High-energy Emissions from the Pulsar/Be Binary System PSR J2032+4127/MT91 213

被引：32

作者：

Takata, J. ^{[1
]}

Tam, P. H. T. ^{[2
]}

Ng, C. W. ^{[3
]}

Li, K. L. ^{[4
]}

Kong, A. K. H. ^{[5
,6
]}

Hui, C. Y. ^{[7
]}

Cheng, K. S. ^{[3
]}

机构：

[1] Huazhong Univ Sci & Technol, Sch Phys, Wuhan 430074, Peoples R China

[2] Sun Yat Sen Univ, Inst Astron & Space Sci, Guangzhou 510275, Guangdong, Peoples R China

[3] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China

[4] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[5] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan

[6] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan

[7] Chungnam Natl Univ, Dept Astron & Space Sci, Daejon 305764, South Korea

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 836卷 / 02期

基金：

新加坡国家研究基金会;

关键词：

methods: numerical; methods: observational; pulsars: individual (PSR J2032+4127); radiation mechanisms: non-thermal; stars: massive; X-rays: binaries; GAMMA-RAY BINARY; MULTIWAVELENGTH LIGHT CURVES; INVERSE COMPTON-SCATTERING; 2004 PERIASTRON PASSAGE; B1259-63/LS; 2883; LS; 5039; MASSIVE BINARIES; STELLAR WINDS; MODEL; TEV;

D O I：

10.3847/1538-4357/aa5c80

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

PSR. J2032+4127 is a radio-loud gamma-ray-emitting pulsar; it is orbiting around a high-mass Be type star with a very long orbital period of 25-50 years, and is approaching periastron, which will occur in late 2017/early 2018. This system comprises a young pulsar and a Be type star, which is similar to the so-called gamma-ray binary PSR. B1259-63/LS2883. It is expected therefore that PSR. J2032+4127 shows an enhancement of high-energy emission caused by the interaction between the pulsar wind and Be wind/disk around periastron. Ho et al. recently reported a rapid increase in the X-ray flux from this system. In this paper, we also confirm a rapid increase in the X-ray flux along the orbit, while the GeV flux shows no significant change. We discuss the high-energy emissions from the shock caused by the pulsar wind and stellar wind interaction and examine the properties of the pulsar wind in this binary system. We argue that the rate of increase of the X-ray flux observed by Swift indicates (1) a variation of the momentum ratio of the two-wind interaction region along the orbit, or (2) an evolution of the magnetization parameter of the pulsar wind with the radial distance from the pulsar. We also discuss the pulsar wind/Be disk interaction at the periastron passage, and propose the possibility of formation of an accretion disk around the pulsar. We model high-energy emissions through the inverse-Compton scattering process of the cold-relativistic pulsar wind off soft photons from the accretion disk.

引用

页数：18

共 89 条

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