The phase-resolved high energy spectrum of the crab pulsar

Jia, J. J.; Tang, Anisia P. S.; Takata, Jumpei; Chang, Hsiang-Kuang; Cheng, K. S.

doi:10.1016/j.asr.2007.02.076

Cited by 8 publications

(9 citation statements)

References 32 publications

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“…We are interested in finding a general scenario that can produce both the -ray and the X-ray regimes in the phase-resolved spectra of the Crab pulsar. Our preliminary results were reported at the 2006 COSPAR conference (Jia et al 2007). We have since continued to study these spectra in more detail.…”

Section: Introductionmentioning

confidence: 82%

A Revisit of the Phase‐resolved X‐Ray and Gamma‐Ray Spectra of the Crab Pulsar

Tang

Takata

Jia

et al. 2008

ApJ

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We use a modified outer-gap model to study the multifrequency phase-resolved spectra of the Crab pulsar. The emissions from both poles contribute to the light curve and the phase-resolved spectra. Using the synchrotron selfCompton mechanism and by considering the incomplete conversion of curvature photons into secondary pairs, the observed phase-averaged spectrum from 100 eV to 10 GeV can be explained very well. The predicted phase-resolved spectra can match the observed data reasonably well, too. We find that the emission from the north pole mainly contributes to leading wing 1. The emissions in the remaining phases are mainly dominated by the south pole. The widening of the azimuthal extension of the outer gap explains trailing wing 2. The complicated phase-resolved spectra for the phases between the two peaks, namely, trailing wing 1, the bridge, and leading wing 2, strongly suggest that there are at least two well-separated emission regions with multiple emission mechanisms-synchrotron radiation, inverse Compton scattering, and curvature radiation. Our best-fit results indicate that there may exist some asymmetry between the south and north poles. Our model predictions can be examined with GLAST.

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Section: Introductionmentioning

confidence: 82%

A Revisit of the Phase‐resolved X‐Ray and Gamma‐Ray Spectra of the Crab Pulsar

Tang

Takata

Jia

et al. 2008

ApJ

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“…The X-ray pulse of the Crab pulsar is composed of two peaks and inter peak region and changes significantly with energy. Jia et al (2007) have calculated the light curves of the Crab pulsar with assumption that inner boundary is extended inward from the null charge surface to 10 stellar radii(Fig. 2).…”

Section: Comparison Of the Pulse Profiles With Model Predictionsmentioning

confidence: 99%

“…Hirotani, Harding & Shibata (2003) pointed out that the large current in the outer gap can change the boundary of the outer gap (Hirotani & Shibata 2001;Hirotani, Harding & Shibata 2003). The modified outer-gap model could well predict the double peak profile and fit the phase-resolved X-ray spectra of the Crab pulsar using the synchrotron self-Compton mechanism (Jia et al 2007;Tang et al 2008). calculated the optical, X-ray and gamma-ray light curves and spectra of PSRs B0540-69 and B1509-58 using the CRZ model.…”

Section: Introductionmentioning

confidence: 99%

X-RAY PHASE-RESOLVED SPECTROSCOPY OF PSRs B0531+21, B1509–58, AND B0540–69 WITH RXTE

Ge¹,

Lu²,

Qu³

et al. 2012

ApJS

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The Rossi X-ray Timing Explorer (RXTE) has made hundreds of observations on three famous young pulsars (PSRs) B0531+21 (Crab), B1509-58, and B0540-69. Using the archive RXTE data, we have studied the phase-resolved spectral properties of these pulsars in details. The variation of the X-ray spectrum with phase of PSR B0531+21 is confirmed here much more precisely and more details are revealed than the previous studies: the spectrum softens from the beginning of the first pulse, turns to harden right at the pulse peak and becomes the hardest at the bottom of the bridge, softens gradually until the second peak, and then softens rapidly. Different from the previous studies, we found that the spectrum of PSR B1509-58 is significantly harder in the center of the pulse, which is also in contrast to that of PSR B0531+21. The variation of the X-ray spectrum of PSR B0540-69 seems similar to that of PSR B1509-58, but with a lower significance. Using the about 10 years of data span, we also studied the real time evolution of the spectra of these pulsars, and no significant evolution has been detected. We have discussed about the constraints of these results on theoretical models of pulsar X-ray emission.RXTE has made hundreds of observations on the three young pulsars that we studied, which were listed in Table. 3. The total exposure time of PSRs B0531+21, B1509-58, and B0540-69 is 172, 578, and 2,663 ks, respectively ( Table. 3), and with such plenty of data we can perform detailed phase-resolved spectroscopic study. The Event mode data were selected for our analyses, so as to have good time resolution and enough spectral channels.Heasoft (v6.10) was used to process the observational data as follows: (1) Create the filter file for each observation with XTEFILT; (2) generate the Good Time Interval (GTI) file by MAKETIME using the filter file; (3) using the GTI file to create the "good" events file with GROSSTIMEFILT; and (4) remove the clock events from the event mode data by SEFITER and FSELECT. The resulted new events data will be used in the timing and

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“…The theoretical models for radiation from high-energy pulsars (e.g., Crab and Vela) require the radiation engine to be located in the open field line region in the polar gap model ( Harding 1981;Daugherty & Harding 1996), the outer gap model (Cheng et al 1986;Chiang & Romani 1994;Romani & Yadigaroglu 1995;Cheng et al 2000), and the modified outer gap model (Dyks & Rudak 2003;Jia et al 2007). However, we cannot apply these models to magnetars to explain their persistent X-ray emissions.…”

Section: Why Closed Regions?mentioning

confidence: 99%

A Morphological Approach to the Pulsed Emission from Soft Gamma Repeaters

Jia¹,

Huang²,

Cheng³

2008

ApJ

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We present a geometrical methodology to interpret the periodical light curves of soft gamma repeaters based on the magnetar model and the numerical arithmetic of the three-dimensional magnetosphere model for the young pulsars. The hot plasma released by the starquake is trapped in the magnetosphere, and photons are emitted tangentially to the local magnetic field lines. The variety of radiation morphologies in the burst tails and the persistent stages could be well explained by the trapped fireballs on different sites inside the closed field lines. Furthermore, our numerical results suggest that the pulse profile evolution of SGR 1806À20 during the 2004 December 27 giant flare is due to a lateral drift of the emitting region in the magnetosphere.

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The phase-resolved high energy spectrum of the crab pulsar

Cited by 8 publications

References 32 publications

A Revisit of the Phase‐resolved X‐Ray and Gamma‐Ray Spectra of the Crab Pulsar

A Revisit of the Phase‐resolved X‐Ray and Gamma‐Ray Spectra of the Crab Pulsar

X-RAY PHASE-RESOLVED SPECTROSCOPY OF PSRs B0531+21, B1509–58, AND B0540–69 WITH RXTE

A Morphological Approach to the Pulsed Emission from Soft Gamma Repeaters

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