Optical spectroscopy of Z Canis Majoris, V1057 Cygni, and FU Orionis - Accretion disks and signatures of disk winds

Details Optical spectroscopy of Z Canis Majoris, V1057 Cygni, and FU Orionis - Accretion disks and signatures of disk winds Optical spectroscopy of Z Canis Majoris, V1057 Cygni, and FU Orionis - Accretion disks and signatures of disk winds

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...397..260w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 397, no. 1, p. 260-276.

Astronomy and Astrophysics

Astrophysics

42

Accretion Disks, Stellar Spectrophotometry, Stellar Winds, Supergiant Stars, Data Reduction, H Alpha Line, High Resolution, Signal To Noise Ratios, Stellar Models

Scientific paper

High resolution, high SNR optical spectra have been used to investigate the hypothesis that in outburst, FU Ori objects are self-luminous accretion disks whose light dominates at optical and near-IR wavelengths. Strong evidence has been found for linewidth versus wavelength correlation in good agreement with model predictions for Z CMa and V1057 Cyg, but not for FU Ori itself. Linewidth varies continuously with wavelength at optical wavelengths in the former two objects, In the case of FU Ori, it is argued that a combination of strong wind components to spectral lines, and surface gravity possibly being lower than that of supergiants, conceals the underlying linewidth versus wavelength relationship. A marginal correlation is found between linewidth and lower excitation potential in all three objects. Synthetic disk spectra are subtracted from observed spectral, and remarkably good fits are found for all three objects for wavelengths longer than about 5000 A.

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