11

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)

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!

33

　　

　　

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 !

Basic Idea and Purpose

Meson Synchrotron Emission

Decay

, e ＋ e ー

~ TeV neutrinos

Decay－

bb

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

Meson Synchrotron Emission2nd Quantization of Meson Field

g = Strong Coupling Const.

77

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

Meson Energy Spectra

(1S)

photon

log(E) (eV)

log(

dI/d

E)

(s-1)

(1S) Meson Intensities

(1S) meson

(1S) from protons

log(Etot)

log(

I) (

eV s

-1)

(1S) from iron

Meson Intensities

(1S), (2S), (3S)

photon

log()

log(

I) (

eV s

-1)

11

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

-meson dom

inance

Meson synchrotron emission can exceed photon emission !

dominance

dominance

Upsilon-meson dom

inance

-meson dom

inance

dominance

1313

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

Cooling of + - and + - by synchotron photon radiation before decay to neutrinos

+ - lepton

+ - leptontcool

16

e -spectra from (1S) Decay

8 10 12 14 16 18 20

-10

-15

-20

-25

-30

-35

－ e － e

－ e － e

－ －

17

　

　

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.

18

　

　

Without -Oscillation

1 : 1 : 0 1 : 1 : 6

19

　

　

With -Oscillation

4 : 3 : 3 2 : 2 : 1

There is a Signature of Neutrinos from Meson Synchrotron Emission.

3 : 3 : 4 (1012eV < E)

1 : 2 : 2 (E < 1012eV)

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.

2222

　　

　　 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