Identifying the neutrino mass hierarchy with supernova neutrinos
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- Harvey Hutchinson
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1 Identifying the neutrino mass hierarchy with supernova neutrinos Ricard Tomàs AHEP Group - Institut de Física Corpuscular (CSIC - Universitat de València) IPM School & Conference on Lepton & Hadron Physics May 15-20, 2006, Tehran R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 1 / 31
2 Outline 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 2 / 31
3 Outline 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 2 / 31
4 Outline 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 2 / 31
5 Outline 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 2 / 31
6 Outline Introduction Determination of the Neutrino Mass Hierarchy 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 3 / 31
7 Introduction Determination of the Neutrino Mass Hierarchy Neutrino Properties: we know... three ν weak and they do mix : ν weak = U αi ν mass U PMNS : c 13 0 e iδ s 13 0 c 23 s s 23 c 23 }{{} atm., K2K, MINOS m 2 atm e iδ s 13 0 c 13 }{{} talks by G. Altarelli and A. Yu. Smirnov c 12 s 12 0 s 12 c } {{ } solar, KamLAND m 2 [M. Maltoni, T. Schwetz, M. A. Tórtola and J. W. F. Valle, 2004] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 4 / 31
8 Introduction Determination of the Neutrino Mass Hierarchy Neutrino Properties: we know... three ν weak and they do mix : ν weak = U αi ν mass U PMNS : c 13 0 e iδ s 13 0 c 23 s s 23 c 23 }{{} atm., K2K, MINOS m 2 atm } e iδ s 13 0 {{ c 13 } θ 13, δ talks by G. Altarelli and A. Yu. Smirnov c 12 s 12 0 s 12 c } {{ } solar, KamLAND m 2 we don t know mixing parameters: θ 13, δ mass hierarchy: sign( matm) 2 absolute mass scale Majorana or Dirac sterile, NSI, µ ν, decay,... R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 4 / 31
9 Introduction Determination of the Neutrino Mass Hierarchy Determination of the Neutrino Mass Hierarchy terrestrial experiments neutrinoless double beta decay experiments: depends on m ee oscillation experiments: vacuum: P(ν α ν β ) basically depends on matm. 2 Earth matter effects: matm/2e 2 + V long baseline suppressed by θ 13 high precision needed superbeams, neutrino factories,... R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 5 / 31
10 Introduction Determination of the Neutrino Mass Hierarchy Determination of the Neutrino Mass Hierarchy terrestrial experiments neutrinoless double beta decay experiments: depends on m ee oscillation experiments: vacuum: P(ν α ν β ) basically depends on matm. 2 Earth matter effects: matm/2e 2 + V long baseline suppressed by θ 13 high precision needed superbeams, neutrino factories,... extraterrestrial sources core-collapse supernovae R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 5 / 31
11 Outline Introduction Role of Core-collapse Supernovae 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 6 / 31
12 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
13 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics: location, explosion mechanism,... R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
14 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics : location, explosion mechanism,... extreme conditions (ρ, B, L,...) drastic matter effects ν propagation very sensitive to ν properties: mass scale, hierarchy, θ 13, µ ν, NSI, ν s,... R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
15 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics : location, explosion mechanism,... but... extreme conditions (ρ, B, L,...) drastic matter effects ν propagation very sensitive to ν properties: mass scale, hierarchy, θ 13, µ ν, NSI, ν s,... large uncertainties in the SN models R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
16 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics : location, explosion mechanism,... but... extreme conditions (ρ, B, L,...) drastic matter effects ν propagation very sensitive to ν properties: mass scale, hierarchy, θ 13, µ ν, NSI, ν s,... large uncertainties in the SN models very low rate: 2 or 3 per century in our Galaxy R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
17 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics : location, explosion mechanism,... but... extreme conditions (ρ, B, L,...) drastic matter effects ν propagation very sensitive to ν properties: mass scale, hierarchy, θ 13, µ ν, NSI, ν s,... large uncertainties in the SN models very low rate: 2 or 3 per century in our Galaxy SNe in nearby galaxies [Ando, Beacom and Yüksel, 2005] diffuse supernova neutrino background (DSNB) information about the cosmic star formation rate (CSFR) [Ando and Sato, 2004, Strigari, Beacom, Walker and Zhang, 2005, C. Lunardini, 2006, A. M. Hopkins and J. F. Beacom, 2006] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
18 Introduction Role of Core-collapse Supernovae Role of Core-collapse Supernovae advantages: SN powerful source of ν s particular ν properties (mixing, weakly interacting,..) ideal messengers of SN physics : location, explosion mechanism,... but... extreme conditions (ρ, B, L,...) drastic matter effects ν propagation very sensitive to ν properties: mass scale, hierarchy, θ 13, µ ν, NSI, ν s,... large uncertainties in the SN models still important information on ν very low rate: 2 or 3 per century in our Galaxy R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 7 / 31
19 Outline Core-collapse Supernova Neutrinos Neutrino Emission 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 8 / 31
20 Neutrino Emission Core-collapse Supernova Neutrinos Neutrino Emission Energy balance Gravitational binding energy G NM 2 R O(1053 ) erg 0.01 % optical energy 1 % kinetical energy 99 % carried away by neutrinos { all flavors roughly equipartioned R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
21 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Emission Energy balance Energy balance: O(10 53 ) erg in all ν flavors Duration several seconds [Totani et al., 1998] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
22 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Emission Energy balance Energy balance: O(10 53 ) erg in all ν flavors Duration Duration: several seconds Spectra Formation [Keil et al., 2003] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
23 Neutrino Emission Core-collapse Supernova Neutrinos Neutrino Emission Energy balance Energy balance: O(10 53 ) erg in all ν flavors Duration Duration: several seconds Spectra Parametrization ( ) α f ν (E) E e E (α+1)e/ E [Keil et al., 2003] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
24 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Emission Energy balance Energy balance: O(10 53 ) erg in all ν flavors Duration Duration: several seconds Spectra Spectra: f ν (E, α, E ) uncertainties in α and E R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
25 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Emission Energy balance Energy balance: O(10 53 ) erg in all ν flavors Duration Duration: several seconds Spectra Spectra: f ν (E, α, E ) uncertainties in α and E but PNS composition differences in the spectra ( hierarchy: E νe E νe E νx ) ν conversion observable effects R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton... 9 / 31
26 Outline Core-collapse Supernova Neutrinos Neutrino Propagation 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
27 Core-collapse Supernova Neutrinos Neutrino Propagation Neutrino Propagation R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
28 Core-collapse Supernova Neutrinos Neutrino Propagation General description Schrödinger equation i d dr ν e ν µ ν τ = [ ] U M2 2E U + V (r) ν e ν µ ν τ talk by A. Yu. Smirnov neutrino propagation basically determined at the resonances m 2 cos(2θ)/2e=v (r res ), V (r) ρ(r) R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
29 Core-collapse Supernova Neutrinos Neutrino Propagation General description Schrödinger equation i d dr ν e ν µ ν τ = [ ] U M2 2E U + V (r) ν e ν µ ν τ talk by A. Yu. Smirnov neutrino propagation basically determined at the resonances m 2 cos(2θ)/2e=v (r res ), V (r) ρ(r) channel: ν or ν? sign( m 2 ), θ adiabaticity: γ γ = m2 sin 2 2θ 2E cos(2θ) 1 d ln V /dr R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
30 Core-collapse Supernova Neutrinos Neutrino Propagation Supernovae two resonances at m 2 : Low { m12 2, θ 12} ν and adiabatic mass hierarchy at matm 2 : High depends on { normal ν inverted ν θ 13 { large adiabatic small non adiabatic SN progenitor ρ profile level crossings [A. Dighe and A. Yu. Smirnov, 2000] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
31 Core-collapse Supernova Neutrinos Neutrino Propagation Supernovae two resonances at m 2 : Low { m12 2, θ 12} ν and adiabatic mass hierarchy at matm 2 : High depends on { normal ν inverted ν θ 13 { large adiabatic small non adiabatic Case Hierarchy sin 2 θ 13 ν SN e P ee ν SN e P ēē A Normal > 10 3 ν 3 0 ν 1 cos 2 θ 12 B Inverted > 10 3 ν 2 sin 2 θ 12 ν 3 0 C Any < 10 5 ν 2 sin 2 θ 12 ν 1 cos 2 θ 12 matter eff. strong dependence of P αβ on the ν scheme! R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
32 Outline Core-collapse Supernova Neutrinos Neutrino Detection 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
33 Neutrino Detection Core-collapse Supernova Neutrinos Neutrino Detection Water Cherenkov : ν e + p n + e + (SK) ν e + p n + e + isotropical ( ) reactions ν + e ν + e forward ( ) ν e + 16 O X + e backwards ( ) R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
34 Determining the Mass Hierarchy: Observables Determining the Mass Hierarchy: Observables Objective determine θ 13 and mass hierarchy with SN ν s F det ν α =P αβ (θ 13, sign( m 2 atm))f 0 ν β why SN ν s? P αβ depends strongly on θ 13 and sign( m 2 atm) R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
35 Determining the Mass Hierarchy: Observables Determining the Mass Hierarchy: Observables Objective determine θ 13 and mass hierarchy with SN ν s Problem F det ν α =P αβ (θ 13, sign( m 2 atm))f 0 ν β why SN ν s? P αβ depends strongly on θ 13 and sign( m 2 atm) large uncertainties in the initial fluxes, F 0 ν R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
36 Determining the Mass Hierarchy: Observables Determining the Mass Hierarchy: Observables Objective determine θ 13 and mass hierarchy with SN ν s Problem F det ν α =P αβ (θ 13, sign( m 2 atm))f 0 ν β why SN ν s? P αβ depends strongly on θ 13 and sign( m 2 atm) large uncertainties in the initial fluxes, F 0 ν Solutions combine observables reduce dependence on SN [Lunardini and Smirnov, 2003] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
37 Determining the Mass Hierarchy: Observables Determining the Mass Hierarchy: Observables Objective determine θ 13 and mass hierarchy with SN ν s F det ν α =P αβ (θ 13, sign( m 2 atm))f 0 ν β Problem why SN ν s? P αβ depends strongly on θ 13 and sign( m 2 atm) large uncertainties in the initial fluxes, F 0 ν Solutions combine observables reduce dependence on SN [Lunardini and Smirnov, 2003] energy/time dependence of P αβ { Earth matter effects shock wave propagation R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
38 Determining the Mass Hierarchy: Observables Determining the Mass Hierarchy: Observables Objective determine θ 13 and mass hierarchy with SN ν s F det ν α =P αβ (θ 13, sign( m 2 atm))f 0 ν β Problem why SN ν s? P αβ depends strongly on θ 13 and sign( m 2 atm) large uncertainties in the initial fluxes, F 0 ν Solutions combine observables reduce dependence on SN [Lunardini and Smirnov, 2003] energy/time dependence of P αβ { Earth matter effects shock wave propagation times where SN models agree neutronization burst R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
39 Outline Determining the Mass Hierarchy: Observables Earth matter effects 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
40 Determining the Mass Hierarchy: Observables Earth matter effects Earth matter effects If SN ν s cross the Earth spectra modulation F νe = F vac ν e + F 0 ν Ā sin 2 (12.5 m 2 L/E) depends on the ν scheme Case Hierarchy sin 2 θ 13 ν e ν e A Normal > 10 3 B Inverted > 10 3 C Any < 10 5 two detectors [Lunardini and Smirnov, 2001, Dighe et al, 2003] one detector [Dighe et al., 2003, Dighe, Kachelrieß, Raffelt and R. T., 2004] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
41 Determining the Mass Hierarchy: Observables Earth matter effects Earth matter effects If SN ν s cross the Earth spectra modulation F νe = F vac ν e + F 0 ν Ā sin 2 (12.5 m 2 L/E) depends on the ν scheme Case Hierarchy sin 2 θ 13 ν e ν e A Normal > 10 3 B Inverted > 10 3 C Any < 10 5 Fourier analysis peaks at k = 2 m 2 L position: independent of F 0 ν Earth matter effects in ν e scenario B ruled out R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
42 Determining the Mass Hierarchy: Observables Earth matter effects channel: ν e Earth matter effects observed scenario A/C confirmed not observed scenario B? P A,C ēē = cos 2 θ 12 P B ēē 0 R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
43 Determining the Mass Hierarchy: Observables Earth matter effects channel: ν e Earth matter effects observed scenario A/C confirmed not observed scenario B? NO! scenario B A/C with very similar initial fluxes F 0 ν 0 P A,C ēē = cos 2 θ 12 P B ēē 0 R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
44 Outline Determining the Mass Hierarchy: Observables Shock wave propagation 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
45 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation SN progenitor density profile R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
46 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation shock wave propagation SN progenitor density profile [Schirato and Fuller, 2002] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
47 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation shock wave propagation breaks adiabaticity P surv (E, t) forward forward+reverse [Schirato and Fuller, 2002] [Fogli et al., 2003, Lunardini and Smirnov, 2003, R. T., Kachelrieß, Raffelt, Dighe, Janka and Scheck, 2004, Fogli et al., 2004, Barger et al., 2005] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
48 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation effect depends on ν scheme Case Hierarchy sin 2 θ 13 ν e ν e A Normal > 10 3 B Inverted > 10 3 C Any < 10 5 R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
49 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation effect depends on ν scheme Case Hierarchy sin 2 θ 13 ν e ν e A Normal > 10 3 B Inverted > 10 3 time structure independent of F 0 : presence of dips C Any < 10 5 R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
50 Determining the Mass Hierarchy: Observables Shock wave propagation Shock wave propagation effect depends on ν scheme Case Hierarchy sin 2 θ 13 ν e ν e A Normal > 10 3 B Inverted > 10 3 time structure independent of F 0 : presence of dips C Any < 10 5 if dips observed in ν e scenario B confirmed R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
51 Determining the Mass Hierarchy: Observables Shock wave propagation channel: ν e Earth matter effects observed scenario A/C confirmed not observed scenario B? NO! scenario B very similar initial fluxes F 0 ν 0 P A,C ēē = cos 2 θ 12 P B ēē 0 shock wave propagation signal scenario B R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
52 Determining the Mass Hierarchy: Observables Shock wave propagation channel: ν e Earth matter effects observed scenario A/C confirmed not observed scenario B? NO! scenario B very similar initial fluxes F 0 ν 0 P A,C ēē = cos 2 θ 12 P B ēē 0 shock wave propagation signal scenario B how can we disentangle A from C? R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
53 Determining the Mass Hierarchy: Observables Shock wave propagation channel: ν e Earth matter effects observed scenario A/C confirmed not observed scenario B? NO! scenario B very similar initial fluxes F 0 ν 0 P A,C ēē = cos 2 θ 12 P B ēē 0 shock wave propagation signal scenario B how can we disentangle A from C? channel: ν e P A ee 0 P B,C = sin 2 θ 12 neutronization burst R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
54 Outline Determining the Mass Hierarchy: Observables Neutronization burst 1 Introduction Determination of the Neutrino Mass Hierarchy Role of Core-collapse Supernovae 2 Core-collapse Supernova Neutrinos Neutrino Emission Neutrino Propagation Neutrino Detection 3 Determining the Mass Hierarchy: Observables Earth matter effects Shock wave propagation Neutronization burst 4 Summary R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
55 Determining the Mass Hierarchy: Observables Neutronization burst Neutronization burst intense and short ( 20 ms) ν e emission as shock wave reaches ν-sphere R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
56 Determining the Mass Hierarchy: Observables Neutronization burst Neutronization burst intense and short ν e emission progenitor mass Robust feature of SN simulations e capture rates EOS R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
57 Determining the Mass Hierarchy: Observables Neutronization burst Neutronization burst intense and short ν e emission progenitor mass Robust feature of SN simulations e capture rates EOS Case Hierarchy sin 2 θ 13 P ee ν e ν properties A Normal > B Inverted > 10 3 sin 2 θ 12 C Any < 10 5 sin 2 θ 12 SN distance R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
58 Determining the Mass Hierarchy: Observables Neutronization burst Neutronization burst detection: ν e channel + big detectors water Cherenkov: ν + e ν + e time structure Gadolinium + angular-energy cuts (1 Mton detector) SN models uncertainties smaller than statistical errors [Kachelrieß, R. T, Buras, Janka, Marek and Rampp, 2005] R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
59 Summary Summary Core-collapse SNe : powerful source of neutrinos if galactic O( ) events expected ν properties information SN physics if F 0 ν 0 megaton water Cherenkov detector: Case Hierarchy sin 2 θ 13 Earth shock wave ν e peak A Normal > 10 3 B Inverted > 10 3 C Any < 10 5 R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
60 More information shock wave R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
61 More information neutronization R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
62 Bibliography T. Totani, K. Sato, H. E. Dalhed and J. R. Wilson, Future detection of supernova neutrino burst and explosion mechanism, Astrophys. J. 496 (1998) 216 M. T. Keil, G. G. Raffelt and H. T. Janka, Monte Carlo study of supernova neutrino spectra formation, Astrophys. J. 590 (2003) 971 C. Lunardini and A. Y. Smirnov, Probing the neutrino mass hierarchy and the 13-mixing with supernovae, JCAP 0306 (2003) 009 C. Lunardini and A. Y. Smirnov, Supernova neutrinos: Earth matter effects and neutrino mass spectrum, Nucl. Phys. B 616 (2001) 307 A. S. Dighe, M. T. Keil and G. G. Raffelt, Detecting the neutrino mass hierarchy with a supernova at IceCube, JCAP 0306 (2003) 005 A. S. Dighe, M. T. Keil and G. G. Raffelt, R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
63 Bibliography Identifying earth matter effects on supernova neutrinos at a single detector, JCAP 0306 (2003) 006 A. S. Dighe, M. Kachelriess, G. G. Raffelt and R. Tomàs, Signatures of supernova neutrino oscillations in the earth mantle and core, JCAP 0401 (2004) 004 R. C. Schirato, G. M. Fuller, (. U. (. LANL), UCSD and LANL), Connection between supernova shocks, flavor transformation, and the neutrino signal, arxiv:astro-ph/ G. L. Fogli, E. Lisi, D. Montanino and A. Mirizzi, Analysis of energy- and time-dependence of supernova shock effects on neutrino crossing probabilities, Phys. Rev. D 68 (2003) R. Tomas, M. Kachelrieß, G. Raffelt, A. Dighe, H. T. Janka and L. Scheck, Neutrino signatures of supernova shock and reverse shock propagation, JCAP 0409 (2004) 015 G. L. Fogli, E. Lisi, A. Mirizzi and D. Montanino, R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
64 Bibliography Probing supernova shock waves and neutrino flavor transitions in next-generation water-cherenkov detectors, arxiv:hep-ph/ V. Barger, P. Huber and D. Marfatia, Supernova neutrinos can tell us the neutrino mass hierarchy independently of flux models, arxiv:hep-ph/ M. Kachelriess, R. Tomas, R. Buras, H. T. Janka, A. Marek and M. Rampp, Exploiting the neutronization burst of a galactic supernova, Phys. Rev. D 71 (2005) S. Ando, J. F. Beacom and H. Yürkel astro-ph/ S. Ando and K. Sato, Relic neutrino background from cosmological supernovae, New J. Phys. 6 (2004) 170 L. E. Strigari, J. F. Beacom, T. P. Walker and P. Zhang, R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
65 Bibliography The concordance cosmic star formation rate: Implications from and for the supernova neutrino and gamma ray backgrounds, arxiv:astro-ph/ I. Gil-Botella et al. M. Maltoni, T. Schwetz, M. A. Tortola and J. W. F. Valle, New J. Phys. 6 (2004) 122. C. Lunardini, Phys. Rev. D 73 (2006) A. M. Hopkins and J. F. Beacom, arxiv:astro-ph/ R. Tomàs (AHEP Group -IFIC) Identifying the neutrino mass hierarchy with SN ν s IPM School & Conference on Lepton / 31
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