Measuring neutron star mass and radius with three mass–radius relations

  1. C. M. Zhang1,*,
  2. H. X. Yin1,
  3. Y. Kojima2,
  4. H. K. Chang3,
  5. R. X. Xu4,
  6. X. D. Li5,
  7. B. Zhang6,
  8. B. Kiziltan7

Article first published online: 8 NOV 2006

DOI: 10.1111/j.1365-2966.2006.11133.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 374, Issue 1, pages 232–236, January 2007

Additional Information

How to Cite

Zhang, C. M., Yin, H. X., Kojima, Y., Chang, H. K., Xu, R. X., Li, X. D., Zhang, B. and Kiziltan, B. (2007), Measuring neutron star mass and radius with three mass–radius relations. Monthly Notices of the Royal Astronomical Society, 374: 232–236. doi: 10.1111/j.1365-2966.2006.11133.x

Author Information

  1. 1

    National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China

  2. 2

    Department of Physics, Hiroshima University, Higashi-Hiroshima 739-8526, Japan

  3. 3

    Department of Physics and Institute of Astronomy, National Tsing Hua University, Hsinchu 30013, Taiwan

  4. 4

    Department of Astronomy, Peking University, Beijing 100871, China

  5. 5

    Department of Astronomy, Nanjing University, Nanjing 210093, China

  6. 6

    Department of Physics, University of Nevada, NV 89154-4002, USA

  7. 7

    Department of Astronomy & Astrophysics, University of California, Santa Cruz, USA

* E-mail: zhangcm@bao.ac.cn

Publication History

  1. Issue published online: 30 NOV 2006
  2. Article first published online: 8 NOV 2006
  3. Accepted 2006 October 2. Received 2006 August 11; in original form 2005 December 6

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Keywords:

  • equation of state;
  • stars: neutron;
  • pulsars: general;
  • X-rays: stars

ABSTRACT

We propose to determine the mass and radius of a neutron star (NS) using three measurable mass–radius relationships, namely the ‘apparent’ radius inferred from the NS thermal emission, the gravitational redshift inferred from the absorption lines, as well as the averaged stellar mass density inferred from the orbital Keplerian frequency derived from the kilohertz quasi-periodic oscillation data. We apply the method to constrain the NS mass and radius of the X-ray sources, 1E 1207.4−5209, Aql X-1 and EXO 0748−676.

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