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UHE NEUTRINOS: FROM CONVENTIONAL TO NEW PHYSICS

V. Berezinsky

INFN, Laboratori Nazionali del Gran Sasso, Italy


UHE NEUTRINOS with E > 1017 eV Cosmogenic neutrinos
Reliable prediction guaranteed by observations of UHECR.

Production:
p+
tar

+ + + n µ+ + µ e+ + µ + e ¯

p+

tar

- + all µ- + µ ¯ e- + µ + e ¯

No -neutrinos and deficit of e neutrinos. They appear due to oscilla¯ tions, with equipartition at observations µ : e : = 1 : 1 : 1 as approximation.. Neutrinos beyond SM · Topological Defects · Superheavy Dark Matter · Mirror Matter


COSMOGENIC NEUTRINOS

Volume 28B, number 6

PHYSICS LETTERS

6 January 1969

COSMIC RAYS AT ULTRA HIGH ENERGIES (NEUTRINO?)

V. S. BERESINSKY and G. T. ZATSEPIN
Academy of Sciences of the USSR. Physical Institute. Moscow Received 8 November 1968 Th e n e u t ri n o s p calcu lated . A sp ectr a t an en erg y E > 3 ri se e c t r u m p r o d u c e d b y p r o t o n s o n mi c r o w a v e p h o t o n s i s u m o f e9 t ens i ve ai r sho we r pri ma ri e s can ha ve no cut -o ff x x 1 0 1 e V . I f t h e n e u t r i n o - n u c l e o n t o t a l c ro s s - s e c t i o n s u p t o t h e g e o me t r i c a l o n e o f a n u c l e o n .

Greisen [1] and then Zatsepin and Kusmin [2] have predicted a rapid cutoff in the energy spectrum of cosmic ray protons near E~3xl019 eV because of pion production on 2.7° black body radiation. Detailed calculations of the spectrum were made by Hillas [3]. Recently there were observed [4] three extremely energe9ic extensive air showers with an energy of primary particles t exceeding 5 x l01 eV. The flux of these particles turned out of be 10 times greater than according to Hillas' calculations. In the light of this it seems to be of some interest to consider the possibilities of absence of rapid (or any) fall in the energy spectrum of shower producing particles. A hypothetic possibility we shall discuss* 19 consists of neutrinos being the shower producing particles at E > 3 x 10 eV due to which the energy spectrum of shower producing particles cannot only have any fall but even some flattening.

p-unmodified

EAS by

p


RECENT WORKS
· Engel, Seckel, Stanev 2001 · Kalashev, Kuzmin, Semikoz, Sigl 2002 · Fodor, Katz, Ringwald , Tu 2003 · VB, Gazizov, Grigorieva 2003 · Hooper et al. 2004 · M. Ave et al. 2004

APPROACH and RESULTS:
· Normalization by the observed UHECR flux · Neutrino flux is SMALL in non-evolutionary models with E · Neutrino flux is LARGE in evolutionary models with E
max max

1021 eV

1022 eV


COSMOGENIC NEUTRINOS IN THE DIP MODEL FOR UHECR
V.B. and Grigorieva 1988; V.B., Gazizov, Grigorieva 2005 - 2006.

The dip is a feature in the spectrum of UHE protons propagating through CMB: p + CMB e+ + e- + p Calculated in the terms of modification factor (E ) the dip is seen in all observational data. Jp (E) (E) = unm Jp (E) ,
unm where Jp (E ) includes only adiabatic energy losses and Jp (E ) - all energy losses.


DIP AND GZK CUTOFF IN THE DIFFUSE SPECTRUM

DEFINITION OF MODIFICATION FACTOR Jp (E ) (E ) = unm Jp (E )
unm where Jp (E ) includes only adiabatic energy losses (redshift) and Jp (E ) includes total energy losses, tot (E ) or adiabatic, e+ e- energy losses, ee (E ).


DIP AND GZK CUTOFF IN TERMS OF MODIFICATION FACTOR

The dotted curve shows ee , when only adiabatic and pair-production energy losses are included. The solid and dashed curves include also the pion-production losses.


COMPARISON OF DIP WITH OBSERVATIONS

10

0

10
ee

0

modification factor

modification factor





ee

10

-1

10

-1

Akeno-AGASA
10
-2

Yakutsk
-2

g=2.7
10
17



to ta l

10

g=2.7
10
17



to ta l

10

18

10

19

10

20

10

21

10

18

10

19

10

20

10

21

E, eV

E, eV

10

0

modification factor



ee

10

-1

HiRes I - HiRes II


10

-2

g=2.7
10
17

to ta l

10

18

10

19

10

20

10

21

E, eV


AUGER DATA 2010


GZK CUTOFF IN HiRes DATA In the integral spectrum GZK cutoff is numerically characterized by energy E1/2 where the calculated spectrum J (> E ) becomes half of power-law extrapolation spectrum K E - at low energies. As calculations (V.B.&Grigorieva 1988) show E1
/2

= 1019

.72

eV

valid for a wide range of generation indices from 2.1 to 2.8. HiRes obtained: E
1.2

1/2

= 10

19.73±0.07

eV

1

J(>E)/KE

-

0.8

0.6

0.4

0.2

0

17

17.5

18

18.5

19

19.5

20

20.5

21

log10(E) (eV)


COSMOGENIC NEUTRINO FLUXES IN THE DIP MODEL
E J(E) eV m-2sec-1ster
-1

10

25

z HiRes II

max=2;

E

max

=1021eV; g=2.7; m=0 HiRes I

1024

p

2

1023



3

i

10

18

10

19

10

20

1021

E, eV
10
25

z HiRes II

max=5;

E

max

=10 eV; g=2.47; m=3.2
23

E J(E) eV m-2sec-1ster

-1

HiRes I

p
1024

2

1023



i

3

10

18

10

19

10

20

10

21

1022

10

23

E, eV


COSMOGENIC NEUTRINO FLUXES FROM AGN

1025 E3J(E), eV 2 m-2 s-1 sr
-1

g=2.52, z

max

=2, z c =1.2, m=2.7

10

24

p
Emax=1022eV

+

1023

Emax=1021eV

1017

1018

1019

1020

1021

1022

E, eV


LOWER LIMIT ON NEUTRINO FLUXES IN THE PROTON MODELS
V.B. and A. Gazizov 2009

E J(E) eV m-2sec-1ster

-1

1025

zmax=2; Emax=1021eV; m=0 HiRes II
2.7

HiRes I

1024

2.0

2

p 2.0
1023 2.7 2.7 2.0 10
18

3



i

10

19

10

20

1021

E, eV


CASCADE UPPER LIMIT
V.B. and A.Smirnov 1975 e - m cascade on target photons : + tar e+ + e e + tar e +
-

Spectrum of cascade photons
cas J

(E ) =

K (E /X )- K (E /X )-

3 /2 2

for for

E X , X E a ,
2

(1)

with a steepening at E > a , and X = 1/3 (a /me ) cmb . obs EGRET: agreement with spectrum (1) and 3 â 10-6 eV/cm3 .


UPPER LIMIT ON NEUTRINO FLUX cas 4 > c
E

4 E J (E )dE > E c
2



J (E )dE
E

4 E J (> E ) c

E

-2

c E I ( E ) < cas. 4 c cas - generation spectrum : E 2 Ji (E ) < , i = µ + µ etc. ¯ 12 ln Emax /Emin


CASCADE UPPER LIMIT FROM FERMI LAT
V.B., Gazizov, Kachelriess, Ostapchenko 2010.

max cas = 5.8 â 10

-7

eVcm-

3


OBSERVATIONAL AND THEORETICAL UPPER LIMITS
V.B., Gazizov, Kachelriess, Ostapchenko 2010.


UHE NEUTRINOS FROM TOPOLOGICAL DEFECTS
Symmetry breaking in early universe results in phase transitions, which are accompanied by Topological Defects. TDs OF INTEREST FOR UHE NEUTRINOS. · Monopoles: · Ordinary strings: · Superconducting strings: · Monopoles connected by strings: e.g. necklaces Zn = Z2 .
NECKLACE
M M

G H â U (1) U (1) breaking U (1) breaking G H â U (1) H â Z
n

MS NETWORK

M

M

M

M


ORDINARY and SUPERCONDUCTING STRINGS
Ordinary strings are produced at U (1) symmetry breaking, i.e. by the Higgs mechanism: L = (+ - 2 )2 . They are produced as long strings and closed loops. The fundamental property of a loop is oscillation with periodically produced cusp, where v c. In a wide class of particle physics strings are superconducting (Witten 1985) dJ/dt e2 E If a string moves through magnetic field the electric current is induced J e2 vBt The charge carriers X are massless inside the string, and massive outside. When current exceeds the critical value Jc emX , the charge carriers X can escape. Energy of released particles is EX c mX , they are emitted in a cone 1/c . In ordinary strings the neutral particles, e.g. Higgses, can escape through a cusp, too.


UHE neutrino jets from superconducting strings V.B., K.Olum, E.Sabancilar and A.Vilenkin 2009 > Basic parameter: symmetry breaking scale 1 â 109 GeV. Lorentz factor of cusp c 1012 . Electric current is generated in magnetic fields (B , fB ). Clusters of galaxies dominate. max J e2 B l, Jcusp c J, Jcusp ic e . Particles are ejected with energies EX ic c 1022 GeV. Diffuse neutrino flux : E 2 J (E ) = 2 â 10-8 ic B-6 f-3 GeVcm does not depend on in a range > 1 â 109 GeV. Signatures:
-2 -1

s

· Correlation of neutrino flux with clusters of galaxies. · Detectable flux of 10 TeV gamma ray flux from Virgo cluster. · Multiple simultaneous neutrino induced EAS in field of view of JEM-EUSO.


NECKLACES
V.B., A.Vilenkin, PRL 79, 5202, 1997 G H â U (1) H â Z2 m s 2 mass of monopole: m = 4 m /e, tension: µ = 2 s Due to gravitational radiation, strings shrink, and monopoles inevitably annihilate. ¯ M + M Aµ , H pions neutrinos Production rate of X-particles: nX r2 µ/t3 mX , where r = m/µd . Energy density mX nX t must be less 2 â 10-6 eV/cm3 (EGRET). r2 µ 8.5 â 10 Neutrino energy: E
max 27

GeV

2

0.1m

X

1013 (mX /1014 ) GeV


UHE NEUTRINOS FROM NECKLACES

1e+26 1e+25 1e+24 1e+23

¦¥ ¤ ¸ ¢¡

1e+22 1e+18

1e+19

1e+20

1e+21

B9 A@ 8 9 7
1e+22

¤ ¦¸ 65 4 32 10 )% (' &% $# "! 8

1e+27

§ © ¨ §




MONOPOLES CONNECTED BY STRINGS
V.B., X.Martin, A.Vilenkin, PR D56, 2024, 1997 G H â U (1) H â ZN m s Due to cosmological evolution monopoles become relativistic at t t0 : Monopoles oscillate due to f = µ and obtain a proper acceleration amax = 1.
2

0 33

2 . 0

mX (mX is the boson mass) accelerated monopoles can radiIn case a ate the massive gauge bosons with g2 P= 3 2 , 0 16 6 2 Emax = 0 a
max

2 3 = 30

E

max

REACHES THE PLANCKIAN SCALE !


UHE MIRROR NEUTRINOS
1. CONCEPT OF MIRROR MATTER Mirror matter is based on the theoretical concept of the space reflection, as first suggested by Lee and Yang (1956) and developed by Landau (1956), Salam (1957), Kobzarev, Okun, Pomeranchuk (1966) and Glashow (1986, 1987): see review by Okun hep-ph/0606202 Extended Lorentz group includes reflection: x -x. In particle space it corresponds to inversion operation Ir . Reflection x -x and time shift t t + t commute as coordinate transformations. In the particle space the corresponding operators must commute, too: [ H , Ir ] = 0 . Hence, Ir must correspond to the conserved value. · Lee and Yang: Ir = P · R , where R transfers particle to mirror particle: Ir L =R and Ir R =
L

· Landau: Ir = C · P , where C transfers particle to antiparticle.


2. OSCILLATION OF MIRROR AND ORDINARY NEUTRINOS
Kobzarev, Okun, Pomeranchuk suggested that ordinary and mirror sectors communicate only gravitationally. COMMUNICATION TERMS include EW SU(2) singlet interaction term: L
comm

=

1¯ ( )( ) MPl

(2)

where L = (L , L ) and = ( , - ). + 0 After SSB, Eq.(2) results in mixing of ordinary and mirror neutrinos. L with µ v
2 EW mix 2 vEW = , MPl

/MPl = 2.5 · 10

-6

eV.

It implies oscillations between and . Berezhiani, Mohapatra (1995) and Foot, Volkas (1995).


3. UHE NEUTRINOS FROM MIRROR TDs
In two-inflatons scenario with curvature-driven phase transition (V.B. and Vilenkin 2000) there can be: matter matter , TD TD HE mirror 's are produced by mirror TDs and oscillate into visible 's. All other HE mirror particles which accompany neutrino production remain invisible. short-distance and long-distance oscillations (V.B, Narayan, Vissani 2003): P
µ e

=

1 sin2 2 8

12

,P

µ µ

= P

µ

=

11 - sin2 212 , 46

Pµ






=

1 . 2

Signature: diffuse flux exceeds cascade upper limit.


CONCLUSIONS
· UHE neutrino astronomy has a balanced program of observations of reliably existing cosmogenic neutrinos, and top-down neutrinos predicted by the models beyond SM (e.g. topological defects or SHDM). · Fluxes of cosmogenic neutrinos are strongly bounded by the cascade upper limit with the new extragalactic gamma-ray background radiation measured by Fermi-LAT. With this upper limit detectability of neutrino flux max depends on maximum acceleration energy Emax . Acceleration to Ep max 1 â 1022 eV is a problem in astrophysics. With this Ep cosmogenic neutrinos can be detected only marginally by JEM-EUSO. Fluxes of cosmogenic neutrinos are further lowered if heavy-nuclei make the substantial contribution to primary radiation. and are undetectable in case heavy nuclei are dominant component. · Energies of cosmogenic neutrinos are expected below E 1021 eV, while energies of neutrinos in top-down scenarios should be much higher. Thus neutrinos with E > 1021 - 1022 eV are a signal for a new physics.


PRINCIPLES OF EUSO OBSERVATIONS