首页> 外文期刊>Nature >An ultraluminous X-ray source powered by an accreting neutron star
【24h】

An ultraluminous X-ray source powered by an accreting neutron star

机译:由正中子星驱动的超发光X射线源

获取原文
获取原文并翻译 | 示例
           

摘要

The majority of ultraluminous X-ray sources are point sources that are spatially offset from the nuclei of nearby galaxies and whose X-ray luminosities exceed the theoretical maximum for spherical infall (the Eddington limit) onto stellar-mass black holes. Their X-ray luminosities in the 0.5-10 kiloelectronvolt energy band range from 10~(39) to 10~(41) ergs per second. Because higher masses imply less extreme ratios of the luminosity to the isotropic Eddington limit, theoretical models have focused on black hole rather than neutron star systems. The most challenging sources to explain are those at the luminous end of the range (more than 10~(40) ergs per second), which require black hole masses of 50-100 times the solar value or significant departures from the standard thin disk accretion that powers bright Galactic X-ray binaries, or both. Here we report broadband X-ray observations of the nuclear region of the galaxy M82 that reveal pulsations with an average period of 1.37 seconds and a 2.5-day sinusoidal modulation. The pulsations result from the rotation of a magnetized neutron star, and the modulation arises from its binary orbit. The pulsed flux alone corresponds to an X-ray luminosity in the 3-30 kiloelectronvolt range of 4.9 × 10~(39) ergs per second. The pulsating source is spatially coincident with a variable source that can reach an X-ray luminosity in the 0.3-10 kiloelectronvolt range of 1.8 × 10~(40) ergs per second. This association implies a luminosity of about 100 times the Eddington limit for a 1.4-solar-mass object, or more than ten times brighter than any known accreting pulsar. This implies that neutron stars may not be rare in the ultraluminous X-ray population, and it challenges physical models for the accretion of matter onto magnetized compact objects.
机译:大多数超发光X射线源都是点光源,这些点光源在空间上偏离附近星系的原子核,并且它们的X射线光度超过了理论上球形恒星黑洞的最大入射角(爱丁顿极限)。它们在0.5-10千伏电子能带的X射线发光度范围为每秒10〜(39)到10〜(41)ergs。由于较高的质量意味着光度与各向同性爱丁顿极限的极端比率较小,因此理论模型将重点放在黑洞而不是中子星系统上。要解释的最具挑战性的光源是处于该范围的发光端(每秒超过10〜(40)ergs)的光源,这些光源需要黑洞质量是太阳值的50-100倍,或者与标准薄磁盘的吸积有明显偏差可以为明亮的银河X射线二进制文件或两者提供动力。在这里,我们报告了对银河系M82核区域进行的宽带X射线观察,该观察结果揭示了平均周期为1.37秒和2.5天正弦调制的脉动。脉动是由磁化中子星的旋转产生的,而调制是由其中枢轨道产生的。单独的脉冲通量对应于在4.9×10〜(39)ergs /秒的3-30千伏电压范围内的X射线发光度。脉动源与可变源在空间上重合,可变源可以在0.3×10千电子伏范围内以每秒1.8×10〜(40)ergs的速度达到X射线发光度。这种关联意味着光度约为1.4太阳质量物体的爱丁顿极限的100倍,或者比任何已知的增生脉冲星的亮度高十倍。这意味着中子星在超发光的X射线族中可能并不罕见,并且对物质在磁化的紧凑物体上积聚的物理模型提出了挑战。

著录项

  • 来源
    《Nature》 |2014年第7521期|202-204|共3页
  • 作者单位

    Universite de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planetologie, 9;

    Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France,CNRS, Institut de Recherche en Astrophysique et Planetologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Universite de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planetologie, 9;

    Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France,CNRS, Institut de Recherche en Astrophysique et Planetologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France;

    Physics Department, Columbia University, 538 West 120th Street, New York, New York 10027, USA;

    Space Sciences Laboratory, University of California, Berkeley, California 94720, USA;

    DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark;

    Lawrence Livermore National Laboratory, Livermore, California 94550, USA;

    Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA, UK;

    Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA;

    NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA;

    Department of Physics, McGill University, Montreal, Quebec H3A 2T8, Canada;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Department of Physics, Texas Tech University, Lubbock, Texas 79409, USA;

    Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, Michigan 48109-1042, USA;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA;

    Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology, Pasadena, California 91125, USA;

    Space Sciences Laboratory, University of California, Berkeley, California 94720, USA;

    Universite de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planetologie, 9;

    Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France,CNRS, Institut de Recherche en Astrophysique et Planetologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France;

    NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱:kefu@zhangqiaokeyan.com

京公网安备:11010802029741号 ICP备案号:京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有
  • 客服微信

  • 服务号