The effects of mass on the radiation of a relativistically rotating neutron star |
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| Affiliation: | 1. Instituto de Astronomía y Física del Espacio (IAFE), Universidad de Buenos Aires, CC 67–Suc. 28 (C1428ZAA) CABA, Argentina;2. Lab AIM, CEA/CNRS/Université Paris-Saclay, Université de Paris, F-91191 Gif-sur-Yvette, France;3. Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, P.O. Box 3-72, 58090, Morelia, Michoacán, México;4. Mesoamerican Center for Theoretical Physics, Universidad Autónoma de Chiapas, 29050 Tuxtla Gutiérrez, Chiapas, México;1. Institute of Astronomy and Space Physics, CONICET-Universidad de Buenos Aires, Ciudad Universitaria, 1428 Buenos Aires, Argentina;2. Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu−CNRS, CEA-Saclay, pt courrier 131, 91191 Gif-sur-Yvette, France;1. Department of Astronomy, Xiamen University, Xiamen, Fujian 361005, China;2. Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA;3. Department of Astronomy, School of Physics, Peking University, Beijing 100871, China;4. Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing 100871, China |
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| Abstract: | We investigate the effect of mass on the radiation of a relativistically rotating neutron star. The method of Haxton and Ruffini is used to find the radiation flux from a relativistically rotating neutron star. By extending the idea of a point charge orbiting a black hole, a pulsar is modeled by simulating a relativistically rotating magnetic dipole embedded within a neutron star. The resulting equations retain the mass of the neutron star, thereby introducing effects of general relativity on the radiation from the dipole. We present exact solutions to the modeling equation as well as plots of energy spectra at different rotational velocities and inclination angles. We also present plots of total energy versus mass and two tables containing a comparison of energy ratios. These demonstrate that, for realistic neutron star masses, the high speed enhancement of the radiation is always more than compensated by the frame dragging effect, leading to a net reduction of radiation from the star. It is found that the inclusion of mass not only reduced the special relativistic enhancement, but negates it entirely as the mass of the neutron star approaches the mass limit. |
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| Keywords: | Pulsars Neutron stars |
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