MULTI-WAVELENGTH OBSERVATIONS OF THE BLACK WIDOW PULSAR 2FGL J2339.6-0532 WITH OISTER AND SUZAKU

被引：7

作者：

Yatsu, Yoichi ^{[1
]}

Kataoka, Jun ^{[2
]}

Takahashi, Yosuke ^{[2
]}

Tachibana, Yutaro ^{[1
]}

Kawai, Nobuyuki ^{[1
]}

Shibata, Shimpei ^{[3
]}

Pike, Sean ^{[4
]}

Yoshii, Taketoshi ^{[1
]}

Arimoto, Makoto ^{[1
]}

Saito, Yoshihiko ^{[1
]}

Nakamori, Takeshi ^{[3
]}

Sekiguchi, Kazuhiro ^{[5
]}

Kuroda, Daisuke ^{[6
]}

Yanagisawa, Kenshi ^{[6
]}

Hanayama, Hidekazu ^{[7
]}

Watanabe, Makoto ^{[8
]}

Hamamoto, Ko ^{[8
]}

Nakao, Hikaru ^{[8
]}

Ozaki, Akihito ^{[8
]}

Motohara, Kentaro ^{[9
]}

Konishi, Masahiro ^{[9
]}

Tateuchi, Ken ^{[9
]}

Matsunaga, Noriyuki ^{[10
]}

Morokuma, Tomoki ^{[9
,10
]}

Nagayama, Takahiro ^{[11
,12
]}

Murata, Katsuhiro ^{[11
]}

Akitaya, Hiroshi ^{[13
]}

Yoshida, Michitoshi ^{[13
]}

Ali, Gamal B. ^{[14
]}

Essam, A. ^{[14
]}

Isogai, Mizuki ^{[15
]}

Arai, Akira ^{[15
]}

Takahashi, Hidenori ^{[9
,16
]}

Hashimoto, Osamu ^{[16
]}

Miyanoshita, Ryo ^{[12
]}

Omodaka, Toshihiro ^{[12
]}

Takahashi, Jun ^{[17
]}

Tokimasa, Noritaka ^{[17
]}

Matsuda, Kentaro ^{[17
]}

Okumura, Shin-Ichiro ^{[18
]}

Nishiyama, Kota ^{[18
]}

Urakawa, Seitaro ^{[18
]}

Nogami, Daisaku ^{[19
]}

Oasa, Yumiko ^{[20
]}

机构：

[1] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ohokayama, Tokyo 1528551, Japan

[2] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[3] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan

[4] Brown Univ, Dept Phys, Providence, RI 02912 USA

[5] Natl Astron Observ Japan, Natl Inst Nat Sci, Mitaka, Tokyo 1818588, Japan

[6] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan

[7] Natl Astron Observ Japan, Ishigakijima Astron Observ, Ishigaki, Okinawa 9070024, Japan

[8] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan

[9] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan

[10] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan

[11] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan

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

[13] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan

[14] Natl Res Inst Astron & Geophys, Cairo 11722, Egypt

[15] Kyoto Sangyo Univ, Kamiyama Astron Observ, Kita Ku, Kyoto 6038555, Japan

[16] Gunma Astron Observ, Takayama, Gunma 3770702, Japan

[17] Univ Hyogo, Ctr Astron, Nishi Harima Astron Observ, Sayo Cho, Hyogo 6795313, Japan

[18] Japan Spaceguard Assoc, Bisei Spaceguard Ctr, Ibara, Okayama 7141411, Japan

[19] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan

[20] Saitama Univ, Fac Educ, Sakura, Saitama, Japan

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 802卷 / 02期

关键词：

gamma rays: stars; pulsars: general; pulsars: individual (2FGL J2339.6-0532); X-rays: binaries; HUBBLE-SPACE-TELESCOPE; X-RAY; MILLISECOND PULSAR; GAMMA-RAY; ACCRETION; ROTATION; DISCOVERY; WIND; OBJECT; NEBULA;

D O I：

10.1088/0004-637X/802/2/84

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Multi-wavelength observations of the black widow binary system 2FGL J2339.6-0532 are reported. The Fermi gamma-ray source 2FGL J2339.6-0532 was recently categorized as a black widow in which a recycled millisecond pulsar (MSP) is evaporating the companion star with its powerful pulsar wind. Our optical observations show clear sinusoidal light curves due to the asymmetric temperature distribution of the companion star. Assuming a simple geometry, we constrained the range of the inclination angle of the binary system to 52 degrees < i < 59 degrees, which enables us to discuss the interaction between the pulsar wind and the companion in detail. The X-ray spectrum consists of two components: a soft, steady component that seems to originate from the surface of the MSP, and a hard, variable component from the wind-termination shock near the companion star. The measured X-ray luminosity is comparable to the bolometric luminosity of the companion, meaning that the heating efficiency is less than 0.5. In the companion orbit, 10(11) cm from the pulsar, the pulsar wind is already in the particle-dominant stage with a magnetization parameter of sigma < 0.1. In addition, we precisely investigated the time variations of the X-ray periodograms and detected a weakening of the orbital modulation. The observed phenomenon may be related to unstable pulsar wind activity or weak mass accretion, both of which can result in the temporal extinction of the radio pulse.

引用

页数：11

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