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L. Amati, G. Barbiellini , A Celotti, A. Galli, R. Landi, F. Longo, N. Omodei, M. Tavani

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. Bright and Dim GRB. Q = cts/peak cts. (Connaughton 2002). BRIGHT GRB  DIM GRB.

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L. Amati, G. Barbiellini , A Celotti, A. Galli, R. Landi, F. Longo, N. Omodei, M. Tavani

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  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 Q = cts/peak cts (Connaughton 2002) • 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 >1.5 cm-2 s-1 • Mean Fluence 1.5  10-5erg cm-2 • Q = 4.0  0.8 10-4 (5 ) fit over PL •  = 1.3 • Dim bursts (tail at 300s) • peak counts < 0.75cm-2 s-1 • Mean fluence 1.3  10-6erg 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) Electron Spectrum Emitted Photon 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 Q+=enr03~n0 (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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