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Hot Relics in GRB Photosphere and GeV Photon Delay. Kunihito Ioka (KEK). Contents. Very High Lorentz Factor (VHLF) G max can be up to ~10 6 (> G max, conv ~10 3 ) Internal Shock Synchrotron ⇒ Power-law component over >7 decades - PowerPoint PPT Presentation
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Hot Relics in GRB Photosphere and GeV Photon Delay
Kunihito Ioka (KEK)
ContentsVery High Lorentz Factor (VHLF)Gmax can be up to ~106 (> Gmax,conv~103)
Internal Shock Synchrotron⇒ Power-law component over >7 decades
c tdelay ~ Baryon Load Radius~ Progenitor Radius ~ 1010cm
Neutrino – GeV g Anti-Correlation
Fermi Revolution
Abdo+ 09Ohno’s talk
MeV
GeV
GeV onset delay gg→e+e-
⇒ G>103
~1 sec
Fermi Revolution
Abdo+ 09Ohno’s talk
GRB 090902B
GRB 090510
Band component+ Power Law
Band ~ Black body-like⇒ Photosphere emission
GeVkeV
Hurley+94Gonzaletz+03
Photosphere-Internal-External Shock Model
Photo-sphere
InternalShock
ExternalShock
€
νFν
€
νkeV MeV GeV
Toma, Wu & MeszarosKumar & Barniol Duran 09Ghisellini+09, Wang+09Corsi+09, Gao+10
Variable Long-lived
Amati/Yonetoku Relation
L T∝ 2
€
L = 4πr02aT0
4
Tobs ~ T0
L T∝ 4
Yonetoku+KI 03[Ghirlanda’s talk]
A Distance Indicator
Fireball Dissipation
ln r
€
L = 4πrb2aTb
4
Tb ∝ rb−1 2L1 4
r0 rb
G
rsh rph
Tobs
Gm
For Yonetoku Rel.
€
rb ∝Γm−1 ∝ L−1 2
Rees & Meszaros 05Thompson+ 07Ghisellini+ 07Ryde & Pe’er 09KI+07
Radiation
in Comoving
Proton
Energy Densityafter Shock
pp collision thick pp collision thin
Accelerated to Very High
Radiation Dominated
€
Gm
€
′ U γ ~ ′ U p>> ′ U p,rest
€
Gc ~ Γm2
€
~ 104 −106( )
€
′ g p ~ Γm
€
~ 102 −103( )
€
(A) Ekinetic << Eγ ⇐ E internal( )
€
(B) Eγ ~ Ekinetic ⇐ E internal( )
~ Hot Relicsin Cosmology
Conventional Fireball
Gmax~103
Meszaros & ReesShemi & PiranPaczynskiGoodman
Baryon-LessBaryon-Rich
Reheated FireballGmax~106!
KIin prep.
Baryon-LessBaryon-Rich
Internal Shock Synchrotron
KIin prep.
For Moderate GToma+10
G~103
Max Synchrotron Energy
€
′ t acc = ′ t cool
€
νmaxcool = mec
2
αΓ ~ 500 GeV Γ
104
⎛ ⎝ ⎜
⎞ ⎠ ⎟
€
′ t acc = ′ t dyn
€
νmaxdyn ~ 1 GeV Γ
6 ×104
⎛ ⎝ ⎜
⎞ ⎠ ⎟−6
GRB 090926 Break??
A target for CTA
Very High Lorentz Factor (VHLF) case
Wang+ 09Piran & Nakar 10Barniol Duran & Kumar 10
KI in prep.
GeV Onset Delay
pp Collision Thick Thin⇒[Baryon-rich Barion-less]⇒
€
νFν
€
νFν
€
νFν
Time
MeV g
GeV g
TeV ν
Time
Time
€
η
Time
€
ηk1pp thinpp thick
pp→p→νeν~Gm
2mpc2>0.1TeV
TeV ν – GeV g Anti-Correlation
Baryon-lessBaryon-rich
SummaryVery High Lorentz Factor (VHLF)Gmax can be up to ~106 (> Gmax,conv~103)
Internal Shock Synchrotron⇒ Power-law component over >7 decades
c tdelay ~ [rm=rpp~L-1/5] ~ Rstar ~ 1010cm
Neutrino – GeV g Anti-Correlation
Two-Mass Collision
Coasting Gc~Gm2
Mass=ErGr/Gm2<10− 8M ( available at Rstar)
€
E rΓr + Mc 2 = Γm Mc 2 + Em( )Γm
E r Γr2 −1 = Γm Mc2 + Em( ) Γm
2 −1
Energy
Momentum
€
⇒ Gm ~ E rΓr
2Mc 2 ∝ L1 2
€
E r
Γr
< Mc 2 < E rΓr
⎛ ⎝ ⎜
⎞ ⎠ ⎟
YonetokuRelation
€
Em ~ Γm Mc2 Before dissipation,rela. matter E ~ radiation E