Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-30T01:45:48.839Z Has data issue: false hasContentIssue false
  • English
  • Français

Optical and X-ray study of V404 Cyg during its activity in the Summer 2015

Published online by Cambridge University Press:  30 December 2019

Evgeniya A. Nikolaeva ,
Ilfan F. Bikmaev ,
Maxim V. Glushkov ,
Eldar N. Irtuganov  and
Irek M. Khamitov
Evgeniya A. Nikolaeva
Affiliation:
Kazan Federal University, 420008, Kremlyovskaya St. 18, Kazan, Russian Federation email: [email protected] Academy of Sciences of Tatarstan, 420111, Bauman St. 20, Kazan, Russian Federation
Ilfan F. Bikmaev
Affiliation:
Kazan Federal University, 420008, Kremlyovskaya St. 18, Kazan, Russian Federation email: [email protected] Academy of Sciences of Tatarstan, 420111, Bauman St. 20, Kazan, Russian Federation
Maxim V. Glushkov
Affiliation:
Kazan Federal University, 420008, Kremlyovskaya St. 18, Kazan, Russian Federation email: [email protected]
Eldar N. Irtuganov
Affiliation:
Kazan Federal University, 420008, Kremlyovskaya St. 18, Kazan, Russian Federation email: [email protected] Academy of Sciences of Tatarstan, 420111, Bauman St. 20, Kazan, Russian Federation
Irek M. Khamitov
Affiliation:
TUBITAK National Observatory, 07058, Akdeniz University Campus, Antalya, Turkey
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

. The black hole X-ray binary V404Cyg was studied during of the 2015 outburst. Optical photometry and spectroscopy were performed by using 1.5-meter Russian-Turkish telescope (RTT-150) facilities at the TUBITAK National Observatory (Antalya, Turkey). From June 22 to June 28, 2015, shell expansion velocity decreased from 650 to 400 km s–1 as measured by Hα and Hβ lines and from 450 to 330 km s–1 as measured by HeI and HeII lines. Thus, the shell expansion occurred with deceleration, where the hydrogen and helium line formation regions are at different radial distances from the center of the star. The correlation of flow variability in the optical and X-ray ranges is caused by fluctuations in the rate of accretion near a compact source where X-ray photons are generated.

Keywords

V404 Cyglow-mass X-ray binary
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 268 - 272
Copyright
© International Astronomical Union 2019 

References

Barthelmy, S.D., D’Ai, A., D’Avanzo, P., Krimm, H.A., Lien, A.Y., Marshall, F.E., Maselli, A., & Siegel, M.H. 2015, GCN, 17929,Google Scholar
Beardmore, A. P., Altamirano, D., Kuulkers, E., Motta, S. E., Osborne, J. P., Page, K. L., Sivakoff, G. R., & Vaughan, S. A. 2015, ATEL, Google Scholar
Blay, P., Munoz-Darias, T., Kajava, J., Casares, J., Motta, S., & Telting, J. 2015, ATEL, Google Scholar
Itoh, R., Watanabe, M., Imai, M., Nakaoka, T., Takaki, K., Shiki, K., Tanaka, Y. T., Uemura, M., & Kawabata, K. S. 2015, ATEL, Google Scholar
Negoro, H., Matsumitsu, T., Mihara, T., Serino, M., Matsuoka, M., Nakahira, S., Ueno, S., Tomida, H., Kimura, M., Ishikawa, M., Nakagawa, Y. E., Sugizaki, M., Shidatsu, M., Sugimoto, J., Takagi, T., Kawai, N., Yoshii, T., Tachibana, Y., Yoshida, A., Sakamoto, T., Kawakubo, Y., Ohtsuki, H., Tsunemi, H., Imatani, R., Nakajima, M., Tanaka, K., Ueda, Y., Kawamuro, T., Hori, T., Tsuboi, Y., Kanetou, S., Yamauchi, M., Itoh, D., Yamaoka, K., & Morii, M. 2015, ATEL, Google Scholar
Panopoulou, G., Reig, P., & Blinov, D. 2015, ATEL, Google Scholar
Rahoui, Farid, Tomsick, J. A., Gandhi, P., Casella, P., Frst, F., Natalucci, L., Rossi, A., Shaw, A. W., Testa, V., & Walton, D. J. 2017, MNRAS, 465, 4468 CrossRefGoogle Scholar