2013/07/30 by Jaziel G. Coelho, J. G. Coelho, Coelho, J. G. +2 · 3 citations
Engineering · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #FOS: Physical sciences #Galaxy #Geometry #Geophysics and Sensor Technology #High Energy Astrophysical Phenomena (astro-ph.HE) #Luminosity #Magnetic field #Neutron star #Nuclear Theory (nucl-th) #Physics #Pulsar #Pulsars and Gravitational Waves Research #Quantum mechanics #Rotation (mathematics) #Rotational energy #Solar and Stellar Astrophysics (astro-ph.SR) #Spin (aerodynamics) #X-ray pulsar #astro-ph.HE #astro-ph.SR #nucl-th
paper · pdf · doi:10.48550/arxiv.1307.8158
published in arXiv (Cornell University) (Cornell University) · Contribution for the Conference Proceedings of the Compact Stars in the QCD Phase Diagram III (CSQCD III), December 12-15, 2012, Guarujá, Brazil. http://www.astro.iag.usp.br/~foton/CSQCD3
arxiv created 2013/07/30 · openalex publication_date 2013/07/30 · arxiv updated 2013/08/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
SGRs/AXPs are considered a subclass of pulsars powered by magnetic energy and not by rotation, as normal radio pulsars. They are understood as strongly magnetized neutron star, with large periods of rotation P∼(2-12) s, and large spin-down, with typical P∼(10-13-10-10) s/s in contrast to P∼10-15 s for ordinary pulsars. Their persistent X-ray luminosity, as well as the bursts and flares typical of these sources, are instead believed to be powered by the decay of their ultrastrong magnetic field. SGRs/AXPs typically have a larger X-ray luminosity that can not be explained by their spin-down luminosity (LX>E\rm rot), unlike rotation-powered pulsars. However, the recent discovery of radio-pulsed emission in four of this class of sources, where the spin-down rotational energy lost E\rm rot is larger than the X-ray luminosity LX during the quiescent state - as in normal pulsars - opens the question of the nature of these radio sources in comparison to the others of this class. In this contribution, we show that the radio SGRs/AXPs obey a linear log-log relation between LX and E\rm rot, very similar to the one satisfied by X-ray and gamma-ray neutron star pulsars, suggesting their neutron star nature. Furthermore, we show that almost all the high-B pulsars are also near the line found for the radio AXPs. In contrast, for almost all the others SGRs/AXPs, log LX does not vary too much as function of log E\rm rot, a phenomenology not shared by X-ray neutron star pulsars, suggesting a different nature for these sources.