2015ApJ...807...84L -
Astrophys. J., 807, 84 (2015/July-1)
High resolution optical and NIR spectra of HBC 722.
LEE J.-E., PARK S., GREEN J.D., COCHRAN W.D., KANG W., LEE S.-G. and SUNG H.-I.
Abstract (from CDS):
We present the results of high resolution (R ≥ 30,000) optical and near-IR spectroscopic monitoring observations of HBC 722, a recent FU Orionis object that underwent an accretion burst in 2010. We observed HBC 722 in the optical/near-IR with the Bohyunsan Optical Echelle Spectrograph, Hobby-Eberly Telescope-HRS, and Immersion Grating Infrared Spectrograph, at various points in the outburst. We found atomic lines with strongly blueshifted absorption features or P Cygni profiles, both evidence of a wind driven by the accretion. Some lines show a broad double-peaked absorption feature, evidence of disk rotation. However, the wind-driven and disk-driven spectroscopic features are anti-correlated in time; the disk features became strong as the wind features disappeared. This anti-correlation might indicate that the rebuilding of the inner disk was interrupted by the wind pressure during the first 2 years. The half-width at half-depth of the double-peaked profiles decreases with wavelength, indicative of the Keplerian rotation; the optical spectra with the disk feature are fitted by a G5 template stellar spectrum convolved with a rotation velocity of 70 km/s while the near-IR disk features are fitted by a K5 template stellar spectrum convolved with a rotation velocity of 50 km/s. Therefore, the optical and near-IR spectra seem to trace the disk at 39 and 76 R☉, respectively. We fit a power-law temperature distribution in the disk, finding an index of 0.8, comparable to optically thick accretion disk models.
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Journal keyword(s):
stars: formation - stars: protostars
Simbad objects:
7
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