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AXPs & SGRs: Magnetar or Quarctar?

Published online by Cambridge University Press:  20 March 2013

Guojun Qiao ,
Xionwei Liu ,
Renxin Xu ,
Yuanjie Du ,
Jinlin Han ,
Hao Tong  and
Hongguang Wang
Guojun Qiao
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, China, email: gjn@pku.edu.cn, xiongwliu@163.com, r.x.xu@pku.edu.cn
Xionwei Liu
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, China, email: gjn@pku.edu.cn, xiongwliu@163.com, r.x.xu@pku.edu.cn
Renxin Xu
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, China, email: gjn@pku.edu.cn, xiongwliu@163.com, r.x.xu@pku.edu.cn
Yuanjie Du
Affiliation:
Center for Space Science and Applied Research, CAS, Beijing, 100190, China email: duyj@nssc.ac.cn
Jinlin Han
Affiliation:
National Astronomical Observatories, CAS, Beijing 100012, China email: hjl@nao.cas.cn
Hao Tong
Affiliation:
Xinjiang Astronomical Observatory, CAS, Urumqi, Xinjiang 830011, China email: tonghao@xao.ac.cn
Hongguang Wang
Affiliation:
Center for Astrophysics, Guangzhou University, Guangzhou 510400, China email: cosmic008@yahoo.com.cn
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Abstract

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The concept of a “magnetar” was proposed mainly because of two factors. First, the X-ray luminosity of Anomalous X-ray Pulsars (AXPs) and Soft Gamma-Ray Repeaters (SGRs) is larger than the rotational energy loss rate (Lx > Ėrot), and second, the magnetic field strength calculated from “normal method” is super strong. It is proposed that the radiation energy of magnetar comes from its magnetic fields. Here it is argued that the magnetic field strength calculated through the normal method is incorrect at the situation Lx > Ėrot, because the wind braking is not taken into account. Besides, the “anti-magnetar” and some other X-ray and radio observations are difficult to understand with a magnetar model.

Instead of the magnetar, we propose a “quarctar”, which is a crusted quark star in an accretion disk, to explain the observations. In this model, the persistent X-ray emission, burst luminosity, spectrum of AXPs and SGRs can be understood naturally. The radio-emitting AXPs, which are challenging the magnetar, can also be explained by the quarctar model.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 474 - 476
Copyright
Copyright © International Astronomical Union 2013

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