1. GRB 050315: A step in the proof of the uniqueness of the overall GRB structure R. Ruffini, M.G. Bernardini, C.L. Bianco, L. Caito, P. Chardonnet, F. Fraschetti, R. Guida, G. Vereshchagin, S.-S. Xue Thursday 8 th June 2006 San Servolo Island – Venice – Italy

2. The energetics of our GRB model All GRBs, short and long, are produced by the gravitational collapse to a black hole. The energy source is the Blackholic energy: the Coulomb energy extractable from the black hole. Maximum energy extractable 1.8·10 54 (M BH /M Sun ) ergs (no need of beaming for energetics!) The energy extraction occurs by the vacuum polarization process in a supercritical electromagnetic field leading to the e + e - pair creation in the dyadosphere of the black hole generating an optically thick e + e - plasma which self-accelerates out of the black hole. Damour, Ruffini, Phys.Rev.Lett., 35, 463, (1975) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L113, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, Cosmology and Gravitation, AIP, (2003)

3. The free parameters of our model Characterizing the source: The energy of the dyadosphere E dya. The baryonic matter B = M B c 2 /E dya < 10 -2. Characterizing the environment: The ISM distribution (n ism, R = A em /A tot )

4. The emission process in the extended afterglow phase Special relativistic equations of motion in spherical symmetry (no r -3/2 power-law) Full shape of the Equitemporal Surfaces Observed spectrum as a double convolution of an infinite number of thermal spectra in the co-moving frame. Bianco, Ruffini, ApJ, 633, L13, (2005) Bianco, Ruffini, ApJ, 620, L23, (2005) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Bernardini, Bianco, Chardonnet, Fraschetti, Ruffini, Xue, ApJ, 634, L29 (2005)

5. - Relative Space Time Transformations (RSTT) paradigm (Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L107, 2001) - Interpretation of the Burst Structure (IBS) paradigm (Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L113, 2001) - GRB-supernova Time Sequence (GSTS) paradigm (Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L117, 2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, Int. Journ. Mod. Phys. D, 12, 173, (2003) Summary of our Model (tested on GRB 991216) E dya = 4.8x10 53 ergB = 3.0x10 -3

6. BATSE noise level P-GRB Afterglow Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 555, L113, (2001) Ruffini, Bianco, Chardonnet, Fraschetti, Xue, ApJ, 581, L19, (2002) Ruffini, Bianco, Chardonnet, Fraschetti, Vitagliano, Xue, Cosmology and Gravitation, AIP, (2003) GRB991216

7. GRB 050315: BAT + XRT Light curve Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press. Afterglow P-GRB (not shown) Prompt Emission (afterglow peak)

8. GRB 050315: BAT Light curve (15-25 keV) Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press. Afterglow

9. GRB 050315: BAT Light curve (25-50 keV) Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press. Afterglow

10. GRB050315: BAT Light curve (50-100 keV) Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press. Afterglow

11. GRB 050315: BAT Light curve (15-350 keV) Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press. Afterglow P-GRB

12. GRB 050315: Instantaneous spectra Ruffini, Bernardini, Bianco, Chardonnet, Fraschetti, Guida, Xue, ApJ Lett., in press.

13. Conclusions on GRB 050315 Thanks to the Swift data, with GRB 050315, for the first time, we reconstruct the complete afterglow in 5 energy bands, including the prompt emission in the early phases, all the way to the latest phases of the afterglow. The prompt emission is not due to the prolonged activity of an inner engine, but corresponds to the emission at the peak of the afterglow. The theoretical prediction on the P-GRB energy 1.98×10 51 erg and its temporal separation from the peak of the afterglow t a d = 51 s are in agreement with the observational data. The afterglow canonical behavior observed by Swift, showing an initial very steep decay followed by a shallow decay and finally a steeper decay, as well as the time structure of the prompt emission, have been related to the fluctuations of the ISM density and of the R parameter.

14. More general conclusions Additional work has to be done on the structure of the P-GRB in relation to the inner engine. (see Poster n. 190 by Xue et al.) A clear enhancement of the P-GRB with respect to the afterglow for different values of the baryon loading has been shown in GRB 970228. (see Poster n. 172 by Ruffini et al.) The flares observed in the X-ray afterglows of many GRBs can be related as well to inhomogeneities in the ISM. (see Poster n. 104 by Bianco et al.)

15. Even more general conclusions The Kouveliotou – Tavani classification of short and long bursts. The Amati relation. The Ghirlanda relation. Lowering the threshold, we need to reconsider: