OSSE observations of the Crab pulsar

Ulmer, M. P.; Lomatch, S.; Matz, S. M.; Grabelsky, D. A.; Purcell, W. R.; Grove, J. E.; Johnson, W. N.; Kinzer, R. L.; Kurfess, J. D.; Strickman, M. S.; Cameron, R. A.; Jung, G. V.

doi:10.1086/174564

Cited by 33 publications

(30 citation statements)

References 28 publications

(55 reference statements)

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“…In addition, the pulsed spectral index was found to be consistent with a constant value throughout the pulse, at odds with the behavior seen in hard X-rays from the Crab, another young, isolated pulsar (Ulmer et al 1994). …”

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confidence: 70%

The X-Ray Spectrum of the Plerionic System PSR B1509−58/MSH 15−52

Marsden

Blanco

Gruber

et al. 1997

The Astrophysical Journal

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We present the results of observations of the PSR B1509Ϫ58/MSH 15Ϫ52 system in X-rays (2-250 keV) by the Rossi X-Ray Timing Explorer. The spectra of the peak of the pulsed component (radio phase 0.17-0.53) is fitted by a power law of photon index , with no evidence of a high-energy spectral break seen up 1.36 ‫ע‬ 0.01 to ∼200 keV. For the off-pulse spectral component, the spectrum from 2-250 keV is fitted by a power law of photon index . An iron emission line at 6.7 keV with an equivalent width of 129 eV improves 2.215 ‫ע‬ 0.005 the fit, but only at a marginal significance. Thermal bremsstrahlung and Raymond-Smith models produce much worse fits to the unpulsed data. The lack of a high-energy spectral break in the pulsed emission implies an efficiency of ≥3% in the conversion of pulsar spin-down energy to pulsed X-rays in the system. Subject headings: ISM: individual (MSH 15Ϫ52) -pulsar: individual (PSR B1509Ϫ58) -stars: neutron

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confidence: 70%

The X-Ray Spectrum of the Plerionic System PSR B1509−58/MSH 15−52

Marsden

Blanco

Gruber

et al. 1997

The Astrophysical Journal

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“…Therefore, we extended our energy window by analysing consistently not only the CGRO EGRET (30 MeV-10 GeV) high-energy γ-ray data, but also Xray/soft γ-ray data from the ROSAT HRI (0.1-2.4 keV), BeppoSAX LECS (0.1-10 keV), MECS (1.6-10 keV) and PDS (15-300 keV), and CGRO BATSE (20 keV-1 MeV). The (on board folded) data from CGRO BATSE overlap in energy with the data from CGRO OSSE for which results have already been published by Ulmer et al (1994Ulmer et al ( , 1995. However, due to the enormous exposure in the coadded BATSE data the statistics are much better than can be obtained in the combined OSSE Crab observations.…”

Section: Pulse Profiles Of Psr B0531+21 From 01 Kev Up To 10 Gevmentioning

confidence: 94%

“…9 our derived Total Pulse Crab EGRET spectrum (30 MeV-10 GeV, Cycle 0-IV) and the published Total Pulse spectra from GRIS (20 keV-1 MeV: Bartlett 1994a) and OSSE (50 keV-0.59 MeV: Ulmer et al 1994). In the latter two publications slightly different phase intervals have been used to derive the Total Pulse spectrum.…”

Section: Crab Total Pulse Spectrummentioning

confidence: 97%

“…Toor & Seward 1977;Hasinger 1984Hasinger , 1985Ulmer et al 1994;Mineo et al 1997;Massaro et al 1998Massaro et al , 2000, generally over more restricted energy windows with poorer data coverage, and/or often using data of inferior statistical quality. Particularly the "transition" region of the COMPTEL MeV window is now well covered for the first time.…”

Section: P2/p1 and Bridge/p1 Ratios As A Function Of Energymentioning

confidence: 99%

“…The results based on data from an early set of observations performed during the first-year all-sky survey of the CGRO mission had been published by Much et al (1995) and Carramiñana et al (1994). Ulmer et al (1994) presented the first findings from the Oriented Scintillation Spectrometer Experiment OSSE (50 keV-10 MeV), and in a CGRO-paper (Ulmer et al 1995) the first results from OSSE, COMPTEL and EGRET were combined. It was shown that the overall pulse phase-averaged spectrum is not well fitted by a single power-law, better with a broken power-law.…”

Section: Introductionmentioning

confidence: 99%

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The Crab pulsar in the 0.75-30 MeV range as seen by CGRO COMPTEL

Kuiper

Hermsen

Cusumano

et al. 2001

A&A

249

280

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Abstract. We present the time-averaged characteristics of the Crab pulsar in the 0.75-30 MeV energy window using data from the imaging Compton Telescope COMPTEL aboard the Compton Gamma-Ray Observatory (CGRO) collected over its 9 year mission. Exploiting the exceptionally long COMPTEL exposure on the Crab allowed us to derive significantly improved COMPTEL spectra for the Crab nebula and pulsar emissions, and for the first time to accurately determine at low-energy γ-rays the pulse profile as a function of energy. These timing data, showing the well-known main pulse and second pulse at a phase separation of ∼0.4 with strong bridge emission, are studied together with data obtained at soft/hard X-ray energies from the ROSAT HRI, BeppoSAX LECS, MECS and PDS, at soft γ-rays from CGRO BATSE and at high-energy γ-rays from CGRO EGRET in order to obtain a coherent high-energy picture of the Crab pulsar from 0.1 keV up to 10 GeV. The morphology of the pulse profile of the Crab pulsar is continuously changing as a function of energy: the intensities of both the second pulse and the bridge emission increase relative to that of the first pulse for increasing energies up to ∼1 MeV. Over the COMPTEL energy range above 1 MeV an abrupt morphology change happens: the first pulse becomes again dominant over the second pulse and the bridge emission loses significance such that the pulse profile above 30 MeV is similar to the one observed at optical wavelengths. A pulse-phase-resolved spectral analysis performed in 7 narrow phase slices consistently applied over the 0.1 keV-10 GeV energy interval shows that the pulsed emission can empirically be described with 3 distinct spectral components: i) a power-law emission component (1 keV-5 GeV; photon index 2.022 ± 0.014), present in the phase intervals of the two pulses; ii) a curved spectral component required to describe soft ( < ∼ 100 keV) excess emission present in the same pulsephase intervals; iii) a broad curved spectral component reflecting the bridge emission from 0.1 keV to ∼10 MeV. This broad spectral component extends in phase over the full pulse profile in an approximately triangular shape, peaking under the second pulse. Recent model calculations for a three-dimensional pulsar magnetosphere with outer magnetospheric gap acceleration by Cheng et al. (2000) appear at present most successful in explaining the above complex high-energy characteristics of the Crab pulsar.

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What Pulsar High-Energy Emission Model Survives?

Hirotani

2010

High-Energy Emission From Pulsars and Their Systems

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OSSE observations of the Crab pulsar

Cited by 33 publications

References 28 publications

The X-Ray Spectrum of the Plerionic System PSR B1509−58/MSH 15−52

The X-Ray Spectrum of the Plerionic System PSR B1509−58/MSH 15−52

The Crab pulsar in the 0.75-30 MeV range as seen by CGRO COMPTEL

What Pulsar High-Energy Emission Model Survives?

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