来自Kes 75中的年轻脉冲星的磁铁状辐射
F P Gavriil1, M E Gonzalez, E V Gotthelf
1NASA/Goddard Space Flight Center, Code 662, Greenbelt, MD 20771, USA. fotis.p.gavriil@nasa.gov
概括
从年轻的脉冲星PSR J1846-0258中检测到类似磁铁的X射线爆发,挑战了以前的分类. 这一发现表明中子星的磁性活动连续存在,与磁场强度有关.
科学领域:
- 天文学和天体物理学
- 高能天体物理学 高能天体物理学
- 中子星物理学 中子星物理学
背景情况:
- 年轻的脉冲星PSR J1846-0258,位于超新星残余Kes 75,此前被认为是完全旋转动力的.
- 它推断的表面双极磁场 (4.9 x 10 ^ 13 高斯) 比大多数旋转动力的脉冲星高,但低于典型的磁星.
研究的目的:
- 为了研究PSR J1846-0258的性质及其潜在的磁器类活动.
- 探索磁场强度和中子星中的磁活性之间的关系.
主要方法:
- 来自PSR J1846-0258.8.的X射线爆发的检测和分析.
- 监测流量变化和与爆发相关的时间行为.
主要成果:
- 从PSR J1846-0258.8观察到类似磁铁的X射线爆发.
- 爆发与X射线流量突然增加的同时发生.
- 记录了脉冲星计时行为的前所未有的变化.
结论:
- 这些发现挑战了旋转动力脉冲星和磁星之间的严格二分法.
- 这些结果表明,与以前想象的相比,磁场较低的中子星中可能会发生类似磁星的行为.
- 建议在中子星中存在磁性活动的连续性,随着磁场强度的增加而增加.
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