Teleskopy na neutrina neutrinová astronomie. Princip detekce.

Prezentace na téma: "Teleskopy na neutrina neutrinová astronomie. Princip detekce."— Transkript prezentace:

1 Teleskopy na neutrina neutrinová astronomie

2 Princip detekce

3 Amanda a IceCube

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5 Antares

6 Výsledky ICECUBE

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8 Citlivost detektorů a limity

9 Difusní toky (limity)

10 Průchod neutrin Zemí

11 Sluneční a atmosferická neutrina, historie: 1931 - Pauli presents hypothetical "neutron" particlePauli presents hypothetical "neutron" particle 1934 - Fermi develops theory of weak interaction and baptizes the neutrinoFermi develops theory of weak interaction and baptizes the neutrino 1956 - First discovery of the neutrino by an experimentFirst discovery of the neutrino by an experiment 1962 - Discovery of an other type of neutrino at Brookhaven National LabDiscovery of an other type of neutrino at Brookhaven National Lab 1968 - First experiment to detect electron neutrinos produced by the sunFirst experiment to detect electron neutrinos produced by the sun 1978 - Discovery of the tau lepton at Stanford Linear Accelerator Center, existence of tau neutrino theorizedDiscovery of the tau lepton at Stanford Linear Accelerator Center, existence of tau neutrino theorized 1983 - Kamiokande becomes operationalKamiokande becomes operational 1985 - The IMB experiment & Russian team reports measurement of non-zero neutrino massThe IMB experiment & Russian team reports measurement of non-zero neutrino mass 1987 - Kamiokande and IMB detect simultaneous burst of neutrinos from SupernovaKamiokande and IMB detect simultaneous burst of neutrinos from Supernova 1989 - Kamiokande becomes second experiment detecting neutrinos from the sun and confirms anomaly of finding only 1/3 expected rateKamiokande becomes second experiment detecting neutrinos from the sun and confirms anomaly of finding only 1/3 expected rate 1990 - IMB confirms deficit of muon neutrino interactionsIMB confirms deficit of muon neutrino interactions 1991 - LEP experiments show that there are only three light neutrinosLEP experiments show that there are only three light neutrinos 1994 - First proclamation of possible neutrinos oscillations seen by LSND experimentFirst proclamation of possible neutrinos oscillations seen by LSND experiment 1995 - Missing solar neutrinos confirmed by GALLEXMissing solar neutrinos confirmed by GALLEX 1996 - AMANDA neutrino telescope observes neutrinos at the south poleAMANDA neutrino telescope observes neutrinos at the south pole 1998 - Super-Kamiokande collaboration announces evidence of non-zero neutrino massSuper-Kamiokande collaboration announces evidence of non-zero neutrino mass 2002 – SNO potvrzuje model Slunce, triumf oscilaci

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13 Sluneční neutrina

14 galiu m chlorin e SNO, SuperK Sluneční neutrina

15 Sluneční neutrina, detekce HOMESTAKE – extrakce radiochemicky Davis, Bahcal, málo neutrin ze slunce podobný princip GALEX a SAGE detekce kolem 100-800 keV neutrin A nebo v detektorech typu KAMIOKANDE a SUPERKAMIOKANDE Inverzní beta rozpad

16 SuperKamiokande

17 mio n elektro n

18 Něco tady chybí, nebo je špatné model Slunce?

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20 Neutronov y zachyt na deuteronu

21 Slana faze - SNO

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23 1964: Něco tady chybí (oscilace?), nebo je špatne model Slunce? 2002: Odpověď SNO : Chybí mi eletronová neutrina, ale celkový počet neutrin je v pořádku TEDY OSCILACE Nobelova cena 2002... only who dares can win... Your humble servant, W. Pauli

24 Oscilace Flavour stav Hmotový stav Mixing matice Vývoj stacionárního stavu Stav po čase t,v t=0 čistě stav alfa Pravděpodobnost, že z alfa bude po čase t beta Pro dva flavoury

25 Atmosférická neutrina 1 : 2 cca. :)

26 Atmosférická neutrina e pod GeV e nad GeV miony nad GeV miony pod GeV SuperK TEDY OSCILACE

27 Supernova 1987A a KAMIOKANDE inverzni beta rozpad