It appears you don't have support to open PDFs in this web browser. To view this file, Open with your PDF reader
Abstract
We investigate the possibility of some Soft Gamma-ray Repeaters (SGRs) and Anomalous X-ray Pulsars (AXPs) could be described as rotation-powered neutron stars (NSs). The analysis was carried out by computing the structure properties of NSs, and then we focus on giving estimates for the surface magnetic field using both realistic structure parameters of NSs and a general relativistic model of a rotating magnetic dipole. We show that the use of realistic parameters of rotating neutron stars obtained from numerical integration of the self-consistent axisymmetric general relativistic equations of equilibrium leads to values of the magnetic field and radiation efficiency of SGRs/AXPs very different from estimates based on fiducial parameters. This analysis leads to a precise prediction of the range of NS masses, obtained here by making use of selected up-to-date nuclear equations of state (EOS). We show that 40% (nine) of the entire observed population of SGRs and AXPs can be described as canonical pulsars driven by the rotational energy of neutron stars, for which we give their possible range of masses. We also show that if the blackbody component in soft X-rays is due to the surface temperature of NSs, then 50% of the sources could be explained as ordinary rotation-powered pulsars. Besides, amongst these sources we find the four SGRs/AXPs with observed radio emission and six that are possibly associated with supernova remnants (including Swift J1834.9-0846 as the first magnetar to show a surrounding wind nebula), suggesting as well a natural explanation as ordinary pulsars.
You have requested "on-the-fly" machine translation of selected content from our databases. This functionality is provided solely for your convenience and is in no way intended to replace human translation. Show full disclaimer
Neither ProQuest nor its licensors make any representations or warranties with respect to the translations. The translations are automatically generated "AS IS" and "AS AVAILABLE" and are not retained in our systems. PROQUEST AND ITS LICENSORS SPECIFICALLY DISCLAIM ANY AND ALL EXPRESS OR IMPLIED WARRANTIES, INCLUDING WITHOUT LIMITATION, ANY WARRANTIES FOR AVAILABILITY, ACCURACY, TIMELINESS, COMPLETENESS, NON-INFRINGMENT, MERCHANTABILITY OR FITNESS FOR A PARTICULAR PURPOSE. Your use of the translations is subject to all use restrictions contained in your Electronic Products License Agreement and by using the translation functionality you agree to forgo any and all claims against ProQuest or its licensors for your use of the translation functionality and any output derived there from. Hide full disclaimer
Details
1 Departamento de Física, Instituto Tecnológico de Aeronáutica, ITA - DCTA, Vila das Acácias, São José dos Campos, 12228-900 SP, Brazil
2 INPE - Instituto Nacional de Pesquisas Espaciais, Divisão de Astrofísica, Av. dos Astronautas 1758, São José dos Campos, 12227-010 SP, Brazil
3 ICRANet, P.zza della Repubblica 10, I65122 Pescara, Italy
4 Universidade do Estado de Santa Catarina, Av. Madre Benvenuta, 2007 Itacorubi, 88.035–901, Florianópolis, Brazil; ICRANet, P.zza della Repubblica 10, I65122 Pescara, Italy
5 Departamento de Física, Instituto Tecnológico de Aeronáutica, ITA - DCTA, Vila das Acácias, São José dos Campos, 12228-900 SP, Brazil; Dipartimento di Fisica, Sapienza Universit di Roma, P.le Aldo Moro 5, I-00185 Rome, Italy; ICRANet, P.zza della Repubblica 10, I65122 Pescara, Italy
6 Dipartimento di Fisica, Sapienza Universit di Roma, P.le Aldo Moro 5, I-00185 Rome, Italy; ICRANet, P.zza della Repubblica 10, I65122 Pescara, Italy; ICRANet-Rio, Centro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud 150, 2290–180 Rio de Janeiro, Brazil