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High-Energy Gamma-Rays and Physical Implication for GRBs in Fermi Era. Katsuaki Asano (Tokyo Institute of Technology). Outline. Introduction Limit on LIV Jet Acceleration Particle Acceleration. Gamma-Ray Burst. The most luminous explosion in the universe. 10 52 -10 54 erg/s. Reference:
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High-Energy Gamma-Rays and Physical Implication for GRBs in Fermi Era Katsuaki Asano (Tokyo Institute of Technology)
Outline • Introduction • Limit on LIV • Jet Acceleration • Particle Acceleration
Gamma-Ray Burst The most luminous explosion in the universe 1052-1054 erg/s • Reference: • Sun 3.9 1033 erg/s • X-ray star 1038 erg/s • Supernova, Galaxy 1043 erg/s • AGN 1046 erg/s • SGR 1047 erg/s Light Curve
GRB rate Supernova rate ~ 2.4x105 Gpc-3yr-1 (60% II, 30% Ia, 10% type Ib/c) Hypernova ~500 Gpc-3yr-1 GRB (Jet corrected) ~20 Gpc-3yr-1 ~1 detection/day
Standard Picture ISM External Shock Internal Shock
Afterglow Racusin et al. 2009 Nardini et al. 2009
Evidence of Collimated Jet Sideway Expansion Jet Break Stanek et al. 2000 Apparent Energy >1053erg ->Actual Energy 1051 erg?
The most distant object ever confirmed GRB 090423 z=8.2, t=0.6 billion yrs LyαEmitter z=6.964, t=0.78 bill. yrs
Open Problems • Emission Mechanism (Synchrotron?) • High Efficiency • Spectrum • Central Engine (Death of Massive Star?) • Progenitor • Energy Release • Jet Acceleration & Collimation • Afterglow (External Shock?) • Spectrum & Time Evolution
GRB 080916C; Spectra Classical Energy Range
Famous Fermi/LAT GRBs • GRB 080825C • First LAT GRB, delay for>100MeV • GRB 080916C • Eiso=8.8x1054 erg @ z=4.35, delay • GRB 081024B • First short LAT GRB, delay • GRB 090510 • Short @ z=0.903, delay?, extra component • GRB 090902B • Eiso=4x1054 erg @ z=1.822 , extra component
Constraints on Lorentz Invariant Violation
Measuring the Speed of Light GRBs: Bright Distant Objects with Emissions of Wide Energy Ranges -> Ideal to measure the difference of “c”! Loop quantum gravity? NYTimes ’09 Oct. 28
Motivation How to reconcile gravitation with quantum mechanics? -> Classical symmetric properties will be sacrificed? (Spontaneously? Effectively in 4-D?) Effective Field Theory (Colladay & Kostelecky 1998) CPT violating CPT conserving Photon velocity CPT symmetry kills the term.
Quantum Gravity Test 高エネルギー光子が遅れてくる? ? (LHC BH??) Smaller MQG -> large time delay?
GRB 090510 Short GRB Precursor Delay 8keV-260keV 260keV-5MeV z=0.903 (traveling 7.3 Bill. yrs) Eiso=1053erg >100MeV >1GeV 31GeV, 3.4GeV
“c” is the same with 18 digits! 29979245800.0000000?? cm/s depends on E? At least MQG,1>Mpl !
CTA We can expect 1000 photons @ 10 GeV from a GRB. 10 GeV pulse shape ~keV pulse shape Much stronger constraint
Ultra-relativistic… Jet Acceleration
GRB 080916C 8keV-260keV 260keV-5MeV Long GRB Delay z=4.35 Eiso=8.8x1054erg >100MeV ~5xMsunc2 >1GeV 13GeV 3GeV
Compactness Problem If gamma-rays are emitted isotropically, GeV photons cannot escape because electron-positron pairs should be created via photon-photon collision. →Inconsistent with obs. In the comoving frame… If the sources are ultra-relativistic… (We have observed blue-shifted photons) X-ray No high energy photons
Minimum Lorentz factor GRB 090510 > 1200 GRB 080916C > 900
Fireball Acceleration • Radiation dominated plasma; huge amount of electron-positron pairs and photons, and small amount of protons. • Adiabatic Expansion; Thermal Energy -> Bulk Kinetic Energy • Fireball Evolution: is required.
Central Engine How to deposit energy without much baryons? Neutrino pair annihilation? Collimated energy injection can evacuate baryons and make a fireball. Macfadyen & Woosley
Lack of Thermal Emission The fireball becomes optically thin as it expands. -> Thermal Photons GRB 080916C GRB090102 Optical polarization is reported. -> Strongly Magnetized Plasma? Zhang & Pe’er 2009
Poynting Flux Dominated Jet? Magnetic Energy dominates the bulk kinetic energy -> can be relativistic. MHD turbulences (MRI) enhance the magnetic field. • Weak points: • Hard to produce shocks • Hard to induce magnetic reconnection How to convert kinetic energy into photons?? McKinney & Blandford 2009
Ultra High Energy Cosmic Rays Particle Acceleration
Ultra High Energy Cosmic Ray (UHECR) Where is the accelerator?? (Strong magnetic field or large size to confine particles) n(E)∝E-3 Energy distribution >1020eV Ref: 7 TeV by LHC AGN? (low number density)
Highest Accelerator=GRB? We need 6-8 1043 ergs/Mpc3/yr to explain UHECRs See e.g. Murase et al. 2008 We may need Up/Ue>20. If GRB rate is 0.05 Gpc-3/yr, Up/Ue>100 Hidden Energy?
GRB 090510; Spectra Band+ Extra PL
Extra Component=Afterglow? 2009 GRB 090510
GeV-MeV correlate? Abdo et al. 2009 Supporting material
Signature of Proton Acceleration? Hadronic Cascade • p+γ→p(n)+π0(π+) • p+γ→p+ e+ + e- • π0→γ+γ, π+→μ+ +νμ • μ+ →e+ + νμ + νe • Synchrotron from π+ ,μ+,e± • Inverse Compton from π+ ,μ+,e± • γ+γ→ e+ + e- • Synchrotron Self Absorption
Asano, Guiriec & Meszaros 2009 Cascade due to photopion production gg-absorption R=1014 cm G=1500 Band component 3.4GeV Synchrotron and Inverse Compton due to secondary electron-positron pairs
Proton Synchrotron R=1014 cm Even in this case, secondary pairs contribute
Proton Dominated GRBs Favorable for ultra high-energy cosmic ray production Asano, Inoue & Meszaros 2009 GRB 090510 10keV 1MeV 1GeV The extra component: Hard spectrum: Index -1.6 Comparable flux to the Band flux Excess @ 10 keV
Neutrinos from GRB 090510 “Bright” Neutrino We may need >10-2 erg/cm2 to detect with IceCube.
Conclusion • LIV with n=1 may be excluded. • Lorentz factor of GRB Jets > 1000. • Possible signature of UHECR production. New Theoretical Challenge: Delayed onset of GeV Emission GRB 080916C GRB 090510