TESTING PHYSICS BEYOND SM

Transcription

1 SuperGZK NEUTRINOS E ν > ev: TESTING PHYSICS BEYOND SM V. Berezinsky INFN, Laboratori Nazionali del Gran Sasso, Italy

2 PROSPECTS for OBSERVATIONS 1. SPACE DETECTORS: EUSO and OWL

3 2. RADIO DETECTION Askaryan effect (1962): coherent radio-emission by excess of electrons in a shower. GLUE: Radio from the Moon. RICE/ANITA: Radio from Antarctic ice. FORTE: satellite observation of the Greenland ice. COMMON FEATURES: ffl High energy detection threshold E > (1 100) ev. ffl Low-flux detection (very large effective mass).

4 2. RADIO DETECTION Askaryan effect (1962): coherent radio-emission by excess of electrons in a shower. GLUE: Radio from the Moon. RICE/ANITA: Radio from Antarctic ice. FORTE: satellite observation of the Greenland ice. COMMON FEATURES: ffl High energy detection threshold E > (1 100) ev. ffl Low-flux detection (very large effective mass). MOTIVATION: A crazy theory (theorist) will always be available!

5 GENERATION of supergzk NEUTRINOS ffl COSMOGENIC (pfl) NEUTRINOS E ν ο (1 10) ev ffl PHYSICS BEYOND STANDARD MODEL: E ν > ev. Acceleration to E p > ο ev is a challenge for astrophysics. TDs and SHDM provide naturally these energies: ffl Decay of superheavy particles (DM and TD) : E ν < ο 0:1m X, m X up to M GUT. ffl Annihilation of monopoles connected by strings, e.g. necklaces. + μ M! A μ ;H! pions! neutrinos M Radiation by monopoles in network ffl Emission of gauge bosons by accelerated monopoles. E ν ο a, can reach M P` ffl Cusps in superconducting strings

6 ! cas > 4ß c EJ ν (E)dE > 4ß c E Z 1 2 I ν (E) < c E! cas: 4ß CASCADE UPPER LIMIT V.B. and A.Smirnov 1975 e-m cascade on target photons: + fl tar! e + + e fl + fl tar! e 0 + fl 0 e! fl ο (2 3) 10 EGRET: ev/cm. 3 6 obs Z 1 J ν (E)dE 4ß c EJ ν(> E) E E

7 COSMOGENIC NEUTRINOS p CMB ± neutrinos p-unmodified EAS by ν p n J E = E E p g g 1 J unm p E E E p =0.05

8 ffl Engel, Seckel, Stanev 2001 RECENT WORKS ffl Kalashev, Kuzmin, Semikoz, Sigl 2002 ffl Fodor, Katz, Ringwald, Tu 2003 ffl VB, Gazizov, Grigorieva 2003 APPROACH and RESULTS: ffl Normalization to the observed UHECR flux ffl Neutrino flux is SMALL in non-evolutionary models with E max» ev ffl Neutrino flux is LARGE in evolutionary models with E max ev

9 The BGG model for UHECR LOW ENERGY LIMIT FOR COSMOGENIC NEUTRINOS The observed UHECR flux does not guarantee the detectable UHE neutrino flux

10 COSMOGENIC NEUTRINOS IN BGG MODELS

11 UHE NEUTRINOS FROM SUPERHEAVY DARK MATTER PRODUCTION: many efficient mechanisms at post-inflationary epochs, ffl most attractive one is production in time-varying gravitational field. Creation occurs H(t) ο m when X. H(t)» m Since ο ffi GeV: m X ο GeV: e.g. m X ο GeV results in Ω X h 2 ο 0:1. LONGEVITY OF SHDM PARTICLES. ffl Discrete gauge symmetry protection, like R-parity for neutralino. Decay is provided by superweak effects: wormhole, high dimension operators etc. ACCUMULATION IN THE GALACTIC HALO. ffl Like for any overdensity= DM,. 5 ffl X-PARTICLE DECAY. Ratio of fluxes ν : fl : p ß 4 : 2 : 1, Energy spectrum: J SHDM (E) / E fl g, with fl g ß 1:94:

12 1e+27 UHE NEUTRINOS FROM SHDM E 3 J(E) (ev 2 m 2 s 1 sr 1 ) 1e+26 1e+25 1e+24 1e+23 1e+22 ν fl p extr. MX = GeV p 1e+21 1e+18 1e+19 1e+20 1e+21 1e+22 E (ev)

13 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: G! H U (1) ffl Ordinary strings: U (1) breaking ffl Superconducting strings: ffl Monopoles connected by strings: ffl e.g. Z necklaces = Z 2 n. NECKLACE M M U (1) breaking G! H U (1)! H Z n MS NETWORK M M M M

14 max ν E NECKLACES V.B., A.Vilenkin, PRL 79, 5202, 1997! H U (1)! H Z 2 G m s mass of m = 4ß monopole: m =e, μ = 2ß tension: s 2 Due to gravitational radiation, strings shrink, and monopoles inevitably annihilate. M + μ M! A μ ;H! pions! neutrinos Production rate of X-particles: _n X ο r 2 μ=t 3 m X, where r = m=μd. Energy density! ο m X _n X t must be less ev/cm 3 (EGRET). Neutrino energy: r 2 μ» 8: GeV 2 ο 0:1m X ο (m X =10 14 ) GeV

15 UHE NEUTRINOS FROM NECKLACES 1e+27 E 3 J(E) (ev 2 m 2 s 1 sr 1 ) 1e+26 1e+25 1e+24 1e+23 MX = GeV ν p p+fl 1e+22 1e+18 1e+19 1e+20 1e+21 1e+22 fl E (ev)

16 E max = 0a max = ß Ω MONOPOLES CONNECTED BY STRINGS V.B., X.Martin, A.Vilenkin, PR D56, 2024, 1997! H U (1)! H Z N G m s Due to cosmological evolution monopoles become relativistic t ο t at 0 0 fl : 1. Monopoles oscillate f = μ due to and obtain a a proper acceleration Ω. 2 = p max In case a fl m X (m X is the boson mass) accelerated monopoles can radiate the massive gauge bosons with P = 2 g p 6ß Ω2 ; 16 E max REACHES THE PLANCKIAN SCALE!

17 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). Extended Lorentz group includes reflection: ~x! ~x: In particle space it corresponds to inversion operation I r. Reflection ~x! ~x and time shift t! t+ t commute as coordinate transformations. In the particle space the corresponding operators must commute, too: [H;I r ] = 0: Hence, I r must correspond to the conserved value. ffl Lee and Yang: I r = P R, where R transfers particle to mirror particle: r ΨL =Ψ 0 R and I rψr =Ψ 0 L I, C where transfers particle to antiparticle. ffl Landau: I r = C P

18 2 v μν EW L ν 0 R; Pl M 2. OSCILLATION OF MIRROR AND ORDINARY NEUTRINOS Kobzarev, Pomeranchuk, Okun suggested that ordinary and mirror sectors communicate only gravitationally. COMMUNICATION TERMS include EW SU(2) singlet interaction term: comm 1 L ( = μ ψ L ffi)(ψ 0 R ffi0 ) (1) Pl M where μ ψ L = (μν L ; μ`l) and ffi = (ffi Λ 0 ; ffiλ + ). After SSB, Eq.(1) results in mixing of ordinary and mirror neutrinos. with μ v 2 EW =M Pl = 2: ev. It implies oscillations between ν and ν 0. Berezhiani, Mohapatra (1995) and Foot, Volkas (1995).

19 3. UHE NEUTRINOS FROM MIRROR TDs In two-inflatons scenario with curvature-driven phase transition (V.B. and Vilenkin 2000) there can be: 0 matter fi ρ matter ; ρ 0 TD fl ρ TD ρ HE mirror ν s are produced by mirror TDs and oscillate into visible ν s. All other HE mirror particles which accompany neutrino production remain invisible. The upper limit on HE neutrino flux, due to is very weak. ν + ν DM! Z 0! e; fl! cascade It can be constrained only observationally (e.g. by GLUE, RICE, FORTE). Signature: diffuse flux exceeds cascade upper limit.

20 UHE NEUTRINOS FROM MIRROR TDs 7 Log(E 2 Jν(E)=(eV cm 2 s 1 sr 1 )) Rice cascade MX =10 14 GeV Glue mirror TD Forte Log(E=eV)

21 CONCLUSIONS ACCELERATOR (COSMOGENIC) NEUTRINOS Energies are up E to ο 1 10 ν ev. Acceleration to E max p ffl is a problem in 21 astrophysics. ο ev The observed UHECR flux does not guarantee the detectable flux of ffl supergzk neutrinos. SuperGZK neutrino fluxes are detectable in case of evolutionary ffl sources with > 1 ο p E ev They are small/undetectable in case of non-evolutionary sources E with» ffl p 10 ev NON-ACCELERATOR NEUTRINOS SHDM can produce neutrinos with E energies > ο 1 10 ν ev and with ffl fluxes of order of the observed UHECR 22 ο 10 at ev. 20 E TDs, e.g. necklaces, monopole-string network, cusps of ffl superconducting strings etc, can produce large fluxes of supergzk neutrinos with energies > (1 100) 10 ν ev and up to E 20 Pl. E

22 ν (E)» c I 4ß cas! 2 ; or I ν(> E)» 10 km 2 yr 1 sr 1 E 1 20 E FLUX UPPER LIMIT In all above cases the diffuse flux is constrained by the cascade upper limit: MIRROR supergzk NEUTRINOS The energies can be very large with flux unconstrained by ordinanary cascade upper limit