theoretical bounds and current experimental limits on the diffuse neutrino flux
Post on 28-Jan-2016
22 Views
Preview:
DESCRIPTION
TRANSCRIPT
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 11
Theoretical Bounds and Current Theoretical Bounds and Current Experimental Limits Experimental Limits
on the Diffuse Neutrino Fluxon the Diffuse Neutrino Flux
Rezo ShanidzeRezo Shanidze17/06/200417/06/2004
Seminar zu aktuellen Fragen der Seminar zu aktuellen Fragen der AstroteilchenphysikAstroteilchenphysik
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 22
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
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 33
The Sources of High EnergyThe Sources of High Energy
Weak decays: Weak decays: , K, …, charm hadrons:, K, …, charm hadrons:
(99.99 %)(99.99 %)
KK (63.4 %) (63.4 %)
e e 4.9 %, 38.8%) - K4.9 %, 38.8%) - Ke3e3 decay (K, K decay (K, Koo))
4.9 %, 27.2%) - K4.9 %, 27.2%) - K33 decay decay
c c l l ll + X , + X , l l =e, =e, ( 10 %) ( 10 %)
ee ee
cc,K, K,K, Koo)= 7.8 , 3.7 , 15.5 m, )= 7.8 , 3.7 , 15.5 m, L=L=cc =E/m=E/m cc( charm ) ~ 100 ( charm ) ~ 100 mm
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 44
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
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 55
Atmospheric Atmospheric flux flux
CR spectra: CR spectra: dN/dE = a EdN/dE = a E-- =2.7 (knee ~10=2.7 (knee ~101515-10-101616eV)eV) Hydrogen(0,9) He(0.08), …Hydrogen(0,9) He(0.08), …
p(He) + A p(He) + A +X +X exp(-exp(-h/h/
hh00))hh00=8.4km=8.4km Earth atmosphereEarth atmosphere: 1030 g/cm: 1030 g/cm-2-2
AA((KAKA116 (138) gm/116 (138) gm/cmcm-2-2
Int./decay(GeV): 115(850)Int./decay(GeV): 115(850)
change of change of 2.7 2.7 3.7 3.7 Secant theta effectSecant theta effect
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 66
Atmospheric Atmospheric flux flux
CR interaction and propagation:CR interaction and propagation:
MC codes: AIRES, COSMOS, MOCCA, MC codes: AIRES, COSMOS, MOCCA, HEMAS, CORSIKAHEMAS, CORSIKA
CORSICA physics models: CORSICA physics models: VENUS, QGSJET, DPMJET, VENUS, QGSJET, DPMJET, SYBILL, HDPM.SYBILL, HDPM.
Experimental Data:Experimental Data: - Underground experiments:- Underground experiments: MACRO, Frejus, L3C, …MACRO, Frejus, L3C, … - NT data:- NT data: Baikal, AMANDABaikal, AMANDA
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 88
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
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 99
Cosmogenic (GZK) Cosmogenic (GZK) Flux Flux Photopion production by Photopion production by
UHECR (E>10UHECR (E>101919 GeV) : GeV) : + p + p N N nn CMB : 2.7K , ~400 CMB : 2.7K , ~400 /cm /cm33, E , E
~ meV. ~ meV. IR: 1-2 IR: 1-2 cm cm33, E ~ eV. , E ~ eV.
(T.Stanev, astro-ph/0404535(T.Stanev, astro-ph/0404535))
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1010
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):
1 event /yr ~6x101 event /yr ~6x1044mm22
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1111
High Energy High Energy Detectors Detectors
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1212
The Baikal NTThe Baikal NT
First First telescope telescope 1.1 km depth 1.1 km depth NT-36, 96, 192NT-36, 96, 192
140 m
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1313
Results from BAIKALResults from BAIKAL
34 events of upward 34 events of upward
astro-ph/0404096astro-ph/0404096 Search for bright cascadesSearch for bright cascades EE-2-2, , ee=1:1:1=1:1:1 90% C.L. limit 90% C.L. limit EE22::
1.3x101.3x10-6-6 cm cm-2-2ss-1-1srsr-1-1GeVGeV
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1414
AMANDA AMANDA Detector Detector
AAntarcticntarctic MMuonuon AAndnd NNeutrinoeutrino DDetectoretector AArrayrray
AMANDA (ice):AMANDA (ice):1150-2350m1150-2350m
B10 (97-99): B10 (97-99): 10 strings,10 strings,302 OM302 OM
II (2000):II (2000):19 strings19 strings677 OM677 OM
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1515
AMANDA ResultsAMANDA Results ( ( flux) flux)
AMANDA B10: 1977AMANDA B10: 1977 measurement:measurement: Coverage - 2Coverage - 2 ang. ~ 2ang. ~ 2oo -2.5 -2.5oo
logE ~ 0.3-0.4logE ~ 0.3-0.4 6 < E < 1000 TeV6 < E < 1000 TeV PRL 90(2003) 2151101-1PRL 90(2003) 2151101-1
EE-2-2, , ee=1:1:1=1:1:1 EE22(E) <(E) <
8.4x108.4x10-7-7GeV /cmGeV /cm2 2 s srs sr
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1616
AMANDA ResultsAMANDA Results (cascades)(cascades)
cascades:cascades: Coverage - 4Coverage - 4 ang. ~ 30ang. ~ 30oo -40 -40oo
logE ~ 0.1-0.2logE ~ 0.1-0.2 Astro-ph/0405218 Astro-ph/0405218 197 d, MC: 920 d197 d, MC: 920 d 50 TeV<E<5 PeV50 TeV<E<5 PeV EE-2-2, , ee=1:1:1=1:1:1 EE22(E) <(E) <
8.6x108.6x10-7-7GeV /cmGeV /cm2 2 s srs sr
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1717
Acoustic Detection of UHE Acoustic Detection of UHE
Astro-ph/0406105Astro-ph/0406105 SAUND detector: ~ 250 SAUND detector: ~ 250
km2 (US Navy array) - km2 (US Navy array) - only 7 used.only 7 used.
~1600 m undersea~1600 m undersea 147 days of running 147 days of running
(2002)(2002) Calibration, analysisCalibration, analysis
-Energy, position -Energy, position
- Rates, reconstraction - Rates, reconstraction
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 1818
IceCubeIceCube
1400 m
2400 m
AMANDA
South Pole
IceTop
- 80 Strings- 80 Strings- 4800 PMT - 4800 PMT - Instrumented Instrumented
volume: 1 km volume: 1 km3 3
- Installation:Installation: 2004-2010 2004-2010
~ 80.000 atm. per year
10/7/200310/7/2003 C.Spiering, VLVNT WorkshopC.Spiering, VLVNT Workshop
Search for diffuse excess of extra-terrestrial Search for diffuse excess of extra-terrestrial high energy muon neutrinos high energy muon neutrinos
bound
WB bound
DUMAND
FREJUSMACRO
Muons in Amanda-B10 (1997)
Expectation Amanda-II, 3 years
Expectation IceCube, 3 years
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 2020
RICE AGASA
Amanda, Baikal2002
2004
2007
AUGER
Anita
AABN
2012
km3
EUSOAugerSalsa
GLUE
17.05.200417.05.2004 Reso ShanidzeReso Shanidze 2121
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 ..
top related