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,

Slides:

Advertisements

Similar presentations

Lecture 5: Gamma-Ray Bursts Light extinction:. GRBs are brief flashes of soft -ray radiation ( 100 keV), discovered in the 1970s, the origin of which.

Advertisements

Vanessa Mangano - Venice 2006 Rest frame light curves of Swift GRBs Vanessa Mangano, Giancarlo Cusumano, Valentina La Parola, Eleonora Troja, Teresa Mineo.

Some issues on models of black hole X-ray binaries Feng Yuan Shanghai Astronomical Observatory, Chinese Academy of Sciences.

GRB : a canonical fake short burst L. Caito, M.G. Bernardini, C.L. Bianco, M.G. Dainotti, R. Guida, R. Ruffini. 3 rd Stueckelberg Workshop July 8–18,

The Science of Gamma-Ray Bursts: caution, extreme physics at play Bruce Gendre ARTEMIS.

Klein-Nishina effect on high-energy gamma-ray emission of GRBs Xiang-Yu Wang ( 王祥玉） Nanjing University, China （南京大學） Co-authors: Hao-Ning He (NJU), Zhuo.

Bruce Gendre Osservatorio di Roma / ASI Science Data Center Recent activities from the TAROT/Zadko network.

Yun-Wei YU 俞云伟 June 22, 2010, Hong Kong. Outline  Background  Implications from the shallow decay afterglows of GRBs  A qualitative discussion on magnetar.

Low-luminosity GRBs and Relativistic shock breakouts Ehud Nakar Tel Aviv University Omer Bromberg Tsvi Piran Re’em Sari 2nd EUL Workshop on Gamma-Ray Bursts.

Low-luminosity GRBs and Relativistic shock breakouts Ehud Nakar Tel Aviv University Omer Bromberg Re’em Sari Tsvi Piran GRBs in the Era of Rapid Follow-up.

GRB afterglows in the Non-relativistic phase Y. F. Huang Dept Astronomy, Nanjing University Tan Lu Purple Mountain Observatory.

Very High Energy Transient Extragalactic Sources: GRBs David A. Williams Santa Cruz Institute for Particle Physics University of California, Santa Cruz.

GRB Afterglow Spectra Daniel Perley Astro September* 2005 * International Talk Like a Pirate Day.

Spectral Energy Correlations in BATSE long GRB Guido Barbiellini and Francesco Longo University and INFN, Trieste In collaboration with A.Celotti and Z.Bosnjak.

Gamma-Ray Bursts: The Most Brilliant Events in the Universe D. Q. Lamb (U. Chicago) PHYSICS for the THIRD MILLENNIUM: II Huntsville, AL 5–7 April 2005.

Temporal evolution of thermal emission in GRBs Based on works by Asaf Pe’er (STScI) in collaboration with Felix Ryde (Stockholm) & Ralph Wijers (Amsterdam),

Ehud Nakar California Institute of Technology Gamma-Ray Bursts and GLAST GLAST at UCLA May 22.

The general theory of relativity is our most accurate description of gravitation Published by Einstein in 1915, this is a theory of gravity A massive object.

Gamma Ray Bursts and LIGO Emelie Harstad University of Oregon HEP Group Meeting Aug 6, 2007.

Swift Nanjing GRB Conference Prompt Emission Properties of X-ray Flashes and Gamma-ray Bursts T. Sakamoto (CRESST/UMBC/GSFC)

SONG and mini-SONG Observations of GRB Pulsed Emission Jon Hakkila Presented at the 4th SONG Workshop September 17, 2011 Presented at the 4th SONG Workshop.

Jet Models of X-Ray Flashes D. Q. Lamb (U. Chicago) Triggering Relativistic Jets Cozumel, Mexico 27 March –1 April 2005.

COSMIC GAMMA-RAY BURSTS The Current Status Kevin Hurley UC Berkeley Space Sciences Laboratory.

July 2004, Erice1 The performance of MAGIC Telescope for observation of Gamma Ray Bursts Satoko Mizobuchi for MAGIC collaboration Max-Planck-Institute.

GRB s CENTRAL -ENGINE & FLARes WARSAW Guido Chincarini & Raffaella margutti 1WARSAW 2009.

Monte-Carlo Simulation of Thermal Radiation from GRB Jets Sanshiro Shibata (Konan Univ.) Collaborator: Nozomu Tominaga (Konan Univ., IPMU)

Rise and Fall of the X-ray flash : an off-axis jet? C.Guidorzi 1,2,3 on behalf of a large collaboration of the Swift, Liverpool and Faulkes Telescopes,

Gamma-Ray Bursts observed with INTEGRAL and XMM- Newton Sinead McGlynn School of Physics University College Dublin.

She-Sheng XUE ICRANet, Pescara, Italy how the gravitational energy transfers to the electromagnetic energy for Gamma-Ray-Bursts. 1) Electron-positron production,

Is the Amati relation due to selection effects? Lara Nava In collaboration with G. Ghirlanda, G.Ghisellini, C. Firmani Egypt, March 30-April 4, 2009 NeutronStars.

Tight correlations in ‘canonical’ lightcurves of Gamma Ray Bursts M.G. Dainotti 1, R. Willingale 2, V.F. Cardone 3, S. Capozziello 4, M. Ostrowski 1 Dainotti.

Extended emission in short gamma-ray bursts registered by SPI-ACS of INTEGRAL observatory Pavel Minaev 1, 2, Alexei Pozanenko 1, Vladimir Loznikov 1 1-

The Early Time Properties of GRBs : Canonical Afterglow and the Importance of Prolonged Central Engine Activity Andrea Melandri Collaborators : C.G.Mundell,

1 Physics of GRB Prompt emission Asaf Pe’er University of Amsterdam September 2005.

1 Determination of the equation of state of the universe using 0.1Hz Gravitational Wave Antenna Takashi Nakamura and Ryuichi Takahashi Dept. Phys. Kyoto.

A Tidal Disruption model for gamma-ray burst of GRB YE LU National Astronomical Observatories, Chinese Academy of Sciences June 22-27, 2008 Nanjing.

BH Astrophys. Ch3.6. Outline 1. Some basic knowledge about GRBs 2. Long Gamma Ray Bursts (LGRBs) - Why so luminous? - What’s the geometry? - The life.

Gamma-Ray Bursts Energy problem and beaming * Mergers versus collapsars GRB host galaxies and locations within galaxy Supernova connection Fireball model.

Gamma-Ray Bursts: Open Questions and Looking Forward Ehud Nakar Tel-Aviv University 2009 Fermi Symposium Nov. 3, 2009.

The peak energy and spectrum from dissipative GRB photospheres Dimitrios Giannios Physics Department, Purdue Liverpool, June 19, 2012.

Is GRB050509b a genuine short? Gustavo de Barros, Maria Grazia Bernardini, Carlo Luciano bianco, Roberto Guida, Remo Ruffini.

Stochastic Wake Field particle acceleration in GRB G. Barbiellini (1), F. Longo (1), N.Omodei (2), P.Tommasini (3), D.Giulietti (3), A.Celotti (4), M.Tavani.

Primordial black holes B. Czerny Copernicus Astronomical Center, Warsaw on behalf of collaboration: D. Cline, B. Czerny, A. Dobrzycki, A. Janiuk, C. Matthey,

Radiation spectra from relativistic electrons moving in turbulent magnetic fields ＹｕｔｏＴｅｒａｋｉ & Fumio Takahara Theoretical Astrophysics Group Osaka Univ.,

Moriond – 1 st -8 th Feb 2009 – La Thuile, Italy. Page 1 GRB results from the Swift mission Phil Evans, Paul O'Brien and the Swift team.

Chandra Searches for Late-Time Jet Breaks in GRB Afterglows David Burrows, Judith Racusin, Gordon Garmire, George Ricker, Mark Bautz, John Nousek, & Dirk.

Gamma–Ray Bursts, Massive Cores and Particle Physics Remo Ruffini Dipartimento di Fisica – Università di Roma “La Sapienza” ICRANet – Pescara ICRANet –

Gamma-Ray Burst Ring-shaped Jets And Their Afterglows Ming Xu Department of Astronomy, Nanjing University Gamma-ray Sky from Fermi: Neutron.

Francisco Virgili, LJMU June 22, 2012 GRBs 2012 Liverpool C. Mundell, A. Melandri, C. Guidorzi, R. Margutti, A. Gomboc, S. Kobayashi, V. Pal’shin, etc…

Gamma-Ray Bursts. Short (sub-second to minutes) flashes of gamma- rays, for ~ 30 years not associated with any counterparts in other wavelength bands.

A relation to estimate the redshift from the X-ray afterglow light curve Bruce Gendre (IASF-Roma/INAF) & Michel Boër (OHP/CNRS)

Alessandra Corsi (1,2) Dafne Guetta (3) & Luigi Piro (2) (1)Università di Roma Sapienza (2)INAF/IASF-Roma (3)INAF/OAR-Roma Fermi Symposium 2009, Washington.

MICHAEL ROTONDO* R. RUFFINI*°^ S-S. XUE*° *DEPARTMENT OF PHYSICS AND ICRA, UNIVERSITY OF ROME “SAPIENZA” °ICRANET, PESCARA ^ICRANET,UNIVERSITY OF NICE.

Physical parameters of the relativistic shells in the GRBs S. Simić 1, L. Grassitelli 2 and L. Č. Popović 3,4 1) Faculty of Science, Department of Physics,

Fermi GBM Observations of Gamma-Ray Bursts Michael S. Briggs on behalf of the Fermi GBM Team Max-Planck-Institut für extraterrestrische Physik NASA Marshall.

GRB and GRB A the flares and the spectral lag M.G. Dainotti M.G.Bernardini, C.L.Bianco, L. Caito, R. Guida, R.Ruffini.

Gamma-ray Bursts from Synchrotron Self-Compton Emission Juri Poutanen University of Oulu, Finland Boris Stern AstroSpace Center, Lebedev Phys. Inst., Moscow,

Stochastic wake field particle acceleration in Gamma-Ray Bursts Barbiellini G., Longo F. (1), Omodei N. (2), Giulietti D., Tommassini P. (3), Celotti A.

Radio afterglows of Gamma Ray Bursts Poonam Chandra National Centre for Radio Astrophysics - Tata Institute of Fundamental Research Collaborator: Dale.

A complete sample of long bright Swift GRBs: correlation studies Paolo D’Avanzo INAF-Osservatorio Astronomico di Brera S. Campana (OAB) S. Covino (OAB)

Gamma-ray bursts Tomasz Bulik CAM K, Warsaw. Outline ● Observations: prompt gamma emission, afterglows ● Theoretical modeling ● Current challenges in.

Sorting out GRB correlations with spectral peak David Eichler (presented by Jonathan Granot)

1 HETE-II Catalogue HETE-II Catalogue Filip Münz, Elisabetta Maiorano and Graziella Pizzichini and Graziella Pizzichini for HETE team Burst statistics.

She-Sheng XUE ICRANet, Pescara, Italy How the gravitational energy transfers to the electromagnetic energy for Gamma-Ray-Bursts. 1)Electron-positron production,

Gamma-ray bursts from magnetized collisionally heated jets

Le spectre des GRBs dans le modèle EMBH

Photosphere Emission in Gamma-Ray Bursts

Swift observations of X-Ray naked GRBs

Tight Liso-Ep-Γ0 Relation of Long Gamma-Ray Bursts

Stochastic Wake Field particle acceleration in GRB

Presentation transcript:

GRB : 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

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)

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 < Characterizing the environment: The ISM distribution (n ism, R = A em /A tot )

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)

- 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 ) E dya = 4.8x10 53 ergB = 3.0x10 -3

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

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

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

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

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

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

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

Conclusions on GRB Thanks to the Swift data, with GRB , 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.

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 (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.)

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: