17.05.2004 17.05.2004 Reso Shanidze Reso Shanidze 1 Theoretical Bounds and Current Experimental Current Experimental Limits Limits on the Diffuse Neutrino on the Diffuse Neutrino Flux Flux Rezo Shanidze Rezo Shanidze 17/06/2004 17/06/2004 Seminar zu aktuellen Fragen Seminar zu aktuellen Fragen der Astroteilchenphysik der Astroteilchenphysik
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Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux
Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux. Rezo Shanidze 17/06/2004 Seminar zu aktuellen Fragen der Astroteilchenphysik. Layout. The sources of high energy n: - Bottom-up models: pp( g ) g p + X g mn m g e n m n e - PowerPoint PPT Presentation
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LayoutLayout The sources of high energy The sources of high energy - Bottom-up models: pp(- Bottom-up models: pp() ) + X + Xeeee
- Top-down models: Decays of WIMPs - Top-down models: Decays of WIMPs (Dark matter, SUSY, Topolocical defects) (Dark matter, SUSY, Topolocical defects) Models and bounds:Models and bounds: - Atmospheric - Atmospheric , WB-bound, HE-, WB-bound, HE- from the Sun from the Sun - Fluxes from AGN, GRB, …- Fluxes from AGN, GRB, … Current experimental limitsCurrent experimental limits Future prospectsFuture prospects SummarySummary
Neutrino Flux from pp and pNeutrino Flux from pp and p
Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749Learned, Mannheim, Annu.Rev.Nucl.Part.Sci. 50(2000), 679-749 The volume emissivity of produced The volume emissivity of produced
QQ(pp)(pp) = =∫∫nnt t c c NN ( (ddpppp(E(E,E)/dE,E)/dE)()(dN/dE) dEdN/dE) dE
ddpppp(E(EE) /dEE) /dEdiff. Inclusive cross-sectiondiff. Inclusive cross-section dN/dEdN/dE = = N N 00EE–s–s dEdE - - diff. energy spectra of p(CR)diff. energy spectra of p(CR) QQ
(pp)(pp)(E)(E) – – practically same energy spectrapractically same energy spectra
QQ(pp)(pp) ~ ~ QQ
(pp)(pp) (4E (4E)) ~ ~ EE-s-s
dd//dEdE= = ∫∫Q Q dr dr over spatial extent of the sourceover spatial extent of the source
Waxman-Bahcal Bound:Waxman-Bahcal Bound: High energy High energy from astrophysical from astrophysical sourcessources
• E.Waxman,J.Bahcall PRD, v59(1998), 023003E.Waxman,J.Bahcall PRD, v59(1998), 023003• Based on observations of Fly‘s Eye and AGASABased on observations of Fly‘s Eye and AGASA• Cosmological origin of CR above 10Cosmological origin of CR above 101919 GeV GeV ((E.Waxman, astro-ph/9508037E.Waxman, astro-ph/9508037))• Cosmological distribution of CR sources:Cosmological distribution of CR sources:• dN/dE ~ dN/dE ~ EE--22• Energy production rate ~ 5x10 Energy production rate ~ 5x10 4444 erg Mpc erg Mpc-3-3yr yr -1-1
•EE22< 2 x 10< 2 x 10-8-8 GeV/cm GeV/cm22 s sr s sr
High Energy High Energy from the Sun from the Sun Sun as a standard Sun as a standard - candle ? - candle ?
G. Ingelman, M. Thunman Phys. Rev. G. Ingelman, M. Thunman Phys. Rev.
D 54(1996), 4385D 54(1996), 4385
Calculations with LUND MC: Calculations with LUND MC: PYTHIA(v5.7) /JETSET(7.4)PYTHIA(v5.7) /JETSET(7.4)CR flux: (aECR flux: (aE--interactioninteractionWith the Sun atmosphereWith the Sun atmosphere
Rate of Rate of events integrated over events integrated over the Sun solid angle. the Sun solid angle. for NT (Efor NT (E > 100 GeV): > 100 GeV):
Sumary and OutlookSumary and Outlook High energy High energy astronomy: astronomy: Data from Baika(lake), AMANDA(ice)Data from Baika(lake), AMANDA(ice)
New undersea NT: ANTARES, NESTORNew undersea NT: ANTARES, NESTOR
Sensitivity to the cosmicSensitivity to the cosmic diffuse flux diffuse flux NT on km3 scale: IceCube, KM3NeTNT on km3 scale: IceCube, KM3NeT
Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE Acoustic and other technique (RICE, ANITA, EUSO, GLUE) for UHE ..