Download - THE CANNONBALL MODEL AND SHORT HARD BURSTS
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 .