The Effects of Rotation on Thermal X‐Ray Afterglows Resulting from Pulsar Glitches

Hui, C. Y.; Cheng, K. S.

doi:10.1086/420764

Cited by 10 publications

(9 citation statements)

References 36 publications

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“…The X-ray pulse profile in 0.7-2 keV resembles the modulation that resulted from a rotating neutron star while a hot spot on the stellar surface sweeps across our line of sight (e.g., Hui & Cheng 2004;Pechenick et al 1983). This is consistent with the scenario inferred from the phase-averaged spectral analysis which favors a model of a blackbody plus power law or a composite blackbody model.…”

Section: Discussionsupporting

confidence: 83%

Discovery of X-Ray Pulsation From the Geminga-Like Pulsar PSR J2021+4026

Lin

Hui

et al. 2013

ApJ

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We report the discovery of an X-ray periodicity of ∼265.3 ms from a deep XMM-Newton observation of the radioquiet γ -ray pulsar, PSR J2021+4026, located at the edge of the supernova remnant G78.2+2.1 (γ -Cygni). The detected frequency is consistent with the γ -ray pulsation determined by the observation of the Fermi Gamma-ray Space Telescope at the same epoch. The X-ray pulse profile resembles the modulation of a hot spot on the surface of the neutron star. The phase-averaged spectral analysis also suggests that the majority of the observed X-rays have thermal origins. This is the third member in the class of radio-quiet pulsars with significant pulsations detected from both X-ray and γ -ray regimes.

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Section: Discussionsupporting

confidence: 83%

Discovery of X-Ray Pulsation From the Geminga-Like Pulsar PSR J2021+4026

Lin

Hui

et al. 2013

ApJ

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“…Fig. 6 in Hui & Cheng 2004). If θ 0 + α ≤ θ max ≤ 180 o and θ 0 − α ≥ 0, then h(θ; α, θ 0 ) is defined as:…”

Section: Analysis Of the X-ray Pulse Profile Of Psr J2021+4026mentioning

confidence: 97%

“…Fig. 6 in Hui & Cheng 2004). We described the stellar surface by angular spherical coordinates θ and φ where θ is measured from the z-axis defined above.…”

Section: Analysis Of the X-ray Pulse Profile Of Psr J2021+4026mentioning

confidence: 99%

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A DETAILED X-Ray INVESTIGATION OF PSR J2021+4026 AND THE Γ-Cygni SUPERNOVA REMNANT

Hui

Seo

Lin

et al. 2015

ApJ

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We have investigated the field around the radio-quiet γ-ray pulsar, PSR J2021+4026, with a ∼ 140 ks XMM-Newton observation and a ∼ 56 ks archival Chandra data. Through analyzing the pulsed spectrum, we show that the X-ray pulsation is purely thermal in nature which suggests the pulsation is originated from a hot polar cap with T ∼ 3 × 10 6 K on the surface of a rotating neutron star. On the other hand, the power-law component that dominates the pulsar emission in the hard band is originated from off-pulse phases, which possibly comes from a pulsar wind nebula. In re-analyzing the Chandra data, we have confirmed the presence of bow-shock nebula which extends from the pulsar to west by ∼ 10 arcsec. The orientation of this nebular feature suggests that the pulsar is probably moving eastward which is consistent with the speculated proper motion by extrapolating from the nominal geometrical center of the supernova remnant (SNR) G78.2+2.1 to the current pulsar position. For G78.2+2.1, our deep XMM-Newton observation also enables a study of the central region and part of the southeastern region with superior photon statistics. The column absorption derived for the SNR is comparable with that for PSR J2021+4026, which supports their association. The remnant emission in both examined regions are in an non-equilibrium ionization state. Also, the elapsed time of both regions after shock-heating is apparently shorter than the Sedov age of G78.2+2.1. This might suggest the reverse shock has reached the center not long ago. Apart from PSR J2021+4026 and G78.2+2.1, we have also serendipitously detected an X-ray flash-like event XMM J202154.7+402855 from this XMM-Newton observation.

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“…mass shedding, which sets an absolute limit on rapid rotation) are in place, carrying out a 2D study of the thermal evolution of such objects is a challenging task. First steps toward this direction were made in [25,[32][33][34][35]. We note that the 2D cooling of magnetized neutron stars has been previously studied in [35,36], where the 2D effects of the magnetic field in the crust were investigated, and first steps towards a consistent magneto-thermal evolution simulation were taken.…”

Section: D Thermal Evolutionmentioning

confidence: 99%

Thermal evolution of neutron stars in two dimensions

2012

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There are many factors that contribute to the breaking of the spherical symmetry of a neutron star. Most notably is rotation, magnetic fields, and/or accretion of matter from companion stars. All these phenomena influence the macroscopic structures of neutron stars, but also impact their microscopic compositions. The purpose of this paper is to investigate the cooling of rotationally deformed, two-dimensional (2D) neutron stars in the framework of general relativity theory, with the ultimate goal of better understand the impact of 2D effects on the thermal evolution of such objects. The equations that govern the thermal evolution of rotating neutron stars are presented in this paper. The cooling of neutron stars with different frequencies is computed self-consistently by combining a fully general relativistic 2D rotation code with a general relativistic 2D cooling code. We show that rotation can significantly influence the thermal evolution of rotating neutron stars. Among the major new aspects are the appearances of hot spots on the poles, and an increase of the thermal coupling times between the core and the crust of rotating neutron stars. We show that this increase is independent of the microscopic properties of the stellar core, but depends only on the frequency of the star.

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The Effects of Rotation on Thermal X‐Ray Afterglows Resulting from Pulsar Glitches

Cited by 10 publications

References 36 publications

Discovery of X-Ray Pulsation From the Geminga-Like Pulsar PSR J2021+4026

Discovery of X-Ray Pulsation From the Geminga-Like Pulsar PSR J2021+4026

A DETAILED X-Ray INVESTIGATION OF PSR J2021+4026 AND THE Γ-Cygni SUPERNOVA REMNANT

Thermal evolution of neutron stars in two dimensions

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