Low X-ray Efficiency of a Young High-B Pulsar PSR J1208-6238 Observed with Chandra

被引：2
作者：
Bamba, Aya [1 ,2 ]
Watanabe, Eri [3 ]
Mori, Koji [4 ]
Shibata, Shinpei [5 ]
Terada, Yukikatsu [6 ]
Sano, Hidetoshi [7 ,8 ,9 ]
Filipovic, Miroslav D. [10 ]
机构：
[1] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[2] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[3] Yamagata Univ, Dept Phys, 1-4-12 Kojirakawa Machi, Yamagata, Yamagata 9908560, Japan
[4] Miyazaki Univ, Fac Engn, Dept Appl Phys & Elect Engn, 1-1 Gakuen Kibanadai Nishi, Miyazaki 8892192, Japan
[5] Yamagata Univ, Sch Sci & Technol, 1-4-12 Kojirakawa Machi, Yamagata, Yamagata 9908560, Japan
[6] Saitama Univ, Dept Phys, Sci, Sakura, Saitama 3388570, Japan
[7] Nagoya Univ, Inst Adv Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan
[8] Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan
[9] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
[10] Western Sydney Univ, Locked Bag 1797, Penrith, NSW 2751, Australia
来源：
ASTROPHYSICS AND SPACE SCIENCE | 2020年 / 365卷 / 11期
关键词：
Pulsars: individual (PSR J1208-6238); Stars: neutron; Stars: magnetars; Magnetic field; X-rays: stars; ISM: supernova remnants; EMISSION; DISCOVERY;
D O I：
10.1007/s10509-020-03891-6
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
High magnetic field (high-B) pulsars are key sources to bridge magnetars and conventional rotation powered pulsars, and thus to understand the origin of magnetar activities. We have estimated a tight upper limit on the X-ray flux of one of the youngest high-B pulsars PSR J1208-6238 for the first time; a Chandra 10 ks observation shows no significant source. Depending on the emission models, we have the 3 sigma upper limit on the intrinsic 0.5-7 keV flux to 2.2-10.0x10(-14) erg s(-1) cm(-2). Assuming the distance to the pulsar to be 3 kpc, we suggest that the conversion efficiency from the spin-down energy to the X-ray luminosity of this pulsar is almost the smallest among known high-B pulsars, and even smaller for those for a typical rotation-powered one. We also discuss possible associations of a surrounding pulsar wind nebula and a hosting supernova remnant around this high-B pulsar.
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页数：6
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