An ATLAS FOR INTERPRETING Γ-Ray PULSAR LIGHT CURVES

Watters, K.; Romani, Roger W.; Weltevrede, P.; Johnston, S.

doi:10.1088/0004-637x/695/2/1289

Cited by 220 publications

(336 citation statements)

References 27 publications

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“…This result is in broad agreement with the value estimated by scaling the γ-ray flux of the pulsar (Saz Parkinson (Watters et al 2009). By applying this relation, we have a γ-ray efficiency of 0.04, an X-ray efficiency of 3×10 −4 ,and a distance of 600 pc.…”

Section: The Nebulaesupporting

confidence: 91%

The Tale of the Two Tails of the Oldish PSR J2055+2539

Marelli

Pizzocaro

Luca

et al. 2016

ApJ

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We analyzed a deep XMM-Newton observation of the radio-quiet γ-ray PSR J2055+2539. The spectrum of the X-ray counterpart is nonthermal, with a photon index of Γ=2.36±0.14 (1σ confidence). We detected X-ray pulsations with a pulsed fraction of 25% ± 3% and a sinusoidal shape. Taking into account considerations on the γ-ray efficiency of the pulsar and on its X-ray spectrum, we can infer a pulsar distance ranging from 450 to 750 pc. We found two different nebular features associated withPSR J2055+2539 and protruding from it. The angle between the two nebular main axes is ∼162°.8±0°.7. The main, brighter feature is 12′ long and <20″ thick, characterized by an asymmetry with respect to the main axis that evolves with the distance from the pulsar, possibly forming a helical pattern. The secondary feature is 250″×30″. Both nebulae present an almost flat brightness profile with a sudden decrease at the end. The nebulae can be fitted byeithera power-law model or a thermal bremsstrahlung model. A plausible interpretation of the brighter nebula is in terms of a collimated ballistic jet. The secondary nebula is most likely a classical synchrotron-emitting tail.

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Section: The Nebulaesupporting

confidence: 91%

The Tale of the Two Tails of the Oldish PSR J2055+2539

Marelli

Pizzocaro

Luca

et al. 2016

ApJ

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“…Model fits to the observed light curves show that the current sample encompasses a large variety of stellar configurations (αB magnetic obliquity and ζ obs viewing angle, see Figure 2), with low |αB − ζ obs | values when we intercept both the radio and γ-ray beams, and large |αB − ζ obs | values when we intercept only the wide γ-ray beam [54,64,57]. A useful anti-correlation has been found between the phase separation between the two γ-ray peaks (∆) and the phase separation between the radio and first γ-ray peak (alias radio lag δ).…”

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confidence: 93%

Gamma-ray pulsars: A gold mine

Grenier

Harding

2015

Comptes Rendus. Physique

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The most energetic neutron stars, powered by their rotation, are capable of producing pulsed radiation from the radio up to γ rays with nearly TeV energies. These pulsars are part of the universe of energetic and powerful particle accelerators, using their uniquely fast rotation and formidable magnetic fields to accelerate particles to ultra-relativistic speed. The extreme properties of these stars provide an excellent testing ground, beyond Earth experience, for nuclear, gravitational, and quantum-electrodynamical physics. A wealth of γ-ray pulsars has recently been discovered with the Fermi Gamma-Ray Space Telescope. The energetic γ rays enable us to probe the magnetospheres of neutron stars and particle acceleration in this exotic environment. We review the latest developments in this field, beginning with a brief overview of the properties and mysteries of rotation-powered pulsars, and then discussing γ-ray observations and magnetospheric models in more detail. RésuméLes pulsars γ : une mine d'or : Lesétoilesà neutrons les plus puissantes, qui tirent leurénergie de leur rotation, sont capables d'émettre des impulsions lumineuses des ondes radio jusqu'aux rayons γ d'énergies proches du TeV. Ces pulsars font partie des puissants accélérateurs de particules de l'Univers, profitant de leur rotation unique et de leur formidable champ magnétique pour accélérer des particules jusqu'à des vitesses ultra-relativistes. Les propriétés extrêmes de cesétoiles permettent de tester la physique nucléaire, la gravitation et l'électrodynamique quantique dans des conditions inaccessibles sur Terre. Le télescope gamma spatial Fermi vient de révéler un richeéchantillon de pulsars γ. Leur rayonnement γénergétique permet de sonder la magnétosphère desétoilesà neutrons et d'étudier l'accélération de particules dans cet environnement exotique. Nous présentons les derniers développements de ce domaine, en commençant par une rapide revue des propriétés et mystères soulevés par ces pulsars, puis en détaillant plus avant les observations γ et les modèles magnétosphériques.Keywords : pulsar ; neutron star ; magnetosphere ; gamma rays ; acceleration Mots-clés : pulsar ;étoileà neutrons ; magnétosphère ; rayons gamma ; accélération Neutron stars, pulsars, and their puzzlesA neutron star is an extreme object in many regards. It is a compact, rapidly spinning, highly magnetized star, formed from the core of a massive star which runs out of nuclear power and collapses under its own gravity, with 53 radio-loud and γ-loud young pulsars (orange upward triangles), 37 radio-faint and γ-loud young pulsars (red downward triangles), 71 radio-loud and γ-loud millisecond pulsars (green filled circles, circled in black and red when in black-widow and redback systems, respectively), and 2256 other radio pulsars (light blue). Recently discovered millisecond pulsars, with noṖ measurement yet, are plotted as squares atṖ near 10 −21 . Lines of constant spin-down power (brown) and polar magnetic field strength (green) are given for a magnetic dipole i...

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“…There are several applications where this increase in speed will be useful. Some examples include calculation of so-called phase plots (plots of intensity versus observer angle ζ and phase φ; see, e.g., Romani & Yadigaroglu 1995), from which light curves are created by making constant-ζ slices; performing a parameter study for a population of pulsars, which will require spectra and light curves for several observers; and calculation of the geometric factor f Ω used for converting observed energy flux to total gamma-ray luminosity (Watters et al 2009). …”

Section: Resultsmentioning

confidence: 99%

Accelerating High-Energy Pulsar Radiation Codes

Venter

Jager²

2010

ApJ

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Curvature radiation (CR) is believed to be a dominant mechanism for creating gamma-ray emission from pulsars and is emitted by relativistic particles that are constrained to move along curved magnetic field lines. Additionally, synchrotron radiation (SR) is expected to be radiated by both relativistic primaries (involving cyclotron resonant absorption of radio photons and re-emission of SR photons), or secondary electron-positron pairs (created by magnetic or photon-photon pair production processes involving CR gamma rays in the pulsar magnetosphere). When calculating these high-energy spectra, especially in the context of pulsar population studies where several millions of CR and SR spectra have to be generated, it is profitable to consider approximations that would save computational time without sacrificing too much accuracy. This paper focuses on one such approximation technique, and we show that one may gain significantly in computational speed while preserving the accuracy of the spectral results.

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An ATLAS FOR INTERPRETING Γ-Ray PULSAR LIGHT CURVES

Cited by 220 publications

References 27 publications

The Tale of the Two Tails of the Oldish PSR J2055+2539

The Tale of the Two Tails of the Oldish PSR J2055+2539

Gamma-ray pulsars: A gold mine

Accelerating High-Energy Pulsar Radiation Codes

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