002214125 001__ 2214125
002214125 003__ SzGeCERN
002214125 005__ 20230314181957.0
002214125 0248_ $$aoai:inspirehep.net:742087$$pcerncds:CERN$$pcerncds:CERN:FULLTEXT$$pcerncds:FULLTEXT$$qCERN$$qINSPIRE:HEP$$qCERN:arXiv$$qForCDS
002214125 035__ $$9arXiv$$aoai:arXiv.org:astro-ph/0701294
002214125 037__ $$9arXiv$$aastro-ph/0701294$$castro-ph
002214125 035__ $$9Inspire$$aoai:inspirehep.net:742087$$d2023-03-06T19:28:34Z$$h2023-03-14T15:04:51Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002214125 035__ $$9Inspire$$a742087
002214125 041__ $$aeng
002214125 088__ $$9arXiv$$aastro-ph/0701294$$castro-ph
002214125 100__ $$aDado, Shlomo$$uTechnion
002214125 210__ $$aGAMMA-RAY
002214125 245__ $$aImplications of the Large Polarization Measured in Gamma Ray Bursts
002214125 246__ $$9arXiv$$aImplications of the Large Polarization Measured in Gamma Ray
002214125 260__ $$c2007
002214125 269__ $$c2007-01
002214125 300__ $$a8 p
002214125 520__ $$9arXiv$$aThe polarization of the prompt $\gamma$-ray emission has been measured in four bright gamma ray bursts (GRBs). It was nearly maximal in all cases, as predicted by the Cannonball (CB) model of GRBs long before the observations. These results are inconsistent with standard models of GRBs wherein the prompt emission is due to synchrotron radiation. A much smaller linear polarization is predicted by the CB model for the prompt emission in X-ray flashes (XRFs) and in extremely luminous GRBs. These measurements would provide yet another stringent test of the CB model and its unification of GRBs and XRFs.
002214125 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002214125 690C_ $$aCERN
002214125 700__ $$aDar, Arnon$$uTechnion
002214125 700__ $$aDe Rujula, A.$$uCERN
002214125 773__ $$wC06-05-22.5
002214125 8564_ $$82217516$$s122218$$uhttps://cds.cern.ch/record/2214125/files/arXiv:astro-ph_0701294.pdf
002214125 960__ $$a11
002214125 962__ $$b947760$$k$$nvulcano20060522
002214125 980__ $$aPREPRINT
002214125 980__ $$aConferencePaper