The rotation-powered nature of some soft gamma-ray repeaters and anomalous X-ray pulsars

Coelho, Jaziel G.; Cáceres, D. L.; Lima, Rafael C. R. de; Malheiro, M.; Rueda, J. A.; Ruffini, Remo

doi:10.1051/0004-6361/201629521

Cited by 20 publications

(16 citation statements)

References 59 publications

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“…Very recently, to investigate the possibility that some of soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) family could be canonical rotation-powered pulsars, Coelho et al (2017) adopted realistic NS structure parameters (e.g., mass, radius, and moment of inertia) instead of fiducial values and considered the issue related to the high-energy luminosity and the spin-down luminosity of SGRs and AXPs in detail. Their results provide useful constraints on the initial spin period P 0 of PSR J1640−4631.…”

Section: Nuclear Eos and Moment Of Inertiamentioning

confidence: 99%

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

Gao

Wang

Shan

et al. 2017

ApJ

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In this work, we interpreted the high braking index of PSR J1640−4631 with a combination of the magnetodipole radiation and dipole magnetic field decay models. By introducing a mean rotation energy conversion coefficient z , the ratio of the total high-energy photon energy to the total rotation energy loss in the whole life of the pulsar, and combining the pulsar's high-energy and timing observations with a reliable nuclear equation of state, we estimate the pulsar's initial spin period, P 17 44 0~( -) ms, corresponding to the moment of inertia I 0.8 2.1 10 45( -) g cm 2 .Assuming that PSR J1640−4631 has experienced a long-term exponential decay of the dipole magnetic field, we calculate the true age t age , the effective magnetic field decay timescale D t , and the initial surface dipole magnetic field at the pole B 0 p ( ) of the pulsar to be 2900−3100 yr, 1.07 2 10 5 ( ) yr, and 1.84 4.20 10 13 ( -) G, respectively. The measured braking index of n 3.15 3 = ( ) for PSR J1640−4631 is attributed to its long-term dipole magnetic field decay and a low magnetic field decay rate, dB dt 1.66 3.85 10 p 8-( -) G yr −1 . Our model can be applied to both the high braking index (n 3 > ) and low braking index (n 3 < ) pulsars, tested by the future polarization, timing, and high-energy observations of PSR J1640−4631.

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Section: Nuclear Eos and Moment Of Inertiamentioning

confidence: 99%

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

Gao

Wang

Shan

et al. 2017

ApJ

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“…It will be worthwhile to study the effects of the magnetic field [83][84][85][86], generalization of static compact objects to anisotropic [87][88][89][90][91][92], rotating [93][94][95][96][97][98][99][100][101][102], rapidly rotating [103][104][105][106][107][108][109][110] on the structure properties of neutron stars with a quark matter in core can be interesting topics. We leave these issues for future works.…”

Section: Discussionmentioning

confidence: 99%

Contraction of cold neutron star due to in the presence a quark core

2019

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Motivated by importance of the existence of quark matter on structure of neutron star. For this purpose, we use a suitable equation of state (EoS) which include three different parts: (i) a layer of hadronic matter, (ii) a mixed phase of quarks and hadrons, and, (iii) a strange quark matter in the core. For this system, in order to do more investigation of the EoS, we evaluate energy, Le Chatelier's principle and stability conditions. Our results show that the EoS satisfies these conditions. Considering this EoS, we study the effect of quark matter on the structure of neutron stars such as maximum mass and the corresponding radius, average density, compactness, Kretschmann scalar, Schwarzschild radius, gravitational redshift and dynamical stability. Also, considering the mentioned EoS in this paper, we find that the maximum mass of hybrid stars is a little smaller than that of the corresponding pure neutron star. Indeed the maximum mass of hybrid stars can be quite close to the pure neutron stars. Our calculations about the dynamical stability show that these stars are stable against the radial adiabatic infinitesimal perturbations. In addition, our analyze indicates that neutron stars are under a contraction due to the existence of quark core.

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“…It will be worthwhile to study the effects of the magnetic field [76][77][78][79], generalization of static compact objects to anisotropic [80][81][82][83][84][85], rotating [86][87][88][89][90][91][92][93][94][95], rapidly rotating [96][97][98][99][100][101][102][103] on the structure properties of neutron stars with a quark matter in core can be interesting topics. We leave these issues for future works.…”

Section: Discussionmentioning

confidence: 99%

Contraction of cold neutron star due to in the presence a quark core

Panah,

Yazdizadeh,

Bordbar

2018

Preprint

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Motivated by importance of the existence of quark matter on structure of neutron star. For this purpose, we use a suitable equation of state (EoS) which include three different parts: i) a layer of hadronic matter, ii) a mixed phase of quarks and hadrons, and, iii) a strange quark matter in the core. For this system, in order to do more investigation of the EoS, we evaluate energy, Le Chatelier's principle and stability conditions. Our results show that the EoS satisfies these conditions. Considering this EoS, we study the effect of quark matter on the structure of neutron stars such as maximum mass and the corresponding radius, average density, compactness, Kretschmann scalar, Schwarzschild radius, gravitational redshift and dynamical stability. Also we find an upper limit for the maximum mass of these stars. Indeed, our results show that there is no any massive neutron star with mass more than 2M ⊙ ( M ⊙ is solar mass), when we consider a quark core for this object. This means that in the center of massive neutron stars with mass more than 2M ⊙ (for example 4U 1700 − 377 and J1748 − 2021B with masses about 2.4M ⊙ and 2.7M ⊙ , respectively), there is no any quark core. In addition, our analyze indicates that neutron stars are under a contraction due to the existence of quark core.

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The rotation-powered nature of some soft gamma-ray repeaters and anomalous X-ray pulsars

Cited by 20 publications

References 59 publications

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

The Dipole Magnetic Field and Spin-down Evolutions of the High Braking Index Pulsar PSR J1640–4631

Contraction of cold neutron star due to in the presence a quark core

Contraction of cold neutron star due to in the presence a quark core

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