DISCOVERY OF GeV γ-RAY EMISSION FROM PSR B1259–63/LS 2883

Tam, P. H. T.; Huang, R. H. H.; Takata, Jumpei; Hui, C. Y.; Kong, Albert; Cheng, K. S.

doi:10.1088/2041-8205/736/1/l10

Cited by 88 publications

(96 citation statements)

References 30 publications

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“…This is equivalent to the multiplicity κ ∼ 10 5 , about an order of magnitude smaller than the one inferred for the Crab pulsar. The emission from the precursor would be in the optical band, and the IC emission associated with the particles upscattering the stellar photons, in a few hundred MeV -consistent with the high energy flare observed by Fermi-LAT [10].…”

Section: Implications For the Emission In Binariessupporting

confidence: 66%

High-energy emission from pulsar binaries

Mochol

Kirk

2012

AIP Conference Proceedings

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Abstract. Unpulsed, high-energy emission from pulsar binaries can be attributed to the interaction of a pulsar wind with that of a companion star. At the shock between the outflows, particles carried away from the pulsar magnetosphere are accelerated and radiate both in synchrotron and inverse Compton processes. This emission constitutes a significant fraction of the pulsar spin-down luminosity. It is not clear however, how the highly magnetized pulsar wind could convert its mainly electromagnetic energy into the particles with such high efficiency. Here we investigate a scenario in which a pulsar striped wind converts into a strong electromagnetic wave before reaching the shock. This mode can be thought of as a shock precursor that is able to accelerate particles to ultrarelativistic energies at the expense of the electromagnetic energy it carries. Radiation of the particles leads to damping of the wave. The efficiency of this process depends on the physical conditions imposed by the external medium. Two regimes can be distinguished: a high density one, where the EM wave cannot be launched at all and the current sheets in the striped wind are first compressed by an MHD shock and subsequently dissipate by reconnection, and a low density one, where the wind can first convert into an electromagnetic wave in the shock precursor, which then damps and merges into the surroundings. Shocks in binary systems can transit from one regime to another according to binary phase. We discuss possible observational implications for these objects.

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Section: Implications For the Emission In Binariessupporting

confidence: 66%

High-energy emission from pulsar binaries

Mochol

Kirk

2012

AIP Conference Proceedings

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“…The very-high energy radiation is often interpreted as inverse Compton scattering of the UV stellar photons on relativistic pairs accelerated near the shock front between the pulsar wind and the stellar wind (e.g., Tavani and Arons 1997;Kirk et al 1999;Khangulyan et al 2007). The model predicts a maximum of GeV gamma-ray emission close to periastron which was indeed observed for the first time by the Fermi-LAT during the 2010 periastron passage (Tam et al 2011;Abdo et al 2011a). A few weeks after the peak of the periastron emission faded away, and against all expectations, a bright flare appeared in the Fermi data.…”

Section: Comparison With Gev Flares In the Psr B1259-63/ls 2883 Binarymentioning

confidence: 97%

Pulsar-Wind Nebulae

et al. 2015

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“…In this case the efficiency of IC scattering is higher because of the presence of copious target photons provided by the companion star, but the gamma-ray lines are less sharp than for the isolated pulsars because of lower values of the Klein-Nishina parameter b. It has recently been argued ) that the bright flare of the binary pulsar PSR B1259-63/LS2883, detected by Fermi in 2011 (Abdo et al 2011;Tam et al 2011), could be best explained by the IC scattering of the unshocked pulsar. The spectral measurements of Fermi LAT require a relatively modest Lorentz factor of the wind, Γ w ≈ 10 4 .…”

Section: Astrophysical Vhe Gamma-ray Lines?mentioning

confidence: 98%

Cold ultrarelativistic pulsar winds as potential sources of galactic gamma-ray lines above 100 GeV

Aharonian

Khangulyan

Malyshev

2012

A&A

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Context. The evidence of line-like spectral features above 100 GeV, in particular at 130 GeV, which have been recently reported from some parts of the Galactic plane, poses serious challenges for any interpretation of this surprise discovery. It is generally believed that the unusually narrow profile of the spectral line cannot be explained by conventional processes in astrophysical objects, and, if real, is likely to be associated with dark matter. Aims. In this paper we argue that cold ultrarelativistic pulsar winds can be alternative sources of very narrow gamma-ray lines. Methods. We demonstrate that Comptonization of a cold ultrarelativistic electron-positron pulsar wind in the deep Klein-Nishina regime can readily provide very narrow (ΔE/E ≤ 0.2) distinct gamma-ray line features. To verify this prediction, we produced photon-count maps based on the Fermi LAT data in the energy interval 100 to 140 GeV. Results. We confirm earlier reports of the presence of marginal gamma-ray line-like signals from three regions of the Galactic plane. Although the maps show some structure inside these regions, unfortunately the limited photon statistics do not allow any firm conclusion in this regard. Conclusions. The confirmation of 130 GeV line emission by low-energy threshold atmospheric Cherenkov telescope systems, in particular by the new 28 m diameter dish of the H.E.S.S. array, would be crucial for resolving the spatial structure of the reported hotspots, and thus for distinguishing between the dark matter and pulsar origins of the "Fermi Lines".

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DISCOVERY OF GeV γ-RAY EMISSION FROM PSR B1259–63/LS 2883

Cited by 88 publications

References 30 publications

High-energy emission from pulsar binaries

High-energy emission from pulsar binaries

Pulsar-Wind Nebulae

Cold ultrarelativistic pulsar winds as potential sources of galactic gamma-ray lines above 100 GeV

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