3XMM J181923.7–170616: An X-Ray Binary with a 408 s Pulsar
文献类型：期刊论文
| 作者 | Qiu,Hao1; Zhou,Ping1,2,3; Yu,Wenfei4; Li,Xiangdong1,3; Xu,Xiaojie1,3 |
| 刊名 | The Astrophysical Journal
 |
| 出版日期 | 2017-09-20 |
| 卷号 | 847期号:1 |
| 关键词 | binaries: symbiotic stars: individual (3XMM J181923.7–170616 = Swift J1819.2–1706) X-rays: binaries |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/aa8728 |
| 英文摘要 | Abstract We carry out a dedicated study of 3XMM?J181923.7–170616 with an approximate pulsation period of 400?s using the XMM-Newton and Swift observations spanning across nine years. We have refined the period of the source to 407.904(7) s (at epoch MJD 57142) and constrained the 1σ upper limit on the period derivative . The source radiates hard, persistent X-ray emission during the observation epochs, which is best described by an absorbed power-law model (Γ?～?0.2–0.8) plus faint Fe lines at 6.4 and 6.7 keV. The X-ray flux revealed a variation within a factor of 2, along with a spectral hardening as the flux increased. The pulse shape is sinusoid-like and the spectral properties of different phases do not present significant variation. The absorption ( ) is similar to the total Galactic hydrogen column density along the direction, indicating that it is a distant source. A search for the counterpart in optical and near-infrared surveys reveals a low-mass K-type giant, while the existence of a Galactic OB supergiant is excluded. A symbiotic X-ray binary (SyXB) is the favored nature of 3XMM?J181923.7–170616 and can essentially explain the low luminosity of , slow pulsation, hard X-ray spectrum, and possible K3?III companion. An alternative explanation of the source is a persistent Be X-ray binary (BeXB) with a companion star no earlier than B3-type. |
| 语种 | 英语 |
| WOS记录号 | IOP:0004-637X-847-1-AA8728 |
| 出版者 | The American Astronomical Society |
| 源URL | [http://119.78.226.72/handle/331011/32107]  |
| 专题 | 中国科学院上海天文台 |
| 作者单位 | 1.School of Astronomy and Space Science, Nanjing University, 163 Xianlin Avenue, Nanjing 210023, China 2.Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands; p.zhou@uva.nl 3.Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing, China 4.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China |
| 推荐引用方式 GB/T 7714 | Qiu,Hao,Zhou,Ping,Yu,Wenfei,et al. 3XMM J181923.7–170616: An X-Ray Binary with a 408 s Pulsar[J]. The Astrophysical Journal,2017,847(1). |
| APA | Qiu,Hao,Zhou,Ping,Yu,Wenfei,Li,Xiangdong,&Xu,Xiaojie.(2017).3XMM J181923.7–170616: An X-Ray Binary with a 408 s Pulsar.The Astrophysical Journal,847(1). |
| MLA | Qiu,Hao,et al."3XMM J181923.7–170616: An X-Ray Binary with a 408 s Pulsar".The Astrophysical Journal 847.1(2017). |
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