Observation of the Crab pulsar, PSR 0531 + 21, at 0.2-6.0 MeV with the FIGARO II experiment

Sacco, B.; Gerardi, G.; Mineo, T.; Scarsi, L.; Agrinier, B.; Barouch, Eytan; Masnou, J. L.; Parlier, B.; Costa, E.; Massaro, E.; Salvati, M.; Niel, M.; Mandrou, P.; Hote, C.; McCulloch, P. M.

doi:10.1086/168797

Cited by 18 publications

(12 citation statements)

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“…The 1 -10 MeV Crab light curve integrated over the 4 observations is shown in fig. 2 (left); as expected from measurements in similar energy ranges (see for example Agrinier et al, 1990), the shape of the pulsed emission is characterized by two main peaks at about 0.4 phase distance with an important bridge of emission between them. It is important to notice that this bridge is marginal above 50 MeV .…”

Section: The Crab Pulsarsupporting

confidence: 77%

Pulsar studies with GRO-COMPTEL

Buccheri

Bennett

Busetta

et al. 1993

Advances in Space Research

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Section: The Crab Pulsarsupporting

confidence: 77%

Pulsar studies with GRO-COMPTEL

Buccheri

Bennett

Busetta

et al. 1993

Advances in Space Research

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“…From these two gures we see that in the lower energy range, the spectrum of the interpulse region phase bins 20 to 29 is atter than the spectra of the pulse peaks phase bins 14 to 19 and 35 to 41. This is in basic agreement with Knight 1982, Mahoney et al 1984, and Agrinier et al 1990. We have produced several preliminary spectra, but it is too early to report a detailed spectral comparison between the di erent regions.…”

Section: Preliminary Resultssupporting

confidence: 90%

“…We cannot conclusively exclude the existence of the 440 keV line in the spectrum of the second peak reported by the FIGARO group Agrinier et al 1990, Massaro et al 1991 photons cm ,2 s ,1 . The FIGARO result is based on combining data from balloon ights made on 11 July 1986 and 9 July 1990.…”

Section: Preliminary Resultsmentioning

confidence: 67%

OSSE Observations of the Crab Pulsar

Ulmer

Lomatch²,

Matz³

et al. 1991

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We present preliminary results of the Compton Gamma Ray Observatory OSSE observations of the Crab pulsar. The pulsar energy spectra and light curves are in general agreement with previous observations, validating the OSSE pulsar data acquisition modes and data analysis algorithms. The data suggest that the spectrum of the pulsar varies throughout the light curve. The interpulse" region has a slightly atter spectrum in the 60 250 keV region and a slightly steeper spectrum at higher energies than the two main pulses. We nd no evidence for any lines in the spectra with a typical sensitivity of about 10 ,4 photons cm ,2 s ,1 .

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“…11. We also added some data points obtained from the FIGARO II experiment (Agrinier et al 1990;Massaro et al 1998) to fill the gap between 300 keV and 1 MeV.…”

Section: Extension Of the Two-component Model At Higher Energies: Thementioning

confidence: 99%

The optical toγ-ray emission of the Crab pulsar: a multicomponent model

Massaro¹,

Campana²,

Cusumano³

et al. 2006

A&A

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We present a multicomponent model to explain the features of the pulsed emission and spectrum of the Crab Pulsar, on the basis of X and γ-ray observations obtained with BeppoSAX, INTEGRAL and CGRO. This model explains the evolution of the pulse shape and of the phase-resolved spectra, ranging from the optical/UV to the GeV energy band, on the assumption that the observed emission is due to more components. The first component, C O , is assumed to have the pulsed double-peaked profile observed at the optical frequencies, while the second component, C X , is dominant in the interpeak and second peak phase regions. The spectra of these components are modelled with log-parabolic laws and their spectral energy distributions have peak energies at 12.2 and 178 keV, respectively. To explain the properties of the pulsed emission in the MeV-GeV band, we introduce two more components, C Oγ and C Xγ , with phase distributions similar to those of C O and C X and log-parabolic spectra with the same curvature but peak energies at about 300 MeV and 2 GeV. This multicomponent model is able to reproduce both the broadband phase-resolved spectral behaviour and the changes of the pulse shape with energy. We also propose some possible physical interpretations in which C O and C X are emitted by secondary pairs via a synchrotron mechanism while C Oγ and C Xγ can originate either from Compton scattered or primary curvature photons.

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Observation of the Crab pulsar, PSR 0531 + 21, at 0.2-6.0 MeV with the FIGARO II experiment

Cited by 18 publications

References 0 publications

Pulsar studies with GRO-COMPTEL

Pulsar studies with GRO-COMPTEL

OSSE Observations of the Crab Pulsar

The optical toγ-ray emission of the Crab pulsar: a multicomponent model

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