Super‐Massive Neutron Stars

  title={Super‐Massive Neutron Stars},
  author={Paulo C. C. Freire},
  journal={arXiv: Astrophysics},
  • P. Freire
  • Published 30 November 2007
  • Physics
  • arXiv: Astrophysics
We present here the results of the timing of PSR B1516+02B, a 7.95‐ms pulsar in a binary system with a ∼0.17M⊙ companion and an orbital period of 6.85 days located in the globular cluster M5. The eccentricity of the orbit (e = 0.14) has allowed a measurement of the rate of advance of periastron: ω = (0.0136±0.0004)° yr−1. It is very likely that the periastron advance is due to the effects of general relativity; the total mass of the binary system is (2.14±0.08)M⊙. The small measured mass… 

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  • 2006
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  • 2005
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  • 2004