<i>FERMI</i>LARGE AREA TELESCOPE OBSERVATIONS OF THE VELA PULSAR

Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Bagagli, R.; Baldini, Luca; Ballet, J.; Band, D. L.; Barbiellini, G.; Baring, Matthew G.; Bartelt, J.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellardi, F.; Bellazzini, R.; Berenji, B.; Bisello, D.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Ceccanti, M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L.; Conrad, J.; Corbet, R. H. D.; Corucci, L.; Cutini, S.; Davis, David; Deklotz, M.; Dermer, C. D.; Angelis, A. De; Palma, F. de; Digel, S. W.; Dormody, M.; Silva, E. Do Couto E; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C. M.; Farnier, C.; Favuzzi, C.; Flath, D.; Fleury, P.; Focke, W. B.; Frailis, M.; Friere, P. C C; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giannitrapani, R.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M.‐H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Haller, G.; Harding, A. K.; Hart, Philip; Hartman, R. C.; Hays, E.; Hobbs, G.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanbach, G.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kavelaars, A.; Kawai, N.; Kelly, Heather; Kerr, M.; Kızıltan, Bülent; Klamra, W.; Knödlseder, J.; Krämer, M.; Kuehn, F.; Kuss, M.; Landé, J.; Landriu, D.; Latronico, L.; Lee, B.; Lee, S. H.; Lemoine‐Goumard, M.; Livingstone, Margaret A.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marangelli, B.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; McLaughlin, M. A.; Menon, Nidu; Meurer, C.; Michelson, P. F.; Mineo, T.; Mirizzi, N.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Mongelli, M.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, Takeshi; Nolan, P. L.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, Masanori; Paccagnella, A.; Paneque, D.; Panetta, J.; Parent, D.; Pearce, Mark; Pepé, M.; Perchiazzi, M.; Pesce-Rollins, M.; Pieri, L.; Pinchera, Michele; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Rapposelli, Emilio; Razzano, M.; Reimer, A.; Reposeur, T.; Reyes, Luis; Ritz, S.; Rochester, Lynn; Rodriguez, A. Y.; Romani, Roger W.; Roth, M.; Ryde, F.; Sacchetti, A.; Sadrozinski, H. F-W.; Saggini, N.; Sánchez, David; Sander, A.; Parkinson, P. M. Saz; Segal, K.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Starck, Jean-Luc; Stecker, F. W.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, Tadayuki; Tanaka, Takaaki; Tenze, A.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tramacere, A.; Turri, M.; Usher, T.; Vigiani, L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/696/2/1084

Cited by 132 publications

(139 citation statements)

References 36 publications

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“…Another example can be seen in the gamma rays profile of the Vela pulsar revealed by the Fermi-LAT telescope (Abdo et al 2009) displayed in Fig. 2.…”

Section: Introductionmentioning

confidence: 89%

General solution for the vacuum electromagnetic field in the surroundings of a rotating star

Bonazzola¹,

Mottez²,

Heyvaerts³

2014

A&A

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Aims. Many recent observations of pulsars and magnetars can be interpreted in terms of neutron stars with multipole electromagnetic fields. As a first approximation, we investigate the multipole magnetic and electric fields in the environment of a rotating star when this environment is deprived of plasma. Methods. We compute a multipole expansion of the electromagnetic field in vacuum for a given magnetic field on the conducting surface of the rotating star. Then, we consider a few consequences of multipole fields of pulsars. Results. We provide an explicit form of the solution. For each spherical harmonic of the magnetic field, the expansion contains a finite number of terms. A multipole magnetic field can provide an explanation for the stable sub-structures of pulses, and they offer a solution to the problem of current closure in pulsar magnetospheres. Conclusions. This computation generalises the widely used model of a rotating star in vacuum with a dipole field. It can be especially useful as a first approximation to the electromagnetic environment of a compact star, for instance a neutron star, with an arbitrarily magnetic field.

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“…Another example can be seen in the gamma rays profile of the Vela pulsar revealed by the Fermi-LAT telescope (Abdo et al 2009) displayed in Fig. 2.…”

Section: Introductionmentioning

confidence: 89%

General solution for the vacuum electromagnetic field in the surroundings of a rotating star

Bonazzola¹,

Mottez²,

Heyvaerts³

2014

A&A

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“…The first result has settled a two-decade-long debate on the origin of the γ rays in the inner or outer parts of a magnetosphere [48]. Magnetic pair production occurs in the strong fields present above the polar caps.…”

Section: From Six To Ninety Young γ-Ray Pulsarsmentioning

confidence: 99%

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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“…Compared to EGRET, the LAT has a larger effective area (∼8000 cm 2 on-axis above 1 GeV), a broader field of view (∼2.4 sr) and superior angular resolution (∼0.6 • 68% containment at 1 GeV for events converting in the front section of the tracker). The on-orbit calibration is described in Abdo et al (2009c).…”

Section: Lat Description and Observationsmentioning

confidence: 99%

Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357−6429 withFermiandXMM-Newton

Lemoine‐Goumard

Zavlin

Grondin

et al. 2011

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Context. Since the launch of the Fermi satellite, the number of known gamma-ray pulsars has increased tenfold. Most gamma-ray detected pulsars are young and energetic, and many are associated with TeV sources. PSR J1357−6429 is a high spin-down power pulsar (Ė = 3.1 × 10 36 erg s −1 ), discovered during the Parkes multibeam survey of the Galactic plane, with significant timing noise typical of very young pulsars. In the very-high-energy domain (E > 100 GeV), H.E.S.S. has reported the detection of the extended source HESS J1356−645 (intrinsic Gaussian width of 12 ) whose centroid lies 7 from PSR J1357−6429. Aims. We search for gamma-and X-ray pulsations from this pulsar, characterize the neutron star emission and explore the environment of PSR J1357−6429. Methods. Using a rotational ephemeris obtained with 74 observations made with the Parkes telescope at 1.4 GHz, we phase-fold more than two years of gamma-ray data acquired by the Large Area Telescope on-board Fermi as well as those collected with XMM-Newton, and perform gamma-ray spectral modeling. Results. Significant gamma-and X-ray pulsations are detected from PSR J1357−6429. The light curve in both bands shows one broad peak. Gamma-ray spectral analysis of the pulsed emission suggests that it is well described by a simple power-law of index 1.5 ± 0.3 stat ± 0.3 syst with an exponential cut-off at 0.8 ± 0.3 stat ± 0.3 syst GeV and an integral photon flux above 100 MeV of (6.5 ± 1.6 stat ± 2.3 syst ) × 10 −8 cm −2 s −1 . The X-ray spectra obtained from the new data provide results consistent with previous work. Upper limits on the gamma-ray emission from its potential pulsar wind nebula (PWN) are also reported. Conclusions. Assuming a distance of 2.4 kpc, the Fermi LAT energy flux yields a gamma-ray luminosity for PSR J1357−6429 of L γ = (2.13 ± 0.25 stat ± 0.83 syst ) × 10 34 erg s −1 , consistent with an L γ ∝ √Ė relationship. The Fermi non-detection of the pulsar wind nebula associated with HESS J1356−645 provides new constraints on the electron population responsible for the extended TeV emission.

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FERMILARGE AREA TELESCOPE OBSERVATIONS OF THE VELA PULSAR

Cited by 132 publications

References 36 publications

General solution for the vacuum electromagnetic field in the surroundings of a rotating star

General solution for the vacuum electromagnetic field in the surroundings of a rotating star

Gamma-ray pulsars: A gold mine

Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357−6429 withFermiandXMM-Newton

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