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Neutrino Oscillation in Magnetized GRB Fireball Study | Cosmological Phenomenon Research

Investigating neutrino oscillation in magnetized gamma-ray burst (GRB) fireballs, relating to brightest explosions in the Universe, non-thermal bursts, isotropic distribution, and classes of GRBs. Results connect to Supernova and compact binaries, with substantial implications for neutrino detection and astrophysical research. Study parameters based on SNO, SuperKamiokande, and LSND findings are analyzed, providing insights into resonance conditions and potential characteristics of GRB fireballs. Despite challenges in detecting MeV neutrinos, this research contributes valuable understanding to cosmological phenomena.

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Neutrino Oscillation in Magnetized GRB Fireball Study | Cosmological Phenomenon Research

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  1. Neutrinooscillation in MagnetizedGamma-RayBurstFireball NISSIM ILLICH FRAIJA Thiswork (withcollaboratorsSahu et al) wasaccepted in PRD (arXiv: 0904.0138)

  2. GRBs Weknow : • Thebrighestexplotions in theUniverse~1053 erg • flashes of non-thermalbursts of lowenergy 100 keV- 1 MeV • highvariability • HugeOpticaldepthduetheprocess • distributionIsotropic • Cosmologicaldistances. • There are twoclasses (Short GRB lessthan 2 s – long GRB greaterthan 2 s). • Long GRB isrelatedto Supernova • Short GRB isrelatedtotheCoalescing of compact binaries . e-e+

  3. A generic GRB fireball(B. Zhang and Meszaros Int. J. Mod.Phys. A19, 2004) UV/opt/IR/radio gamma-ray central photosphere internal external shocks engine (shocks) (reverse)(forward) t~102 s r~1012cm t~106 s r~1016cm r~107cm T~10 MeV t~103 s r~1014cm

  4.  e n p GRB fireball – Aproximate Inicial state Progenitor Characteristics Energy Temperature Inicial radium OpticalDepth Thereis B~104 G Isthermalized ThisMeV neutrinos are similar totheoneproducedbytype II Supernova (SN1987A)

  5. e if , neutrino test Medium particles  e- e+ n B (magneticfield) p P

  6. In theFireballwehaveBaryons, e  in a magnetizedmedium, f f MSW Effect where, where, Resonancecondition

  7. RESULTS

  8. SNO (SudburyNeutinoObservatory): parameters 6x10-5eV2< m2<10-4eV2 and 0.64<sin22<0.96 m2~ 7.1 x 10-5 eV2 sin22~0.69 Resonancelength =10p m

  9. SuperKamiokande: Parameters 1.9x10-3eV2< m2<3.0x10-3eV2 and 0.9<sin22<1.0 m2~ 2.5 x 10-3 eV2 sin22~0.9 Resonancelength =10p m

  10. LSND (LiquidScintillator Neutrino Detector) : Parameters 0.45 eV2< m2<1 eV2 and 2X10-3<sin22<7X10-3 m2~ 0.5 eV2 sin22~0.0049 Resonancelength =10p m

  11. Conclusions • Wehavestudiedthepossibility of resonantoscillation of e, in GRB Fireball. Wecalculatethe potencial • Forthefireball, weassume : Itwasspherewith radio ~100 – 1000 km, temperature~ 3-10 MeV,electrically neutral charge Le=Lp . Resonanceconditions • We use theparameters of the SNO, Superkamiokande and LSND.

  12. Withthe potencial and theresonancecondition - Wecalculate: • Barionic load • Leptonicasymmetry • ResonanceLength Dueto GRB are of cosmologicaldistanceMeV neutrinos isverydifficulttodetect in thismoment.

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