Accretion disk models for FU Orionis and V1057 Cygni - Detailed comparisons between observations and theory

Details Accretion disk models for FU Orionis and V1057 Cygni - Detailed comparisons between observations and theory Accretion disk models for FU Orionis and V1057 Cygni - Detailed comparisons between observations and theory

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...325..231k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 325, Feb. 1, 1988, p. 231-251. Research supported by the Smithsonian Instit

Astronomy and Astrophysics

Astrophysics

133

Accretion Disks, Pre-Main Sequence Stars, Stellar Mass Accretion, Stellar Models, Stellar Spectrophotometry, Infrared Spectra, Light Curve, Spectral Energy Distribution, Stellar Evolution

Scientific paper

We present further tests of the accretion disk hypothesis for FU Orionis objects. Steady disk models that fit the broad-band energy distributions of V1057 Cyg and FU Ori require accretion rates of M ˜ 10 -4 Msun yr-1, which implies that ˜ 10-3 to 10-2 Msun is added to the central object during an FU Orionis eruption. These models make reasonably quantitative predictions regarding the shape of absorption-line profiles and variation of rotation with wavelength using a small number of free parameters. Our analysis of intermediate and high- resolution observations shows good agreement with theoretical disk spectra. We estimate that the central stars have masses and radii (M* ˜ 0.3-1 Msun;R* ˜ 4 Rsun) appropriate for normal pre-main-sequence stars if the inclination of the disk's rotation axis to the line of sight is i < 30° for V1057 Cyg and 25° < i < 70° for FU Ori. The monotonic fading of brightness of V1057 Cyg in the optical and near-infrared provides strong support for the accretion model. The lack of decline at 4.8 µm cannot be accounted for by steady disks, but may be a consequence of time-dependent phenomena in the evolving disk. Material in the outer disk appears to reprocess radiation emitted by the inner disk, and is responsible for the substantial far-infrared decay at 10-20 µm.

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