Application of the Ghosh & Lamb Relation to the Spin-up/down Behavior in the X-ray Binary Pulsar 4U 1626-67

被引：0

作者：

Takagi, Toshihiro ^{[1
,2
]}

Mihara, Tatehiro ^{[2
]}

Sugizaki, Mutsumi ^{[2
]}

Makishima, Kazuo ^{[2
]}

Morii, Mikio ^{[3
]}

机构：

[1] Nihon Univ, Dept Phys, Chiyoda Ku, 1-8-14 Kandasurugadai, Tokyo 1018308, Japan

[2] RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[3] Inst Stat Math, Res Ctr Stat Machine Learning, 10-3 Midori Cho, Tachikawa, Tokyo 1908562, Japan

来源：

PROCEEDINGS OF THE 14TH INTERNATIONAL SYMPOSIUM ON NUCLEI IN THE COSMOS (NIC2016) | 2016年

关键词：

pulsars: individual (4U 1626-67); stars: neutron; X-rays: binaries; EQUATION-OF-STATE; SLIT CAMERA GSC; NUCLEAR-MATTER; MAXI; DISCOVERY; SUPERNOVA;

D O I：

10.7566/JPSCP.14.020301

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the relation proposed by Ghosh & Lamb (1979) between the pulse-period derivative and the X-ray luminosity in binary X-ray pulsars, we tried to constrain the mass and radius of a neutron star. To apply the relation to the binary X-ray pulsar 4U 1626-67, we compiled previous measurements of its period, period derivative, and flux, and added measurements with the MAXI/GSC onboard the International Space Station. The measured period derivative was tightly correlated with the flux, and the relation is successfully explained by the Ghosh & Lamb relation. We found that an assumed distance of, e.g., 8 kpc, gives a mass of 1.39-1.46 solar mass, and a radius as 11.9-12.0 km. This method thus provides a valuable tool to constrain these parameters, even though we need to precisely know the distance [2].

引用

页数：3

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