THE NEAR INFRARED AND OPTICAL PHOTOMETRIC ACTIVITY OF V517 Cyg
- Authors: Efimova N.V.1, Grinin V.P.1,2, Arkharov A.A.1, Potravnov I.S.3, Melnikov S.Y.4, Larionov V.M.1,2, Klimanov S.A.1, Gorshanov D.L.1
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Affiliations:
- Pulkovo Observatory of the Russian Academy of Sciences
- Saint Petersburg University
- Institute of Astronomy of the Russian Academy of Sciences
- National University of Uzbekistan
- Issue: Vol 100, No 11 (2023)
- Pages: 1005-1022
- Section: Articles
- URL: https://journals.rcsi.science/0004-6299/article/view/148086
- DOI: https://doi.org/10.31857/S000462992311004X
- EDN: https://elibrary.ru/HBOFXB
- ID: 148086
Cite item
Abstract
A near infrared and optical photometric study of Herbig star V517 Cyg has been carried out. Infrared data were obtained in 2003–2017 at the Campo Imperatory Observatory (Italy) with the Pulkovo telescope AZT-24 in Johnson’s \(JHK\) bands. Optical light curves in Johnson \(UBVR\) bands were obtained at the Maidanak observatory. Additional optical photometry from different sources (ASSAS, WISE, and AAVSO) was also used. It was shown that the behavior of V517 Cyg in the near infrared is typical for UX Ori stars. A considerable contribution to the near infrared variability is due to variable extinction along the line of sight, but the disk radiation becomes strong in the \(H\) and \(K\) bands: there is a significant correlation of \(V\) and \(J\) magnitudes (\(r \sim 0.84\)), while \(H\) and \(K\) bands correlates poorly with \(V\) band. The amplitude of variability in \(J\) is quite large (\( \sim {\kern 1pt} {{1.8}^{m}}\)). The deepest minimum (\(\Delta V \sim {{3.6}^{m}}\)) in the \(V\) band demonstrates quasi-periodic variations with an amplitude of \( \sim {\kern 1pt} {{0.8}^{m}}\) and a period of \( \sim {\kern 1pt} 19\) days, the origin of which is still unclear. It is possible that these quasi-periodic variations are related to rotation period of a second companion, a cold T Tauri star. The spectrum V517 Cyg reveals typical for UX Ori stars the double-peaked emission line Hα. The NaI D doublet has inverse P Cyg profiles, indicating intense accretion of gas onto the star. The accretion rate from an equivalent width of the Hα line is \({{\dot {M}}_{{acc}}} = 3.6 \times {{10}^{{ - 8}}}\,{{M}_{ \odot }}\) per year.
About the authors
N. V. Efimova
Pulkovo Observatory of the Russian Academy of Sciences
Email: vgcrao@mail.ru
Russia, Saint Petersburg
V. P. Grinin
Pulkovo Observatory of the Russian Academy of Sciences; Saint Petersburg University
Author for correspondence.
Email: vgcrao@mail.ru
Russia, Saint Petersburg; Russia, Saint Petersburg
A. A. Arkharov
Pulkovo Observatory of the Russian Academy of Sciences
Email: vgcrao@mail.ru
Russia, Saint Petersburg
I. S. Potravnov
Institute of Astronomy of the Russian Academy of Sciences
Email: vgcrao@mail.ru
Russia, Moscow
S. Yu. Melnikov
National University of Uzbekistan
Email: vgcrao@mail.ru
Uzbekistan, Tashkent
V. M. Larionov
Pulkovo Observatory of the Russian Academy of Sciences; Saint Petersburg University
Email: vgcrao@mail.ru
Russia, Saint Petersburg; Russia, Saint Petersburg
S. A. Klimanov
Pulkovo Observatory of the Russian Academy of Sciences
Email: vgcrao@mail.ru
Russia, Saint Petersburg
D. L. Gorshanov
Pulkovo Observatory of the Russian Academy of Sciences
Email: vgcrao@mail.ru
Russia, Saint Petersburg
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