Astrophysical Neutrino at HK

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3 Astrophysical Neutrino at HK Solar neutrino Burning processes, modeling of the Sun Property of neutrino Supernova ν NASA, Chandra & Hubble μpc kpc Mpc SN explosion mechanism SN monitor Nucleosynthe sis SN relic ν wikimedia HK NASA, Hubble 2009 SN mechanism Star formation history Extraordinary SNe Mpc and DM annihilation, GRB ν 3

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5 χ 2 m 2 in ev x10-5 1σ σ 2σ preliminary Same ~2σ tension with KamLAND in Δm 2 21 Solar+KamLAND KamLAND sin 2 θ13=0.0242± Solar sin 2 12 = m 2 21 = sin 2 12 = m 2 21 = sin 2 12 = m 2 21 = σ 2σ 3σ The unit of Δm 2 21 is 10-5 ev 2 Y. Koshio, Neutrino h Aug Workshop for neutrino program in Japan 31 Y. Nakano ICRC2015 5

6 θ Z All solar sin 2 (θ 12 ) = Δm 2 21 = 4.85x10-5 ev 2 Solar+KamLAND sin 2 (θ 12 ) = Δm 2 21 = 7.50x10-5 ev 2 D/N best sin 2 (θ 12 ) = Δm 2 21 = 4.17x10-5 ev 2 6 1σ Solar 1σ KamLAND expected sin 2 θ12=0.314, sin 2 θ13=0.025 SK I- IV Combined StaBsBcal Error Only preliminary P.Weatherly WIN2015 SK-I,II,III,IV combined 1σ range PRL 112, (2014)

7 - 5 original figure: P.Weatherly WIN2015 preliminary KamLAND ν All solar exp. + SK D/N D/N asymmetry D-N 2(D+N) ±1σ region with Hyper- K 10years *assumuing solar best Δm 2, stabsbc (signal and background) error only 7

8 Solar Neutrino : Hep small branch not detected yet Takeuchi-san s slide SK-I energy resolution (40% photo-coverage) no oscillation stat. error only J.N. Bahcall and A.M. Serenelli, Astro. Phys. J. 621, 85 (2005) 6th Aug P(ν e ν e ) Lower threshold It"can"be"seen"with"40%"P.C."cannot" reduce sys. error good energy resolution reduce stat. error is required sys. error ~300"events/"5Mtyears"(>17MeV)" sin 2 (θ) Δm 2 (ev 2 ) 6.3 x x x x x 10-5 Workshop for neutrino program in Japan Koshio - ν e Challenge: survival probability recoil electron spectrum Energy"resolu+on"at"higher"energy" large background ~10% from upturn (~20"MeV)"is"important." should be seen the tail of 8 B solar neutrino with"14%"p.c.."" difficult to extract the hep signal with SK-II energy resolution 8

9 NASA, Chandra & Hubble

10 Features Detection of neutronization ν Measurement of supernova burst time Better directional measurement for SN monitor Energy spectrum measurement Extraordinary SN (BH, dim SN) Handreds of events for neutronizaiton 10

11 Two kind of short Bme variance is proposed from 3D MC simulabon. ConvecBon (SASI) : ± kpc RotaBon : ± 40 10kpc ConvecBon leads an explosion to 3D simulabon model. - > DetecBon/frequency analysis of these variance is important input to supernova theories. SASI Takiwaki (Standing Accretion Shock Instability) Pressure Wave Scheck Neutrino signals from rotating model TOP SIDE Advective-acoustic cycle From Foglizzo s slides Vorticity Wave Standing Accretion Shock Instability(SASI) Takiwaki+ in prep Period of spiral mode is extracted by ν-signal 11 29

12 12

13 Physics of SRN Lunardini (2009) Stellar birth rate(=collapse rate) and Bright collapse rate Horiuchi Event spectra with uncertainbes Horiuchi et.al (2011) with data from Dahlen et.al (2012) Adopted from Horiuchi et al. (2009) 13

14 SRN measurement with HK nσ SRN with Hyper-K 200 SRN events are expected between 20 MeV and 30 MeV, with Hyper-Kamiokande 10 years sigma detection of SRN is expected Mton μ 2 LMA SRN model assumed SRN with Hyper-K+Gd By adding Gadolinium and applying neutrino tagging, we can lower the analysis threshold down to MeV. νe + p -> e+ + n Gd + n -> Gd +γs ( 8 MeV) With Gd, the measurement of Tν and model separation will be possible years HMA LMA HBD 6MeV Chemical Evolution Population Synthesis CGI 14

15 15

16 Solar neutrino fluxes of models. J.N. Bahcall and A.M. Serenelli, Astro. Phys. J. 621, 85 (2005) Table 2: Predicted solar neutrino fluxes from seven solar models. The table presents the predicted fluxes, in units of (pp), 10 9 ( 7 Be), 10 8 (pep, 13 N, 15 O), 10 6 ( 8 B, 17 F), and 10 3 (hep) cm 2 s 1 for the same solar models whose characteristics are summarized in Table 1. Model pp pep hep 7 Be 8 B 13 N 15 O 17 F BP04(Yale) BP04(Garching) BS BS05( 14 N) BS05(OP) BS05(AGS,OP) BS05(AGS,OPAL)

17 Solar neutrino upturn Maltoni et al. hkp://arxiv.org/pdf/ pdf Brx (pp) KL ( 7 Be) Brx (pep) Borexino ( 8 B) Super-K SNO 0.6 P ee = Φ CC / Φ NC pp Brx ( 7 Be) Standard Sterile NSI-up NSI-dw E ν [MeV] 17

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