1. 1 Upsilon production and decay to UHECR neutrinos from GRB and AGN associated with strong magnetic field International Workshop on Heavy Quarkonia 2008 2-5 December 2008, Nara Women's University Taka Kajino National Astronomical Observatory Department of Astronomy, University of Tokyo with A. Tokuhisa, K. Kojima (Tokyo), T. Yoshida (NAO) M. A. Famiano (Western Michigan), G. J. Mathews (Notre Dame)

2. 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!

3. 3 supernova remnants wind supernovae AGN, GRB ? (extra-Galactic?) Spectrum of UHECRs and its Origin  =2.7  =3 GZK cut off N +  CMB → N’+  4x10 19 eV (Sigl, NOW2006) Neutrino ?   e  ：  -neutrino !

4. Basic Idea and Purpose Meson Synchrotron Emission Decay, e ＋ e ー ~ TeV neutrinos Decay － bb

5. 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

6. Meson Synchrotron Emission 2nd Quantization of Meson Field g = Strong Coupling Const.

7. 7 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 -6 s ) Large E.-Loss  e   ( 2.9x10 -13 s )   e m  2m  1.777 3.554 Mass (GeV) 1.969 3.097 3.686 9.469 10.58 D s + (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

8. Meson Energy Spectra  (1S)   photon log(E) (eV) log(dI/dE) (s -1 )

9.  (1S) Meson Intensities  (1S) meson  (1S) from protons log(E tot ) log(I) (eV s -1 )  (1S) from iron

10. Meson Intensities  (1S),  (2S),  (3S)   photon log(  ) log(I) (eV s -1 )

11. 11 M.Boratav 1st Order Fermi Shock Accelaration  ∝ E -q (2<q) When the gyroradius r gyro becomes comparable to the shock size L, the spectrum cuts off. r gyro = mv/QB ～ L log L

12.  -meson dominance Meson synchrotron emission can exceed photon emission !  dominance Upsilon-meson dominance  -meson dominance  dominance

13. 13 Meson Decay Mode to Three Flavor Lepton Pairs, e ＋ e ー Lepton Decay Mode to Neutrinos h   (49.5%) 3x  (15.3%)    loses large energy before decay. Soft  sepectrum   loses small energy before decay. Hard  spectrum

14. Cooling of  + - and  + - by synchotron photon radiation before decay to neutrinos  + - lepton    + - lepton t cool  

15. 15  lepton flux  + - lepton

16. 16   e -spectra from  (1S) Decay 8 10 12 14 16 18 20 -10 -15 -20 -25 -30 -35  －  e － e   －  e － e   －   －  

17. 17 Neutrino Owscillation ee dede dr 1 tan2  >>  m, res = Δ m 2 c 3 sin 2 2  4h   Adabatic Condition for MSW Resonance (Matter Effect) breaks down for neutrinos of  =10 10 -10 20 eV Non-Adiabatic No difference between and sectors. No difference between Normal and Inverted Mass-Hierarchies.

18. 18 Without -Oscillation 1 : 1 : 0 1 : 1 : 6

19. 19 With -Oscillation 4 : 3 : 32 : 2 : 1

20. There is a Signature of Neutrinos from Meson Synchrotron Emission. 3 : 3 : 4 ( 10 12 eV < E ) 1 : 2 : 2 ( E < 10 12 eV )

21. 21 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.

22. 22 Some astrophysical objects with strong magnetic fields are viable sites for strong meson synchrotron emission Some astrophysical objects with strong magnetic fields are viable sites for strong meson synchrotron emission This process can be more efficient than other processes for producing heavy mesons like J/  and Upsilon as well as pions by high energy protons. This process can be more efficient than other processes for producing heavy mesons like J/  and Upsilon as well as pions by high energy protons. A difference in the spectra between the , , and e-type neutrinos could be a unique signature that meson synchrotron radiation has actually taken place. A difference in the spectra between the , , and e-type neutrinos could be a unique signature that meson synchrotron radiation has actually taken place. If a SGR burst occurs within ~ 1 kpc, high energy neutrinos might be observable. If a SGR burst occurs within ~ 1 kpc, high energy neutrinos might be observable. Conclusions