..243h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 312, Jan. 1, 1987, p. 243-253.
Other
112
Accretion Disks, Orion Constellation, Pre-Main Sequence Stars, Stellar Mass Accretion, Stellar Models, Extinction, Infrared Spectra, Molecular Spectra, Stellar Rotation, Stellar Spectra
Scientific paper
The authors report new observations supporting their hypothesis that rapid disk accretion onto pre-main-sequence stars causes the outbursts of FU Orionis objects. High-resolution infrared spectra show that FU Ori rotates rapidly in the 2 μm spectral region, but more slowly than at 6170 Å. This differential rotation is predicted by the accretion disk model for FU Ori outbursts. Optical observations of V1057 Cyg provide additional evidence for double-peaked profiles, another disk model prediction. In the absence of evidence for radial-velocity variability ⪆3 km s-1 in either the optical or infrared regions, it is concluded that the accretion disk is not fed by a companion star, but rather consists of remnant material from the star formation process. Fairly crude statistical arguments suggest that low-mass stars accrete >1% (perhaps as much as 10%) of their mass in FU Ori events.
Hartmann Lee
Kenyon Scott. J.
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