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

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

Bipolar jets fired in mass accretion episodes on compact objectsBipolar jets fired in mass accretion episodes on compact objects(e.g., fall-back matter in SNe(e.g., fall-back matter in SNe, microquasars, n*-n* mergers, phase , microquasars, n*-n* mergers, phase transition in compact stars) produce transition in compact stars) produce GRBsGRBs/SHBs by ICS of light/SHBs by ICS of light

Jet of CBsJet of CBs

ICSICS of Stellar Light/Gloryof Stellar Light/GloryGRB/XRFGRB/XRF/SHB/SHBCR burst (CRB)CR burst (CRB)

Scattering of Scattering of ISMISM

The cannonball )CB( model of GRBs/XRFs/SHBs/CRBs

Magnetic

Scattered light from thewind of the progenitorstar or a companion star,

or an accretion disk

Shaviv & Dar 1995Shaviv & Dar 1995::

wind/ejecta

(Dar et al. 1992)

glory photons

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:

Deceleration of relativistic CBs with moon-like mass fired by the Microquasar XTE J1550-564 in 8/1998observed with the X-ray observatory Chandra

(Corbel et al. 2003)

flare up when aflare up when a CB collides withCB collides with

a density bumpa 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

Two CBs fired by SN1987A

53103

ergs53103E

Approaching CB(superluminal )

Receding CB

SN1987A

Nisenson & Papaliolios, ApJ, 518, L29 )1999(

Release: ergs

ergsjet

ergsejecta51

k

51k

10][E

10][E

Converted to Energy of Cosmic Ray Beamand Gamma Ray Burst

CBs fired by the microquasar XTE J1550-564 seen in X-raysby 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 bya 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:

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 stardue 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 clusterAfterglow Emission: SR from CBs in the ISM outside the cluster

s 100103/~/r~ESC)(

ms 30103/10~/r~SHB)(16

00c

161500g

pcct

ct

The Dominant Emission Mechanisms

in the CB Model

ICS of Light/Glory:

Synchrotron Radiation:Prompt UVO emission

Broad-band AGs SR Flares

Pulse ShapeSpectrumSpectral evolutionPolarization

Correlations between PE ObservablesSub-GeV toTeV photons )Double-Peak (

Light-curves SpectrumSpectral evolutionPolarization

Correlations with GRB Observables

F

Delayed sub-TeV to PeV photons No detectable neutrino fluxesHadronic production:

0

Prompt /X - ray emission

)1/()cos1(E ' z

3E iso pz E)1(

3/1

3/2

)E(~E)1(/1

)E(~E)1(/1

isop

isop

z

z

ICS correlations between:

E

glory

17.00.52/31/3' Eiso~2/](Eiso/Eo)[(Eiso/Eo)pEEpz)(1

CB

ee '

)1/(2cos1(/1 22

)1/(δL 4p z

; EL)1( 4/3iso

2 pzFor each CB peak:

t,L,E,E pisop

Where:

/z)t(1t 'obs

DD 2000( arXiv:astro-ph/0012227 :)

pobs 1/Et

Mot probable angle

Off-axis

Amati Correlation 2002

CB model interpolation formula

CB Model:

2/](Eiso/Eo)[(Eiso/Eo)pEEpz)(1 2/31/3

(DD2000 )

T-Ep, Ep-EisoEp-Lp, Eiso-Lp

Correlationswere predicted by

the CB model

Z=6.69080913

2// )1(~

p

p

EEEE

p E

Eebe

E

Ea

dE

dNE pp

g

ICS of thin thermal brem.

22

2

)0()(p

ppp

tt

tEtE

17.2~p

GRB/SHB Spectrum/Spectral Evolution

)1/(~)0( zE gp

Ep

)][/( / gg

geddn

)( ppp tEE

Fermi accelerated.Bethe-Bloch KO e’sCB Inert e’s

)(~

)/()(

2)0(/2

2/1

)(/

222

222

tEFedEdt

NdEE

eEEt

t

dEdt

NdE

p

pg

EE

tEEp

Approximate ICS Pulse Shape:

FWHM30.0RT

E2FWHM

E)(tt1/2-

0p

a

/RR2

Tγ

σ

]e[1πRσ

dt

dN22

tr

`FRED’ Shape, time lag proportional to width very small for SHBs

with Etof functiona ely approximat isflux energy theE2For E 2p

CB Model Light Curve of LGRB 990123

)(/14

4

2

)(/2)(/1

2

22

1

2

~)( keV 3.0

~keV 10)(keV 3.0

~keV 10)(

: decline emission-prompt of behaviours typicalThree

][)(

tEEp

p

p

tEEtEEpE

E

p

pp

etEFtE

tEFtE

tEFtE

eet

tEdE

dEdt

NdEEF

Decline of the prompt emission

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

-2t

-2t

-4t

2pp

2 tE2/tE-4t e

2pp

2 tE2/tE-4t e

bt

photon spectral index

DD: arXiv:0807.1962( ApJ 2009)

SR

ICS

ICS

ICS

ICSSR

SR

SRSR

Host GalaxyAG

Ep)t(

DD: arXiv:0812.3340 )ApJ 2009(

photon spectral index

GRB 060614: z =0.125, No SN, off-axis SHB?

SR

SR

SR

ICS

ICS

The Synchrotron Radiation from CBs

In the CB’s rest frame:

2γmcE ISM particles enter with energycreate a turbulent equipartition magnetic field The swept-in ISM particles are Fermi accelerated

The accelerated e’s emit synchrotron radiation:

2.2~p Hz,z1

δγn102.68(t)νFor

ν

ν1

ν

ν

νD4

δγcmnηπR(t)F

31/2p5

b

1)/2(p

b

1/2

bb2L

423ee

2

ν

X

1Γ2Γ43ΓΓ/22ν νδγnR)(F t

Rise Fast Decay Plateau gradual break power-law decay

1.2~

Deceleration of CBs( observed from an angle )

sec)1(

103.18

)1(

)1(

]/)1[(

212

33

2142

50330

20

0222

0

220

2/10

2220

0

0

220

2

0220

4

0

Rn

Nz

Rcn

Nzt

tt

tt

t

t

b

b

)(),( tt 0222

0 )1( ttt break practically constant until

AG break at which depends on the viewing anglebreakt

Constant CB Radius, Constant ISM Density, Swept in ISM

+Energy–Momentum Conservation

beyond which they approach behaviour1/4tγδ

Plateau 1Γ1/2-Γ1Γ24Γ νt~νγ :(t)Fν

:γ(t)

Data:Kuin et al. 2009 Data: GCNs

2exp

2

)1(/

tt

teF

ta

Early –time SR lightcurvesData: Racusin et al. 2008

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

ICS Delayed GeV-TeV Photons From Relativistic Cannonballs

Lab Frame

CB’s Rest Frame

Magnetic Isotropization of HE e’s

0

CCBB

Lab Frame

10γ~θ

e

e

Inverse Compton scattered of glory photons

MeV/keV)z)(E0.75(1/4εz)E3(1E

TeV~ε(4/3)γE(glory)γ'(ISM)e'2

p1g2p1p2

g4

γ

Dado & Dar 2006: Double Peak with a second EpννF

mγE 0'e

Sub-TeV sub-PeV Photons (?) and Neutrinos

Lab Frame

CB’s Rest Frame

HECRs

0

CCBB

Lab Frame

10γ~θ

p

p

Inverse Compton scattered of glory photons

PeV1.0~ E2 X;p(CB)(CB)p

PeV1.0~ E2 X;p(ISM)p

0.1TeV~ E2 X;p(ISM)p(CB)

0CR

0CR

0

Dar & De Rujula 2000, 2006 )arXiv:hep-ph/0606199, Phys. Rep. 466, 179-241, )2008((

p0'p mγE p’

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 .