The Spectroscopic Variations of the FU Orionis Object V960 Mon
arXiv:1801.00883 · doi:10.3847/1538-3881/aaa545
Abstract
We present the results of the spectroscopic monitoring of the FU Orionis type star V960 Mon. Spectroscopic variations of a FU Orionis type star will provide valuable information of its physical nature and the mechanism of the outburst. We conducted medium-resolution (R~10000) spectroscopic observations of V960 Mon with 2m Nayuta telescope at the Nishi-Harima Astronomical Observatory, from 2015 January to 2017 January for 53 nights in total. We focused on H alpha line and nearby atomic lines, and detected the strength variations in both absorption and emission lines. The observed variation in the equivalent width of the absorption lines correspond to a decrease in effective temperature and increase in surface gravity. These variations were likely to originate from the luminosity fading of the accretion disk due to the decrease in mass accretion rate.
10 pages, 5 figures, accepted for publication in AJ
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- Measuring Optical Extinction Towards Young Stellar Objects Using Diffuse Interstellar Bands
- A Study of Millimeter Variability in FUor Objects
- Spectroscopy of 9 eruptive young variables using TANSPEC
- Revealing the spectroscopic variations of FU Orionis object V960 Mon with high-resolution spectroscopy
- Molecular inventory of a young eruptive star's environment -- Case study of the classical FU Orionis star V1057 Cyg
- A study of the photometric and spectroscopic variations of the prototypical FU Orionis-type star V1057 Cyg