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Light Curves for Rapidly Rotating Neutron Stars

Coire Cadeautheoretical Physics Institute, Department of Physics, University of Alberta, Edmonton, CanadaSharon M. Morsinktheoretical Physics Institute, Department of Physics, University of Alberta, Edmonton, CanadaD. A. LeahyDept of Physics and Astronomy, University of Calgary, Calgary, CanadaSheldon CampbellDepartment of Physics, Texas A&M University, College Station, TX

2006en

ABI

Annotatsiya

We present raytracing computations for light emitted from the surface of a rapidly-rotating neutron star in order to construct light curves for X-ray pulsars and bursters. These calculations are for realistic models of rapidly-rotating neutron stars which take into account both the correct exterior metric and the oblate shape of the star. We find that the most important effect arising from rotation comes from the oblate shape of the rotating star. We find that approximating a rotating neutron star as a sphere introduces serious errors in fitted values of the star's radius and mass if the rotation rate is very large. However, in most cases acceptable fits to the ratio M/R can be obtained with the spherical approximation.

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Identifikatorlar

DOI: 10.1086/509103

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