l. amati, g. barbiellini , a celotti, a. galli, r. landi, f. longo, n. omodei, m. tavani
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Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 1
Relativistic interaction of a high intensity photon beam with a
plasma: a possible GRB emission
mechanism
L. Amati, G. Barbiellini, A Celotti, A. Galli, R. Landi, F. Longo, N. Omodei, M. Tavani
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 2
Bright and Dim GRB(Connaughton 2002)
Q = cts/peak cts
BRIGHT GRB DIM GRB
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 3
The Compton Tail
Barbiellini et al. (2004) MNRAS 350, L5
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 4
The Compton tail
“Prompt” luminosity
Compton “Reprocessed” luminosity
“Q” ratio
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 5
Bright and Dim Bursts
Bright bursts (tail at 800 s) Peak counts >1.5 cm-2 s-1 Mean Fluence 1.5 10-5 erg cm-2
Q = 4.0 0.8 10-4 (5 ) fit over PL
= 1.3 Dim bursts (tail at 300s)
peak counts < 0.75 cm-2 s-1
Mean fluence 1.3 10-6 erg cm-2
Q = 5.6 1.4 10-3 (4 ) fit over PL
=2.8
“Compton” correction
R = 1015 cmR ~ R ~ 0.1
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 6
WakeField Acceleration
(Ta Phuoc et al. 2005)
Laser Pulse tlaser = 3 10-14 sLaser Energy = 1 JouleGas Surface = 0.01 mm2
Gas Volume Density = 1019 cm3
Power Surface Density W= 3 1018 W cm-2
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 7
WakeField Acceleration(Ta Phuoc et al. 2005)
Emitted Photon SpectrumElectron Spectrum
Simulated Photon Spectrum
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 8
r0 ~ n-1/3 1/2
b~ n-1/21/2
p~ n-1/2
Scaling relations
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 9
Scaling relations
V ~ r03 ~ n-1
Q+=enr03~n0
~n-1/3
Ep = 3/4 hc2 r0/p2
(1019) ~ 102
(109) ~ 2x105
(102) ~ 2x108
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 10
3D PIC Simulation
PhD Thesis Marco Galimberti 2003 Pisa
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 11
GRB Gamma Emission in the stochastic wake field acceleration
regime
From the equation of the electron energy loss we derive
Re ~ 4.1p (pre
)2 / 31/ 6
Imposing Re = R, we link the jet angle to an energy threshold t
t 1.2(pre
)2 / 7 j 6 / 7
The previous relations allow the prediction of the typical energy emission
i rob
eff2 (
R
b)i
2
Rr0
2
p3 (2) 1.5 j
2
R () 2 2p j25 / 2
E peak eff 25n
109 j 8 / 7keV 350keV
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 12
Condition for the realization of the SWFA regime
N(R) 2ct pR
2 2 1
E(R) E(R0 )F(R)
N(R) E(R)
Ep
prec
F(R) e
n0R0 1R0
R0 (R)
R02 1 R0
R0(R)
2
Precursor Photon interaction condition
Energy Attenuation
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 13
Prediction (1) X-ray light curve for prompt and afterglow emission
(R. Willingale astro-ph/0612031)
secs after peakErgs cm-2s-1 0.3-10 keV
TaTp
n0(R0 )
n(Ra )i)
ii)
Tp R0
2
24c
a 1
2 p
p n0R0 T
n0 1.61014 p2m 3
R0 61013 p 1m
2 10 4 Tp p
1 z
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 14
Prediction (2)
Spectral geometrical correlation:
Ep T
1 z
4
7
Eiso T
1 z
27
28
Spectral-Energy correlation:
Eiso0.59
Ep cost (Amati relation: )
(L. Amati Il Nuovo Cimento)
Eiso0.58
Ep cost
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 15
Predictions (3)
Low Ep
GRB
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 16
Predictions (4)
Low Ep
GRB
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 17
Conclusions
Jetted structure of GRB Presence of Material around GRB Compton tail measurement Plasma acceleration mechanism Laboratory vs Astrophysics Cosmology with Spectral – Energy correlations?
Backup
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 19
GRB tails
Connaughton (2002), ApJ 567, 1028 Search for Post Burst emission in prompt GRB energy
band Looking for high energy afterglow (overlapping with
prompt emission) for constraining Internal/External Shock Model
Sum of Background Subtracted Burst Light Curves Tails out to hundreds of seconds decaying as temporal
power law = 0.6 0.1 Common feature for long GRB Not related to presence of low energy afterglow
Guido Barbiellini GLAST Symposium Stanford, February, 7th 2007 20
WakeField Acceleration
(Ta Phuoc et al. 2005)
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