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Where do we stand

Where do we stand. ?. Log(Flux ). Swift. End of the prompt. A few hours. Log(Time ). Kyoto 2010. Log(Flux ). X-Ray Flares. Log(Time ). Kyoto 2010. GRB X- ray Flares. R. Margutti G. Chincarini , G. Bernardini , J. Mao, C. Guidorzi. Early-time flare catalog .

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Where do we stand

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  1. Where do we stand ? Log(Flux) Swift End of the prompt A few hours Log(Time) Kyoto 2010

  2. Log(Flux) X-Ray Flares Log(Time) Kyoto 2010

  3. GRB X-ray Flares R. Margutti G. Chincarini, G. Bernardini, J. Mao, C. Guidorzi Early-time flare catalog Late-time flare catalog Bright flare analysis t< 103s t> 103s 9 flares X-ray + gamma-ray Very good statistics 113 flares 4 different energy bands Asymmetric profile 36 flares Asymmetric profile Evolution with time (up to t≈106 s) 051117A Spectral evolution Evolution with energy band Poster: # Evolution with time Evolution with energy band Margutti et al., MNRAS accepted, Astro-ph: 1004.1568 Astro-ph: 1004.0901 As-complete-as-possible observational picture of the X-ray flare phenomenology AIM: Kyoto 2010

  4. ? GRB X-ray Flares OBSERVATIONALLY: What distinguishes a flare from a prompt pulse Do flares follow the entire set of temporal and spectral relations found from the analysis of prompt emission pulses? Width(T) Luminosity(T) Ep(t) Ep(t)-Liso(t) Ep-Liso Width(E) Lag-Lum Kyoto 2010

  5. The Method: Trise Tdecay Width Tpeak Amplitude If with redshift: Peak Luminosity Energy Evolution with ENERGY BAND Evolution with Tpeak GRB060904B Among different flares In the same flare Kyoto 2010

  6. Width (t) Width=trise+tdecay Width=trise + tdecay Log(width) Log(tpeak) TIME Kyoto 2010

  7. Luminosity (t) Flares get fainter and fainter Early time sample TIME Kyoto 2010

  8. Spectral Evolution (t) 060904B Flare: Prompt: BATSE pulse Peak Energy Time (Peng 2009) Within single flare and pulses TIME Kyoto 2010

  9. Ep(t)-Liso(t) Ep,i (keV) Ep,i (keV) 060904B Flare 060418 Flare Liso (erg/s) Liso (erg/s) Prompt Ep,i (keV) Ghirlanda 2010 Liso (erg/s) Kyoto 2010

  10. Ep-EisoEp-Liso Prompt data from Nava 2009 Flares Flares Kyoto 2010

  11. Width(E) FLARES PROMPT High energy profiles peak before Flare peak Lag Kyoto 2010

  12. Lag-Luminosity PROMPT CCF lag, time integ. 50-100 vs 100-200 keV 1-10000 keVLpeak (Ukwatta 2010) Norris 2000 relation Peak lag, flares 0.3-1vs 3-10 keV 0.3-10 keVLpeak (Margutti 2010) FLARES Kyoto 2010

  13. Summary: Flares paradigm High energy flareprofiles rise faster, decay faster and peak before the low energy emission. FLARES EVOLVE WITH TIME As time proceeds flares become wider, with larger peak lag, lower luminosities and softer emission. Kyoto 2010

  14. Summary: FLARES EVOLVE WITHTIME Margutti 2010 FLARES PROMPT Width(T) Luminosity(T) Ep(t) Ep(t)-Liso(t) Ep-Liso Width(E) Lag-Lum ≈const ≈const ≈similar ? Kyoto 2010 Astro-ph: 1004.1568 Astro-ph: 1004.0901

  15. THANK YOU!! Kyoto 2010

  16. Back-up slides

  17. Lag - HR

  18. HRrise-HRdecay

  19. Energy dependence of the parameter

  20. Lpeak-Width

  21. Trise-tdecay

  22. Ioka plot

  23. Flare and prompt energy

  24. SED

  25. BAT-XRT spectral index BAT XRT

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