hot relics in grb photosphere and gev photon delay
DESCRIPTION
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 PresentationTRANSCRIPT
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Hot Relics in GRB Photosphere and GeV Photon Delay
Kunihito Ioka (KEK)
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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
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Fermi Revolution
Abdo+ 09Ohno’s talk
MeV
GeV
GeV onset delay gg→e+e-
⇒ G>103
~1 sec
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Fermi Revolution
Abdo+ 09Ohno’s talk
GRB 090902B
GRB 090510
Band component+ Power Law
Band ~ Black body-like⇒ Photosphere emission
GeVkeV
Hurley+94Gonzaletz+03
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Photosphere-Internal-External Shock Model
Photo-sphere
InternalShock
ExternalShock
€
νFν
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νkeV MeV GeV
Toma, Wu & MeszarosKumar & Barniol Duran 09Ghisellini+09, Wang+09Corsi+09, Gao+10
Variable Long-lived
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Amati/Yonetoku Relation
L T∝ 2
€
L = 4πr02aT0
4
Tobs ~ T0
L T∝ 4
Yonetoku+KI 03[Ghirlanda’s talk]
A Distance Indicator
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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
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Radiation
in Comoving
Proton
Energy Densityafter Shock
pp collision thick pp collision thin
Accelerated to Very High
Radiation Dominated
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Gm
€
′ U γ ~ ′ U p>> ′ U p,rest
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Gc ~ Γm2
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~ 104 −106( )
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′ g p ~ Γm
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~ 102 −103( )
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(A) Ekinetic << Eγ ⇐ E internal( )
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(B) Eγ ~ Ekinetic ⇐ E internal( )
~ Hot Relicsin Cosmology
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Conventional Fireball
Gmax~103
Meszaros & ReesShemi & PiranPaczynskiGoodman
Baryon-LessBaryon-Rich
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Reheated FireballGmax~106!
KIin prep.
Baryon-LessBaryon-Rich
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Internal Shock Synchrotron
KIin prep.
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For Moderate GToma+10
G~103
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Max Synchrotron Energy
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′ t acc = ′ t cool
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νmaxcool = mec
2
αΓ ~ 500 GeV Γ
104
⎛ ⎝ ⎜
⎞ ⎠ ⎟
€
′ t acc = ′ t dyn
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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.
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GeV Onset Delay
pp Collision Thick Thin⇒[Baryon-rich Barion-less]⇒
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€
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
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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
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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