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Upsilon production and decay to UHECR neutrinos from GRB and AGN associated
with strong magnetic field
International Workshop on Heavy Quarkonia 2008International Workshop on Heavy Quarkonia 20082-5 December 2008, Nara Women's University2-5 December 2008, Nara Women's University
Taka Kajino
National Astronomical ObservatoryDepartment of Astronomy, University of Tokyo
with A. Tokuhisa, K. Kojima (Tokyo), T. Yoshida (NAO)M. A. Famiano (Western Michigan), G. J. Mathews (Notre Dame)
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There are many astrophysical sites associated with strong
magnetic fields
Pulsars, GRBs, Magnetars, AGNs, …, etc.
Such environments can lead to the acceleration of Energetic Protons!
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supernova remnants wind supernovae AGN, GRB ?
(extra-Galactic?)
Spectrum of UHECRs and its Origin
=2.7
=3
GZK cut offN + CMB → N’+
4x10 19 eV
~ ~
(Sigl, NOW2006)
Neutrino ?
e
: -neutrino !
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Basic Idea and Purpose
Meson Synchrotron Emission
Decay
, e + e ー
~ TeV neutrinos
Decay-
bb
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High energy protons precessing along magnetic field lines emit synchrotron radiation.
When a particle is accelerated in an external field it can emit any quanta corresponding to the interactions of the particle.
Can emit: photons, gravitons, scalar and vector mesons, … EM Gravity Strong Interaction
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Meson Synchrotron Emission2nd Quantization of Meson Field
g = Strong Coupling Const.
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Three generations of quarks & leptons
u c t e d s b e
(1S-4S) = bb
Upsilon, a neutral vector meson,is a heavy quarkonium which can decay to lepton pairs:
(1S-4S) e
(2.2x10-6s) Large E.-Loss e
(2.9x10-13s) e
m 2m
1.777 3.554 Mass (GeV) 1.969 3.097 3.686 9.469 10.58 Ds
+(cs) 1S(cc) 2S(cc) 2S(bb) 4S(bb)
Kajino, Tokuhisa, Kojima, Yoshida, Famiano & Mathews (2008)
Waxman & Bahcall (1997)
2nd order
1st order
Botomium
b b
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Meson Energy Spectra
(1S)
photon
log(E) (eV)
log(
dI/d
E)
(s-1)
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(1S) Meson Intensities
(1S) meson
(1S) from protons
log(Etot)
log(
I) (
eV s
-1)
(1S) from iron
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Meson Intensities
(1S), (2S), (3S)
photon
log()
log(
I) (
eV s
-1)
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M.Boratav
1st Order Fermi Shock Accelaration
∝E-q (2<q)
When the gyroradius rgyro becomes comparable to the shock size L,the spectrum cuts off.
rgyro = mv/QB ~ L
log L
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-meson dom
inance
Meson synchrotron emission can exceed photon emission !
dominance
dominance
Upsilon-meson dom
inance
-meson dom
inance
dominance
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Meson Decay Mode to Three Flavor Lepton Pairs
, e + e ー
Lepton Decay Mode to Neutrinos
h (49.5%)
3x (15.3%)
loses large energybefore decay.
Soft sepectrum
loses small energybefore decay.
Hard spectrum
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Cooling of + - and + - by synchotron photon radiation before decay to neutrinos
+ - lepton
+ - leptontcool
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e -spectra from (1S) Decay
8 10 12 14 16 18 20
-10
-15
-20
-25
-30
-35
- e - e
- e - e
- -
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Neutrino Owscillation
e
de
dr1
-1
tan2θ >> λm, res = Δm2c3sin22θ
4h
Adabatic Condition for MSW Resonance (Matter Effect)
breaks down for neutrinos of =1010-1020eV Non-Adiabatic
No difference between and sectors.No difference between Normal and Inverted Mass-Hierarchies.
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Without -Oscillation
1 : 1 : 0 1 : 1 : 6
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With -Oscillation
4 : 3 : 3 2 : 2 : 1
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There is a Signature of Neutrinos from Meson Synchrotron Emission.
3 : 3 : 4 (1012eV < E)
1 : 2 : 2 (E < 1012eV)
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Event Rate number of neutrinos
produced per event
Events detected
Detection efficiency
Ahrens (2003)
High energy synchrotron neutrinos from a SGR burst might be detectable if relatively near by.
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Some astrophysical objects with strong magnetic fields are Some astrophysical objects with strong magnetic fields are
viable sites for strong meson synchrotron emission viable sites for strong meson synchrotron emission
This process can be more efficient than other processes for This process can be more efficient than other processes for producing heavy mesons like J/producing heavy mesons like J/ and Upsilon as well as and Upsilon as well as pions by high energy protons. pions by high energy protons.
A difference in the spectra between the A difference in the spectra between the , , , and e-type , and e-type neutrinos could be a unique signature that meson synchrotron neutrinos could be a unique signature that meson synchrotron radiation has actually taken place.radiation has actually taken place.
If a SGR burst occurs within ~ 1 kpc, high energy neutrinos If a SGR burst occurs within ~ 1 kpc, high energy neutrinos might be observable.might be observable.
ConclusionsConclusions