Further evidence for disk accretion in FU Orionis objects
Abstract
view Abstract Citations (127) References (16) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Further Evidence for Disk Accretion in FU Orionis Objects Hartmann, L. ; Kenyon, S. J. Abstract 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. Publication: The Astrophysical Journal Pub Date: January 1987 DOI: 10.1086/164866 Bibcode: 1987ApJ...312..243H Keywords: Accretion Disks; Orion Constellation; Pre-Main Sequence Stars; Stellar Mass Accretion; Stellar Models; Extinction; Infrared Spectra; Molecular Spectra; Stellar Rotation; Stellar Spectra; Astrophysics; STARS: ACCRETION; STARS: INDIVIDUAL CONSTELLATION NAME: FU ORIONIS; STARS: INDIVIDUAL CONSTELLATION NAME: V1057 CYGNI; STARS: INDIVIDUAL CONSTELLATION NAME: V1515 CYGNI; STARS: PRE--MAIN-SEQUENCE full text sources ADS | data products SIMBAD (4)