Gamma Radiation from PSR B1055−52

Thompson, D. J.; Bailes, M.; Bertsch, D. L.; Cordes, J. M.; D’Amico, N.; Esposito, J. A.; Finley, J. P.; Hartman, R. C.; Hermsen, W.; Kanbach, G.; Kaspi, V. M.; Kniffen, D. A.; Kuiper, L.; Lin, Y. C.; Lyne, A. G.; Manchester, R. N.; Matz, S. M.; Mayer‐Hasselwander, H. A.; Michelson, P. F.; Nolan, P. L.; Öğelman, H.; Pohl, M.; Ramanamurthy, P. V.; Sreekumar, P.; Reimer, O.; Taylor, J. H.; Ulmer, M. P.

doi:10.1086/307083

Cited by 128 publications

(112 citation statements)

References 90 publications

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“…The Energetic Gamma Ray Experiment Telescope and the imaging Compton Telescope aboard the Compton Gamma Ray Observatory have detected pulsed signals from at least seven rotation-powered pulsars (Crab pulsar [10,11]; PSR B1509-58 [12]; Vela pulsar [13,11]; PSR B1706-44 [14]; PSR B1951+32 [15]; Geminga pulsar [16,11]; PSR B1055-52 [17]). Four of them (Crab, Vela, Geminga, and B1951+32) exhibit doublepeaked light curves [18,19,20] (fig.…”

Section: Gamma-ray Observations and Physical Processesmentioning

confidence: 99%

High-Energy Emission From Pulsar Magnetospheres

Hirotani

2006

Mod. Phys. Lett. A

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A synthesis of the present knowledge on gamma-ray emission from the magnetosphere of a rapidly rotating neutron star is presented, focusing on the electrodynamics of particle accelerators. The combined curvature, synchrotron, and inverse-Compton emission from ultra-relativistic positrons and electrons, which are created by two-photon and/or one-photon pair creation processes, or emitted from the neutron-star surface, provide us with essential information on the properties of the accelerator -electric potential drop along the magnetic field lines. A new accelerator model, which is a mixture of traditional inner-gap and outer gap models, is also proposed, by solving the Poisson equation for the electrostatic potential together with the Boltzmann equations for particles and gamma-rays in the two-dimensional configuration and twodimensional momentum spaces.

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Section: Gamma-ray Observations and Physical Processesmentioning

confidence: 99%

High-Energy Emission From Pulsar Magnetospheres

Hirotani

2006

Mod. Phys. Lett. A

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“…Among the pulsars that are either reliably or probably identified with EGRET sources, there is a trend (Thompson et al 1997(Thompson et al , 1999 in which the efficiency of greater than 100 MeV g-ray production increases with decreasing spin-down power ( ), or equivalently, open field line voltage ( 2 4 E ∝ B /P F ∝ ). Their efficiencies range from 0.002 for the Crab to 2 B/P of order unity for the middle-aged pulsars Geminga and PSR B1055Ϫ52.…”

Section: Optical Observationsmentioning

confidence: 99%

PSR J2229+6114: Discovery of an Energetic Young Pulsar in the Error Box of the EGRET Source 3EG J2227+6122

Halpern

Camilo

Gotthelf

et al. 2001

The Astrophysical Journal

141

100

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We report the detection of radio and X-ray pulsations at a period of 51.6 ms from the X-ray source RX/AX J2229.0ϩ6114 in the error box of the EGRET source 3EG J2227ϩ6122. An ephemeris derived from a single ASCA observation and multiple epochs at 1412 MHz from Jodrell Bank indicates steady spin-down withṖ p s s Ϫ1 . From the measured P and , we derive spin-down power ergs s Ϫ1 , magnetic.83 # 10 P E p 2.2 # 10 field G, and characteristic age yr. An image from the Chandra X-Ray Obser-p vatory reveals a point source surrounded by centrally peaked diffuse emission that is contained within an incomplete radio shell. We assign the name G106.6ϩ2.9 to this new supernova remnant, which is evidently a pulsar wind nebula. For a distance of 3 kpc estimated from X-ray absorption, the ratio of X-ray luminosity to spin-down power is ≈ , smaller than that of most pulsars but similar to the Vela pulsar. If PSR J2229ϩ6114 Ϫ58 # 10 is the counterpart of 3EG J2227ϩ6122, then its efficiency of g-ray production, if isotropic, is 0.016 (d/3 kpc) 2 . It obeys an established trend of g-ray efficiency among known g-ray pulsars, which, in combination with the demonstrated absence of any other plausible counterpart for 3EG J2227ϩ6122, makes the identification compelling. If confirmed, this identification bolsters the pulsar model for unidentified Galactic EGRET sources.

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“…For Crab (Nolan et al 1993) and PSR B1951+32 (Srinivasan et al 1997), there was only an indication of a possible cutoff in the GeV energy range. However, the other pulsars detected by CGRO showed no indication of a cutoff up to energies of 5-10 GeV (Fierro 1995; Thompson et al 1999) because of insufficient sensitivity. On the other hand, no indication of pulsed emission in the energy band studied between 150 GeV and 50 TeV has been observed (Aharonian et al 2007a;Albert et al 2008b;Albert et al 2007) by the previous generation of ground-based Imaging Air Cherenkov telescopes (IACT).…”

Section: Introductionmentioning

confidence: 99%

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

Anderhub¹,

Antonelli²,

Antoranz³

et al. 2010

ApJ

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The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other groundbased instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions.

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Gamma Radiation from PSR B1055−52

Cited by 128 publications

References 90 publications

High-Energy Emission From Pulsar Magnetospheres

High-Energy Emission From Pulsar Magnetospheres

PSR J2229+6114: Discovery of an Energetic Young Pulsar in the Error Box of the EGRET Source 3EG J2227+6122

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

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