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Two optical emission components with different variability in V404 Cygni

Published online by Cambridge University Press:  23 June 2017

Yutaro Tachibana ,
Taketoshi Yoshii  and
Nobuyuki Kawai
Yutaro Tachibana
Affiliation:
Department of Physics, Tokyo Institute of Technology, 2-12-1, Ohokayama, Tokyo, Japan email: [email protected]
Taketoshi Yoshii
Affiliation:
Department of Physics, Tokyo Institute of Technology, 2-12-1, Ohokayama, Tokyo, Japan email: [email protected]
Nobuyuki Kawai
Affiliation:
Department of Physics, Tokyo Institute of Technology, 2-12-1, Ohokayama, Tokyo, Japan email: [email protected]
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Abstract

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V404 Cygni went into an outburst again on June 15, 2015 after 26 years of quietness. Soon after the notifications, we started intense optical observation campaign of this source. The spectral index between RC and IC-band was stable over the outburst, whereas that between g′ and RC-band varied violently. With the time domain analysis of the multi-color optical light curves, we successfully decomposed optical variations into three components: highly-variable component (HVC), little-variable component (LVC). The loci of the LVC in the color-color diagram is consistent with that of a single temperature blackbody radiation or a multi-color blackbody radiation from a standard accretion disk, while those of the HVC trace that of power-law spectra.

Keywords

X-rays: binariesStars: individual (V404 Cygni)Techniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S324: New Frontiers in Black Hole Astrophysics , September 2016 , pp. 43 - 44
Copyright
Copyright © International Astronomical Union 2017 

References

Ferrigno, C., Bozzo, E., & Boissay, R. 2015, ATel, 7731, 1 Google Scholar
Gandhi, P., Littlefair, S. P., Hardy, L. K., et al. 2016, MNRAS, 631, 976 Google Scholar
Kimura, M., Isogai, K., Kato, T., et al. 2016, Nature, 529, 54 Google Scholar
Croat, T. K., Stadermann, F. J., & Bernatowicz, T. J. 2005, ApJ, 631, 976 Google Scholar
Makino, F. 1989, IAU Circ., 4782, 1 Google Scholar
Martí, J., Luque-Escamilla, P. L., & García-Hernández, M. T. 2005, A&A, 586, A58 Google Scholar
Tanaka, Y. & Shibazaki, N. 1996, ARA&A, 34, 607 Google Scholar
Tanaka, Y. T., Itoh, R., & Uemura, M., et al. 2016, PASJ, 823, 8 Google Scholar