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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.

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Presentation on theme: "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."— Presentation transcript:

1 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, 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 Dar, Laor & Shaviv, Phys. Rev. Lett. 1998; Dar, Global Catastrophic Risks (Oxford Univ. Press 2008) Dado & Dar, in preparation

2 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 Jet of CBs ICS of Stellar Light/Glory GRB/XRF /SHB CR burst (CRB) Scattering of ISM The cannonball (CB) model of GRBs/XRFs/SHBs/CRBs Magnetic Scattered light from the wind of the progenitor star or a companion star, or an accretion disk Shaviv & Dar 1995: wind/ejecta (Dar et al. 1992) glory photons

3 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 From high resolution radio, optical and X-ray observations:

4 Deceleration of relativistic CBs with moon-like mass fired by the Microquasar XTE J1550-564 in 8/1998 observed with the X-ray observatory Chandra (Corbel et al. 2003) flare up when a CB collides with CB collides with a density bump? Bipolar jets of cannonballs of ordinary matter ejected in mass accretion episodes onto stellar mass black holes or neutron stars Microquasars are Cosmic Cannons

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

6 CBs fired by the microquasar XTE J1550-564 seen in X-rays by Chandra (Corbel et al. 2002) 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) winds blown by a progenitor star, a binary companion, or an accretion disk 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 In the CB model:

7 Merger of neutron stars and of a 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) Collapse of 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 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) SHBs: Progenitors and origin SGRs: SHBs: 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

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

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

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

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

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

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

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 ) practically constant until  AG break at which depends on the viewing angle Constant CB Radius, Constant ISM Density, Swept in ISM + Energy–Momentum Conservation beyond which they approach behaviour Plateau 

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

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)arXiv:0807.1962


22 ICS Delayed GeV-TeV Photons From Relativistic Cannonballs Lab Frame CB’s Rest Frame Magnetic Isotropization of HE e’s CB Lab Frame e e Inverse Compton scattered of glory photons Dado & Dar 2006: Double Peak with a second Ep

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

24 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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