Thermal Response of a Neutron Star to a Glitch

Hirano, Shiro; Shibazaki, N.; Umeda, Hideyuki; Nomoto, Ken’ichi

doi:10.1086/304946

Cited by 22 publications

(35 citation statements)

References 29 publications

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“…45 erg (Hirano et al 1997). This is comparable to the observed energy release in giant SGR flares (Hurley et al 2005).…”

Section: Possible Event In the Gap?supporting

confidence: 79%

“…45 erg (Hirano et al 1997). Such a thermal energy release could be influencing the pulse profile as well, although some change in profile would be expected in the hard band too, which is not observed.…”

Section: Possible Physical Interpretations For 4u 0142+61mentioning

confidence: 92%

“…If the event associated with the putative glitch released energy deep in the neutron-star crust, then the increase could be due to its slow release (eg. Eichler & Cheng 1989;Hirano et al 1997). Given the size of the observed flux increase and its timescale for release, the initial energy deposition would have had to have been large, ∼10…”

Section: Possible Event In the Gap?mentioning

confidence: 99%

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10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Dib

Kaspi

Gavriil

2007

Astrophys Space Sci

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“…45 erg (Hirano et al 1997). This is comparable to the observed energy release in giant SGR flares (Hurley et al 2005).…”

Section: Possible Event In the Gap?supporting

confidence: 79%

Section: Possible Physical Interpretations For 4u 0142+61mentioning

confidence: 92%

Section: Possible Event In the Gap?mentioning

confidence: 99%

See 1 more Smart Citation

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Dib

Kaspi

Gavriil

2007

Astrophys Space Sci

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“…Originally proposed for post-glitch afterglows of ordinary neutron stars (Eichler & Cheng 1989;Hirano et al 1997), this idea is recently investigated in the magnetar context (Lyubarsky et al 2002) and applied to X-ray observations of transient sources Scholz et al 2012). …”

Section: Speculative Relation To Seismologymentioning

confidence: 99%

Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Enoto¹,

Shibata²,

Kitaguchi³

et al. 2017

ApJS

116

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Studies were made of the 1-70 keV persistent spectra of fifteen magnetars as a complete sample observed with Suzaku from 2006 to 2013. Combined with early NuSTAR observations of four hard X-ray emitters, nine objects showed a hard power-law emission dominating at 10 keV with the 15-60 keV flux of ∼1-11 × 10 −11 ergs s −1 cm −2 . The hard X-ray luminosity L h , relative to that of a soft-thermal surface radiation L s , tends to become higher toward younger and strongly magnetized objects. Updated from the previous study, their hardness ratio, defined as ξ = L h /L s , is correlated with the measured spin-down rateṖ as ξ = 0.62 × (Ṗ /10 −11 s s −1 ) 0.72 , corresponding with positive and negative correlations of the dipole field strength B d (ξ ∝ B d) and the characteristic age τ c (ξ ∝ τ −0.68 c ), respectively. Among our sample, five transients were observed during X-ray outbursts, and the results are compared with their long-term 1-10 keV flux decays monitored with Swift/XRT and RXTE/PCA. Fading curves of three bright outbursts are approximated by an empirical formula used in the seismology, showing a ∼10-40 d plateau phase. Transients show the maximum luminosities of L s ∼1035 erg s −1 , which is comparable to those of the persistently bright ones, and fade back to 10 32 erg s −1 . Spectral properties are discussed in a framework of the magnetar hypothesis.

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“…Seward et al (2000) provide a concise introduction to the published models for the thermal response of the stellar surface to a glitch generated by the sudden unpinning of superÑuid vortex lines deep in the star (van Riper, Epstein, & Miller 1991 ;Chong & Cheng 1994 ;Hirano et al 1997 ;Cheng, Li, & Suen 1998), and we need not repeat it here. We follow their approach in deriving parameter limits from the models.…”

Section: T Hermal Emission Constraints On the Neutronmentioning

confidence: 99%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

289

305

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We present high-resolution Chandra X-ray observations of PSR B0833[45, the 89 ms pulsar associated with the Vela supernova remnant. We have acquired two observations separated by 1 month to search for changes in the pulsar and its environment following an extreme glitch in its rotation frequency. We Ðnd a well-resolved nebula with a toroidal morphology remarkably similar to that observed in the Crab Nebula, along with an axial Crab-like jet. Between the two observations, taken D3 ] 105 s and D3 ] 106 s after the glitch, the Ñux from the pulsar is found to be steady to within 0.75% ; the 3 p limit on the fractional increase in the pulsarÏs X-ray Ñux is of the inferred glitch energy. We use [10~5 this limit to constrain parameters of glitch models and neutron star structure. We do Ðnd a signiÐcant increase in the Ñux of the nebulaÏs outer arc ; if associated with the glitch, the inferred propagation velocity is similar to that seen in the brightening of the Crab Nebula wisps. We propose an explana-Z0.7c, tion for the X-ray structure of the Vela synchrotron nebula based on a model originally developed for the Crab Nebula. In this model, the bright X-ray arcs are the shocked termination of a relativistic equatorial pulsar wind that is contained within the surrounding kidney-bean shaped synchrotron nebula comprising the postshock, but still relativistic, Ñow. In a departure from the Crab model, the magnetization parameter p of the Vela pulsar wind is allowed to be of order unity ; this is consistent with the simplest MHD transport of magnetic Ðeld from the pulsar to the nebula, where B ¹ 4 ] 10~4 G. The inclination angle of the axis of the equatorial torus with respect to the line of sight is identical to that of the rotation axis of the pulsar as previously measured from the polarization of the radio pulse. The projection of the rotation axis on the sky may also be close to the direction of proper motion of the pulsar if previous radio measurements were confused by orthogonal-mode polarized components. We review e †ects that may enhance the probability of alignment between the spin axis and space velocity of a pulsar, and speculate that short-period, slowly moving pulsars are just the ones best-suited to producing synchrotron nebulae with such aligned structures. Previous interpretations of the compact Vela nebula as a bow-shock in a very weakly magnetized wind su †ered from data of inadequate spatial resolution and less plausible physical assumptions.

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Thermal Response of a Neutron Star to a Glitch

Cited by 22 publications

References 29 publications

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Magnetar Broadband X-Ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE

Vela Pulsar and Its Synchrotron Nebula

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