The optical to<i>γ</i>-ray emission of the Crab pulsar: a multicomponent model

Massaro, E.; Campana, R.; Cusumano, G.; Mineo, T.

doi:10.1051/0004-6361:20065118

Cited by 29 publications

(33 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…At lower (seed photon) energies, dependencies of the pulse peak positions have previously been studied in detail in the literature (Mineo et al 1997;Massaro et al 2006Massaro et al , 2000, particularly throughout the strong X-ray signal regime. These studies find constancy of the peak positions of both P1 and P2 throughout more than three orders of magnitude, albeit the pulse widths and shapes do change throughout the X-ray domain.…”

Section: Systematic Uncertaintiesmentioning

confidence: 99%

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

Ahnen¹,

Ansoldi²,

Antonelli³

et al. 2017

ApJS

View full text Add to dashboard Cite

Spontaneous breaking of Lorentz symmetry at energies on the order of the Planck energy or lower is predicted by many quantum gravity theories, implying non-trivial dispersion relations for the photon in vacuum. Consequently, gamma-rays of different energies, emitted simultaneously from astrophysical sources, could accumulate measurable differences in their time of flight until they reach the Earth. Such tests have been carried out in the past using fast variations of gamma-ray flux from pulsars, and more recently from active galactic nuclei and gamma-ray bursts. We present new constraints studying the gamma-ray emission of the galactic Crab Pulsar, recently observed up to TeV energies by the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) collaboration. A profile likelihood analysis of pulsar events reconstructed for energies above 400GeV finds no significant variation in arrival time as their energy increases.Ninety-five percent CL limits are obtained on the ) for a quadratic scenario, for the subluminal and the superluminal cases, respectively. A substantial part of this study is dedicated to calibration of the test statistic, with respect to bias and coverage properties. Moreover, the limits take into account systematic uncertainties, which are found to worsen the statistical limits by about 36%-42%. Our constraints would have been much more stringent if the intrinsic pulse shape of the pulsar between 200GeV and 400GeV was understood in sufficient detail and allowed inclusion of events well below 400GeV.

show abstract

Section: Systematic Uncertaintiesmentioning

confidence: 99%

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

Ahnen¹,

Ansoldi²,

Antonelli³

et al. 2017

ApJS

View full text Add to dashboard Cite

show abstract

“…In this case γγ-absorption requires the presence of soft photons in the X-ray regime with s = 0.5 (1 GeV/ ) keV or larger. In the case of, e.g., the Crab pulsar, the X-ray luminosity is of order L x ∼ 10 36 erg/s (Kuiper et al 2001;Possenti et al 2002;Massaro et al 2006), so that the optical depth becomes…”

Section: Pair Creation and γγ-Absorptionmentioning

confidence: 99%

On particle acceleration and very high energy γ-ray emission in Crab-like pulsars

Osmanov

Rieger

2009

A&A

View full text Add to dashboard Cite

Context. The origin of very energetic charged particles and the production of very high-energy (VHE) gamma-ray emission remains still a challenging issue in modern pulsar physics. Aims. By applying a toy model, we explore the acceleration of co-rotating charged particles close to the light surface in a plasma-rich pulsar magnetosphere and study their interactions with magnetic and photon fields under conditions appropriate for Crab-type pulsars. Methods. Centrifugal acceleration of particles in a monopol-like magnetic field geometry is analyzed and the efficiency constraints, imposed by corotation, inverse Compton interactions and curvature radiation reaction are determined. We derive expressions for the maximum particle energy and provide estimates for the corresponding high-energy curvature and inverse Compton power outputs. Results. It is shown that for Crab-like pulsars, electron Lorentz factor up to γ ∼ 10 7 can be achieved, allowing inverse Compton (Klein-Nishina) up-scattering of thermal photons to TeV energies with a maximum luminosity output of ∼10 31 erg/s. Curvature radiation, on the other hand, will result in a strong GeV emission output of up to ∼(10 34 −10 35 ) erg/s, quasi-exponentially decreasing towards higher energies for photon energies below ∼50 GeV. Conclusions. Accordingly to the results presented only young pulsars are expected to be sites of detectable VHE γ-ray emission.

show abstract

“…Massaro et al (2006) developed a phenomenological model of the Crab Pulsar X and γ‐ray emission, explained as due to two different emission components C O and C X , having a log‐parabolic spectrum with the same curvature ( b ≃ 0.16) but different energy peaks and phase distributions. This multicomponent (MC) model also describes the energy variations of the pulse profile.…”

Section: The X‐ray Spectra Of the Pulsar And The Pwnmentioning

confidence: 99%

“…The distance values used are d = 50 and 2 kpc, respectively. Crab data are from the four NFI (Narrow Field Instruments) onboard BeppoSAX and were taken from Massaro et al (2006). Also plotted are the log‐parabolic model for PSR B0540‐69 (blue dashed line) and the total multicomponent model for Crab (black continuous line, with the C O and C X components as orange dash–dotted line and violet dash–dot–dotted line) (see text for discussion).…”

Section: The X‐ray Spectra Of the Pulsar And The Pwnmentioning

confidence: 99%

X-ray observations of the Large Magellanic Cloud pulsar PSR B0540-69 and its pulsar wind nebula

Campana

Mineo

Rosa

et al. 2008

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

PSR B0540-69 is a young pulsar in the Large Magellanic Cloud that has similar properties with respect to the Crab Pulsar, and is embedded in a pulsar wind nebula (PWN). We have analysed the complete archival Rossi X-Ray Timing Explorer (RXTE) data set of observations of this source, together with new Swift/XRT (X-Ray Telescope) and International Gamma-Ray Astrophysics Laboratory (INTEGRAL)/IBIS (Imager on Board INTEGRAL Satellite) data. Accurate light curves are produced in various energy bands between 2 and 60 keV, showing no significant energy variations of the pulse shape. The spectral analysis shows that the pulsed spectrum is curved, and is best fitted up to 100 keV by a log-parabolic model: this strengthens the similarities with the Crab Pulsar, and is discussed in the light of a phenomenologic multicomponent model. The total emission from this source is studied, the relative contributions of the pulsar and the PWN emission are derived and discussed in the context of other INTEGRAL-detected pulsar/PWN systems

show abstract

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

Cited by 29 publications

References 50 publications

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

On particle acceleration and very high energy γ-ray emission in Crab-like pulsars

X-ray observations of the Large Magellanic Cloud pulsar PSR B0540-69 and its pulsar wind nebula

Contact Info

Product

Resources

About