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THE CANNONBALL MODEL AND SHORT HARD BURSTS

THE CANNONBALL MODEL AND SHORT HARD BURSTS. Arnon Dar. 44 th Rencontre De Moriond, La Thuile, Italy, February 1-8, 2009. Based on work done in collaboration with Shlomo Dado and Alvaro De Rujula. 0807.1962 (ApJ 2009) arXiv DD ,.

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THE CANNONBALL MODEL AND SHORT HARD BURSTS

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  1. THE CANNONBALL MODEL AND SHORT HARD BURSTS Arnon Dar 44th Rencontre De Moriond, La Thuile, Italy, February 1-8, 2009 Based on work done in collaboration with Shlomo Dado and Alvaro De Rujula 0807.1962 (ApJ 2009)arXiv DD, Part of a unified theory of high energy astrophysical phenomena (GRBs, XRFs, SHBs, Blazers, Microquasars, Cosmic Rays, Mass Extinctions) based on the cannonball (CB) model of high energy jets and their interactions Dar & De Rujula, Phsics reports 2004 Dado & Dar, ApJ 2009 Dado & Dar, in preparation Dar & De Rujula, Phsics reports 2004 Dar, Laor & Shaviv, Phys. Rev. Lett. 1998; Dar, Global Catastrophic Risks (Oxford Univ. Press 2008)

  2. ICSof Stellar Light/Glory CR burst (CRB) GRB/XRF/SHB The cannonball (CB) model of GRBs/XRFs/SHBs/CRBs Scattering of ISM Magnetic (Dar et al. 1992) wind/ejecta gloryphotons Jet of CBs Scattered light from the wind of the progenitor star or a companion star, or an accretion disk Shaviv & Dar 1995: Bipolar jets fired in mass accretion episodes on compact objects (e.g., fall-back matter in SNe, microquasars, n*-n* mergers, phase transition in compact stars) produce GRBs/SHBs by ICS of light

  3. From high resolution radio, optical and X-ray observations: Relativistic jets are highly collimated plasmoids made of ordinary matter (not conical shells made of e+e- plasma). Their radiation is produced mainly through interaction with the environment (not `internal collisions’). Quasar 3C175

  4. Bipolar jets of cannonballs of ordinary matter ejected in massaccretion episodes onto stellar mass black holes or neutron stars Microquasars are Cosmic Cannons Deceleration of relativistic CBs with moon-like mass fired by theMicroquasarXTEJ1550-564 in 8/1998 observed with the X-ray observatory Chandra (Corbel et al. 2003) flare up when a CB collides with a density bump?

  5. Two CBs fired by SN1987A Nisenson & Papaliolios,ApJ, 518, L29 (1999) ApproachingCB (superluminal) Release: ergs SN1987A Converted to Energy of Cosmic Ray Beam and Gamma Ray Burst RecedingCB

  6. In the CB model: SHBs are produced through ICS of light by the electrons in plasmoids fired by the central engine. The light can be that of a companion star or a glory - light scattered/emitted from CBs fired by the microquasar XTE J1550-564 seen in X-rays by Chandra (Corbel et al. 2002) winds blown by a progenitor star, a binary companion, or an accretion disk HST image of the glory (dust echo) of the stellar outburst of V383 Monocerotis on early January 2002 taken on 28 October 2003 (Bond et al 2003)

  7. SHBs:Progenitors and origin SHBs: Merger ofneutron starsand ofa neutron star and a black hole in compact binaries (Blinnikov et al. 1984, Paczynski 1986, Goodman, Dar and Nussinov 1987, Eichler et al. 1989) launch highly relativistic bipolar jets (Shaviv and Dar 1995, Dar 1998, Dar and De Rujula 2000) Collapseof compact stars (neutron stars, hyper stars, quark stars) to a more compact star due to mass accretion, and/or loss of angular momentum and/or cooling by radiation (Dar et al. 1992, Shaviv and Dar 1995, Dar 1998a,1999, Dar and De Rujula 2000) launch highly relativistic bipolar jets NORMAL ENVIRONMENT: Super star-cluster, Globular cluster SHB Production: ICS of glory light by highly relativistic CBs Extended Soft Component: SR/ICS from CBs crossing the cluster Afterglow Emission: SR from CBs in the ISM outside the cluster SGRs: Phase transitions inside compact stars, such as neutron-stars, hyper-stars and quark stars (Dar 1999, Dar and De Rujula 2000, Dar 2006) Accretion episodes in microblazars and intermediate mass black holes in dense stellar regions (Dar 1998,1999)

  8. The Dominant Emission Mechanisms in the CB Model ICS of Light/Glory: Prompt /X - ray emission Pulse Shape Spectrum Spectral evolution Polarization Correlations between PE Observables Sub-GeV toTeV photons (Double-Peak ) Prompt UVO emission Broad-band AGs SR Flares Synchrotron Radiation: Light-curves Spectrum Spectral evolution Polarization Correlations with GRB Observables Delayed sub-TeV to PeV photons No detectable neutrino fluxes Hadronic production:

  9. ICS correlations between: DD 2000 (arXiv:astro-ph/0012227): CB glory Where: CB Model: For each CB peak: Mot probable angle Off-axis CB model interpolation formula Amati Correlation 2002

  10. Z=6.69 080913 T-Ep, Ep-Eiso Ep-Lp, Eiso-Lp Correlations were predicted by the CB model (DD2000)

  11. GRB/SHB Spectrum/Spectral Evolution ICS of thin thermal brem. Fermi accelerated. Bethe-Bloch KO e’s CB Inert e’s Ep

  12. Approximate ICS Pulse Shape: `FRED’ Shape, time lag proportional to width  very small for SHBs

  13. CB Model Light Curve of LGRB 990123

  14. Decline of the prompt emission Swift repository (Evans et al. 2007) report energy flux light curves in the 0.3-10 keV band

  15. DD: arXiv:0812.3340 (ApJ 2009) ICS SR SR photon spectral index ICS ICS SR SR ICS SR DD: arXiv:0807.1962 (ApJ 2009)

  16. DD: arXiv:0812.3340 (ApJ 2009) GRB 060614: z =0.125, No SN, off-axis SHB ? ICS SR SR Host Galaxy AG photon spectral index Ep(t) ICS SR

  17. The Synchrotron Radiation from CBs In the CB’s rest frame: ISM particles enter with energy create a turbulent equipartition magnetic field The swept-in ISM particles are Fermi accelerated The accelerated e’s emit synchrotron radiation : Rise Fast DecayPlateau gradual break power-law decay

  18. Deceleration of CBs( observed from an angle ) Constant CB Radius, Constant ISM Density, Swept in ISM + Energy–Momentum Conservation practically constant until beyond which they approach behaviour Plateau  AG break at which depends on the viewing angle

  19. Data: Racusin et al. 2008 Early –time SR lightcurves Data:Kuin et al. 2009 Data: GCNs

  20. Comparison between X-ray light curves (Swift XRT repository, Evans et al. 2007) and their CB model description (DD ApJ 2009 (arXiv:0807.1962)

  21. ICS Delayed GeV-TeV PhotonsFromRelativisticCannonballs CB LabFrame CB’s Rest Frame e e Magnetic Isotropization of HE e’s LabFrame Inverse Compton scattered of glory photons Dado & Dar 2006: Double Peak with a second Ep

  22. Sub-TeV sub-PeV Photons (?) and Neutrinos Dar & De Rujula 2000, 2006 (arXiv:hep-ph/0606199, Phys. Rep. 466, 179-241, (2008)) CB LabFrame p’ CB’s Rest Frame p p HECRs LabFrame Inverse Compton scattered of glory photons

  23. Conclusions The numerous predictions of the cannonball model which were derived in fair approximations from underlying solid physical assumptions are simple and falsifiable. So far they agree well with the mounting data accumulated from space- and ground-based observations of GRBs, XRFs and SHBs.

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