Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-04T21:53:38.275Z Has data issue: false hasContentIssue false
  • English
  • Français

Investigation of the Optical Variability of Relativistic Objects with High Time Resolution

Published online by Cambridge University Press:  12 April 2016

S. N. Mitronova ,
G. M. Beskin ,
S. I. Neizvestny ,
V. L. Plokhotnichenko ,
M. Yu. Popova ,
S. Zharikov ,
O. G. Benvenuto ,
C. Feinstein ,
M. Mendez  and
V. Boriakoff
...Show all authors
S. N. Mitronova
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
G. M. Beskin
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
S. I. Neizvestny
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
V. L. Plokhotnichenko
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
M. Yu. Popova
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
S. Zharikov
Affiliation:
Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia
O. G. Benvenuto
Affiliation:
Observatorio Astronomico de la Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
C. Feinstein
Affiliation:
Observatorio Astronomico de la Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
M. Mendez
Affiliation:
Observatorio Astronomico de la Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
V. Boriakoff
Affiliation:
Worcester Polytechnic Institute, USA
D. Dossa
Affiliation:
Worcester Polytechnic Institute, USA

Extract

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.

1. Detection of nonthermal optical flares in low mass X-ray binaries. Eleven low-mass X-ray binaries have been observed with the MANIA (Multichannel Analysis of Nanoseconds Intensity Alteration) complex; X0420+32, A0620-00, X1728–169, X1813–14, X1957+11 in 1986 at the 6 m telescope of SAO [7], and 2S0921–630, 4U1543–475, 4U1636–536, 4U1559–487, MXB1735–44, 4U1822–371 in 1991 at the 2.15 m telescope of CASLEO (Argentina) [1]. Analysis of the data using the special y2 and d2 function formalism [4], [6] has shown no brightness variations on time-scales of 10−7... 10 s for all objects except A0620–00 and MXB1735–44.

A0620–00. The five millisecond flashes were detected on 1986 February 13 (Fig. 1). The first two flares have durations of 3 ms and 5 ms and their rise times were 1...2 ms. The other three events lasted 0.4…0.5 ms with rise times of about 0.1 ms. The lower limit of the flare amplitudes is 40 counts ms−1 and the corresponding brightness temperatures are 5 109 K for the first two and 5 1011 K for the others.

Type
X-Ray Binaries
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 403 - 404
Copyright
Copyright © Kluwer 1996

References

1. Beskin, G.M., Neizvestny, S.I., Plokhotnichenko, V.L., et al., 1994, A&A, 289, 141 Google Scholar
2. Boriakoff, V., Buccheri, R., Fauci, F., 1983, Nature, 304, 417 CrossRefGoogle Scholar
3. Elvis, M., Page, C.G., Pounds, K.A., et al., 1975, Nature, 257, 656 Google Scholar
4. Plokhotnichenko, V.L., 1983, Soobshchenija SAO, 38, 29 Google Scholar
5. Plokhotnichenko, V.L., 1992, Ph.D. thesis, Special Astrophysical ObservatoryGoogle Scholar
6. Shvartsman, V.F., 1977, Soobshchenija SAO, 19, 5 Google Scholar
7. Shvartsman, V.F., Beskin, G.M., Mitronova, S.N., et al., 1989, Sov. Ast. Let., 15, 590 Google Scholar