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Relativistic interaction of a high intensity photon beam with a plasma: a possible GRB emission mechanism

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Title: Relativistic interaction of a high intensity photon beam with a plasma: a possible GRB emission mechanism


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
2
Bright and Dim GRB
  • (Connaughton 2002)

Q cts/peak cts
  • BRIGHT GRB
  • ? DIM GRB

3
The Compton Tail
Barbiellini et al. (2004) MNRAS 350, L5
4
The Compton tail
  • Prompt luminosity
  • Compton Reprocessed luminosity
  • Q ratio

5
Bright and Dim Bursts
  • Bright bursts (tail at 800 s)
  • Peak counts gt1.5 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 lt 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 cm ?R R ? 0.1
6
WakeField Acceleration
(Ta Phuoc et al. 2005)
Laser Pulse tlaser 3 10-14 s Laser Energy 1
Joule Gas Surface 0.01 mm2 Gas Volume Density
1019 cm3 Power Surface Density ?W 3 1018 W
cm-2
7
WakeField Acceleration
(Ta Phuoc et al. 2005)
Emitted Photon Spectrum
Electron Spectrum
Simulated Photon Spectrum
8
Scaling relations
?p n-1/2
?b n-1/2?1/2
r0 n-1/3 ??1/2
9
Scaling relations
V r03 n-1 Qenr03n0
?(1019) 102 ?(109) 2x105 ?(102) 2x108
?n-1/3 Ep 3/4 hcg2 r0/?p2
10
3D PIC Simulation
  • PhD Thesis Marco Galimberti 2003 Pisa

11
GRB Gamma Emission in the stochastic wake field
acceleration regime
From the equation of the electron energy loss we
derive
Imposing Re R?, we link the jet angle to an
energy threshold ?t
The previous relations allow the prediction of
the typical energy emission
12
Condition for the realization of the SWFA regime
Precursor Photon interaction condition
Energy Attenuation
13
Prediction (1)
  • X-ray light curve for prompt and afterglow
    emission
  • (R. Willingale astro-ph/0612031)

Ergs cm-2s-1 0.3-10 keV
secs after peak
i)
ii)
14
Prediction (2)
  • Spectral geometrical correlation
  • Spectral-Energy correlation

(Amati relation ) (L. Amati Il
Nuovo Cimento)
15
Predictions (3)
Low Ep GRB
16
Predictions (4)
Low Ep GRB
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?

18
Backup
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

20
WakeField Acceleration
(Ta Phuoc et al. 2005)
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