Evitable vs Inevitable Complications

Goodman, Richard S

doi:10.3928/0147-7447-19860201-18

Cited by 1 publication

(1 citation statement)

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“…Depending primarily on the dimen-sionless entropy and the magnetisation of the outflow, the emission can stem from the photosphere, internal shocks, magnetic reconnection, or the external shock [26,27]. The high-energy emission is thus typically attributed to synchrotron radiation [28,29] or emission from the photosphere [30,31,32]. The Compton drag model is also considered [33], but is not as well established.…”

Section: High-energy Emission Mechanismmentioning

confidence: 99%

Science prospects for SPHiNX – A small satellite GRB polarimetry mission

Pearce

Eliasson

Iyer

et al. 2019

Astroparticle Physics

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Gamma-ray bursts (GRBs) are exceptionally bright electromagnetic events occurring daily on the sky. The prompt emission is dominated by X-/γ-rays. Since their discovery over 50 years ago, GRBs are primarily studied through spectral and temporal measurements. The properties of the emission jets and underlying processes are not well understood. A promising way forward is the development of missions capable of characterising the linear polarisation of the high-energy emission. For this reason, the SPHiNX mission has been developed for a small-satellite platform. The polarisation properties of incident high-energy radiation (50-600 keV) are determined by reconstructing Compton scattering interactions in a segmented array of plastic and Gd 3 Al 2 Ga 3 O 12 (Ce) (GAGG(Ce)) scintillators. During a two-year mission, ∼200 GRBs will be observed, with ∼50 yielding measurements where the polarisation fraction is determined with a relative error ≤10%. This is a significant improvement compared to contemporary missions. This performance, combined with the ability to reconstruct GRB localisation and spectral properties, will allow discrimination between leading classes of emission models.

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