The 2006 radio outbursts of a microquasar Cygnus X-3: Observations and data

被引：8

作者：

Tsuboi, Masato ^{[1
]}

Tosaki, Tomoka ^{[1
]}

Kuno, Nario ^{[1
]}

Nakanishi, Kouichiro ^{[1
]}

Sawada, Tsuyoshi ^{[1
]}

Umemoto, Tomofumi ^{[1
]}

Trushkin, Sergei A. ^{[2
]}

Kotani, Taro ^{[3
]}

Kawai, Nobuyuki ^{[3
]}

Kurono, Yasutaka ^{[4
]}

Handa, Toshihiro ^{[4
]}

Kohno, Kotaro ^{[4
]}

Tsukagoshi, Takashi ^{[5
]}

Kameya, Osamu ^{[6
]}

Kobayashi, Hideyuki ^{[6
]}

Fujisawa, Kenta ^{[7
]}

Doi, Akihiro ^{[7
]}

Omodaka, Toshihiro ^{[8
]}

Takaba, Hiroshi ^{[9
]}

Sudou, Hiroshi ^{[9
]}

Wakamatsu, Ken-ichi ^{[9
]}

Koyama, Yasuhiro ^{[10
]}

Kawai, Eiji ^{[10
]}

Mochizuki, Nanako ^{[11
]}

Murata, Yasuhiro ^{[11
]}

机构：

[1] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan

[2] RAS, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachaevo Cher, Russia

[3] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan

[4] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1818588, Japan

[5] Grad Univ Adv Studies Sokendai, Tokyo 1818588, Japan

[6] Natl Inst Nat Sci, Natl Astron Observ Japan, Mizusawa VERA Observ, Mizusawa, Iwate 0230861, Japan

[7] Yamaguchi Univ, Fac Sci, Yamaguchi 7538512, Japan

[8] Kagoshima Univ, Fac Sci, Kagoshima 8900065, Japan

[9] Gifu Univ, Fac Engn, Gifu 5011193, Japan

[10] Natl Inst Informat & Commun Technol, Kashima Space Res Ctr, Ibaraki 3148501, Japan

[11] JAXA, Inst Space & Astronaut Sci, Kanagawa 2298510, Japan

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN | 2008年 / 60卷 / 03期

基金：

日本学术振兴会;

关键词：

black hole physics; radio continuum : stars; stars : variables : other;

D O I：

10.1093/pasj/60.3.465

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of multi-frequency observations of radio outbursts of the microquasar Cygnus X-3 in 2006 February and March with the Nobeyama 45-m telescope, the Nobeyama Millimeter Array, and the Yamaguchi 32-m telescope. Since the prediction of a flare by RATAN-600, the source was monitored from January 27 (UT) with these radio telescopes. At the eighteenth day after the quench of activity, successive flares exceeding 1 Jy were successfully observed. The time scale of the variability in the active phase is presumably shorter in higher frequency bands. We also present the result of a follow-up VLBI observation at 8.4 GHz with the Japanese VLBI Network 2.6 d after the first rise. A VLBI image exhibits a single core with a size of < 8 mas (80 AU). The observed image is almost stable, although the core shows a rapid variation in the flux density. No jet structure can be seen at a sensitivity of T-b (brightness temperature) = 7.5 x 10(5) K.

引用

页码：465 / 473

页数：9

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