Distinguishing supernova-ν flavour equalisation from a pure MSW effect

Transcription

1 Distinguishing supernova-ν flavour equalisation from a pure MSW effect based on arxiv: (accepted on PRD), with B. Dasgupta and A. Mirizzi FRANCESCO CAPOZZI

2 Outer layer Accretion phase (t < 0.5 s) Shock wave νβ να ν sphere R ~ 10 km να νβ α, β = e, x 2

3 [1] Dighe, Smirnov, 2000 [2] Schirato, Fuller, 2002 [3] Fogli, Lisi, Mirizzi, Montanino, 2002 MSW effect νe e W e νe ν sphere R ~ 10 km R [10 3,10 5 ] km 3

4 [1] Dighe, Smirnov, 2000 [2] Schirato, Fuller, 2002 [3] Fogli, Lisi, Mirizzi, Montanino, 2002 MSW effect normal ordering (NO) νe e W e νe νe νx ~70% νe ν sphere R ~ 10 km νe ~30% νx R [10 3,10 5 ] km 4

5 [1] Dighe, Smirnov, 2000 [2] Schirato, Fuller, 2002 [3] Fogli, Lisi, Mirizzi, Montanino, 2002 MSW effect inverted ordering (IO) νe e W e νe νx ~70% νe ν sphere R ~ 10 km νe ~30% νx R [10 3,10 5 ] km νe 5

6 [1] Sawyer, [2] Chakraborty, Hansen, Izaguirre, Raffelt, 2016 ( ) ν ( ) ν [3] Dasgupta, Mirizzi, Sen 2016 [4] Capozzi, Dasgupta, Lisi, Marrone, Mirizzi, 2017 Fast conversions ( ) ν Z ( ) ν ν sphere R ~ 10 km R ~ Rν-sphere 6

7 [1] Sawyer, [2] Chakraborty, Hansen, Izaguirre, Raffelt, 2016 ( ) ν ( ) ν [3] Dasgupta, Mirizzi, Sen 2016 [4] Capozzi, Dasgupta, Lisi, Marrone, Mirizzi, 2017 Fast conversions ( ) ν Z ( ) ν νe νx ~33.3% ~66.6% ν sphere νe R ~ 10 km νe ~33.3% ~66.6% νx R ~ Rν-sphere νe 7

8 [1] Sawyer, [2] Chakraborty, Hansen, Izaguirre, Raffelt, 2016 [3] Dasgupta, Mirizzi, Sen 2016 [4] Capozzi, Dasgupta, Lisi, Marrone, Mirizzi, 2017 Fast conversions ( ) ν ( ) ν Z ( ) ν ( ) ν νe νx ~33.3% ~66.6% ν sphere WORK IN PROGRESS R ~ 10 km νe νe ~33.3% ~66.6% νx R ~ Rν-sphere νe 8

9 SNν flavour conversions: summary A list of possible flavour conversion scenarios ME = Matter effects (MSW) FE = flavour equalisation 9

10 SNν flavour conversions: summary A list of possible flavour conversion scenarios Flavour equalisation is still under investigation. 10

11 SNν flavour conversions: summary A list of possible flavour conversion scenarios Flavour equalisation is still under investigation. Can we distinguish scenarios experimentally? 11

12 SNν fluxes 12

13 SN fluxes: Wroclaw/Basel 1D model (W) (Un)Oscillated (Anti)Neutrino energy fluxes Neutrinos Antineutrinos 10 F [a.u.] F [a.u.] 0 ν ν e ν e ν x Matter (NO) Matter (IO) Flavor eq. Fit parameters from: Fischer, et al., Astron. Astrophys. 517, A80 (2010) E ν [MeV] [MeV] In NO differences in Pee for both ν and ν E ν 13

14 SN fluxes: Garching 1D model (G) (Un)Oscillated (Anti)Neutrino energy fluxes Neutrinos Antineutrinos 10 F [a.u.] F [a.u.] 0 ν ν e ν e ν x Matter (NO) Matter (IO) Flavor eq. Fit parameters from: Serpico, et al., Phys. Rev. D85, (2012) E ν [MeV] E ν [MeV] Smaller differences compared to W model 14

15 1) Three SNν detection channels 15

16 JUNO: ν-proton elastic scattering (pes) ( ) W model ( ) νe,μ,τ + p > νe,μ,τ + p G model Number of Events JUNO pes ν x ν e ν e JUNO E vis [MeV] E vis [MeV] JUNO is sensitive mainly to νx and to Eν > 25 MeV. No dependence on flavour conversions 16

17 Hyper-Kamiokande: inverse β decay Number of Events IBD W model Matter (NO) Matter (IO) Flavor eq. E vis νe + p > e + + n [MeV] Hyper-K G model E vis [MeV] Hyper-K Hyper-K is sensitive to νe 17

18 DUNE: ν-cc scattering on 40 Ar (ArCC) νe + 40 Ar > e K* W model G model Number of Events ArCC Matter (NO) Matter (IO) Flavor eq. DUNE DUNE E vis [MeV] E vis [MeV] DUNE is sensitive to νe 18

19 2) Reconstructing oscillated ν-fluxes 19

20 Reconstructing ν flux from pes N i E i vis! df pes de ' df x de [1] H. L. Li, Y. F. Li, M. Wang, L. J. Wen and S. Zhou, Phys. Rev. D 97 (2018) no.6, [2] B. Dasgupta and J. F. Beacom, Phys. Rev. D 83 (2011) ] -1 W model G model MeV 3 9 cm -2 2 df pes /de ν [ E ν [MeV] E ν [MeV] Similar reconstruction method applies to IBD and ArCC 20

21 3) Flux ratios: normal ordering (NO) 21

22 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F ArCC x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 22

23 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F ArCC x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 23

24 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F ArCC x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 R > 6 disfavours matter effects only scenario 24

25 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F ArCC x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 R > 6 disfavours matter effects only scenario R < 6 disfavours flavour equalisation scenario 25

26 Statistical significance: R at 10 kpc 7 W model 7 G model R = F pes /F ArCC σ(r) σ(r) E ν [MeV] E ν [MeV] P ee = 0.1 P ee = 0.2 Flavor eq. Matter (NO) In the case of pure matter effects we can disfavour flavour equalisation at ~2σ (only for W model) 26

27 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F IBD x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 27

28 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F IBD x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 28

29 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F IBD x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 R > 6 disfavours flavour equalization scenario 29

30 Flux ratio: R For Eν > 25 MeV, we define: R = F pes F IBD x = F 0 e F 0 x apple 1 x = F 0 e F 0 x apple 1 R > 6 disfavours flavour equalization scenario R ~ 5-6 leads to degeneracy between scenarios 30

31 Statistical significance: R at 10 kpc R = F pes /F IBD σ(r) σ(r) W model E ν [MeV] E ν [MeV] In the case of pure matter effects we can disfavour flavour equalization at >~2σ (only for W model) G model P ee = 0.4 P ee = 0.6 Flavor eq. Matter (NO) 31

32 Statistical significance: R and R at 1 kpc R = F pes /F ArCC G model P ee = 0.1 P ee = 0.2 Flavor eq. Matter (NO) R = F pes /F IBD G model P ee = 0.4 P ee = 0.6 Flavor eq. Matter (NO) σ(r) σ(r) E ν [MeV] σ(r) σ(r) E ν [MeV] Significance > 3σ for almost all scenarios 32

33 3) Flux ratios: inverted ordering (IO) 33

34 Statistical significance: R at 10 kpc 6 W model 6 G model R = F pes /F IBD P ee = 0.1 P ee = 0.2 Flavor eq. Matter (IO) σ(r) σ(r) E ν [MeV] E ν [MeV] IO is unfavourable for distinguishing scenarios at 10 kpc 34

35 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 35

36 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 36

37 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 2) for each channel we extract the oscillated flux df/deν 37

38 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 2) for each channel we extract the oscillated flux df/deν 3) we calculate the ratio R=FpES/FArCC and R=FpES/FIBD 38

39 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 2) for each channel we extract the oscillated flux df/deν 3) we calculate the ratio R=FpES/FArCC and R=FpES/FIBD ( ) 4) we compare R with expectations for different scenarios 39

40 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 2) for each channel we extract the oscillated flux df/deν 3) we calculate the ratio R=FpES/FArCC and R=FpES/FIBD ( ) 4) we compare R with expectations for different scenarios Our method can be improved and extended to all SN classes 40

41 Conclusions We propose a method to distinguish experimentally SNν flavour equalisation from pure matter effects. Brief summary: 1) we need three channels: pes, IBD and ArCC 2) for each channel we extract the oscillated flux df/deν 3) we calculate the ratio R=FpES/FArCC and R=FpES/FIBD ( ) 4) we compare R with expectations for different scenarios Our method can be improved and extended to all SN classes Our method is independent from the knowledge of F 0 ν 41

42 Thank you

43 Backup

44 [1] Pantaleone, 1992 [2] Hannestad, Raffelt, Sigl, Wong, 2006 [3] Duan, Fuller, Carlson, Qian, 2006 [4] Fogli, Lisi, Marrone, Mirizzi, 2007 Self-induced (slow) ( ) ν Z ( ) ν conversions ( ) ν ( ) ν ν sphere R ~ 10 km R [10 2, few 10 2 ] km 44

45 [1] Pantaleone, 1992 [2] Hannestad, Raffelt, Sigl, Wong, 2006 [3] Duan, Fuller, Carlson, Qian, 2006 Self-induced (slow) [4] Fogli, Lisi, Marrone, Mirizzi, 2007 ( ) ν Z ( ) ν conversions ( ) ν ( ) ν νe νx ~33.3% ~66.6% ν sphere νe R ~ 10 km νe ~33.3% ~66.6% νx R [10 2, few 10 2 ] km νe 45

46 [1] Pantaleone, 1992 [2] Hannestad, Raffelt, Sigl, Wong, 2006 [3] Duan, Fuller, Carlson, Qian, 2006 [4] Fogli, Lisi, Marrone, Mirizzi, 2007 Slow conversions ( ) ν ( ) ν Z ( ) ν ( ) ν νe νx ~33.3% ~66.6% ν sphere WORK IN PROGRESS R ~ 10 km νe νe ~33.3% ~66.6% νx R [10 2, few 10 2 ] km νe 46

47 SN fluxes: parametrization We adopt the following parametrisation: F 0 (E) = 0 f 0 (E) f 0 (E) = 1 he i (1 + ) 1+ (1 + ) E he i exp apple (1 + ) E he i = 2hE i 2 he 2 i he 2 i he i 2 [1] M. Keil, G. G. Raffelt, and H.-T. Janka, Astrophys. J. 590, (2003) 47

48 SN fluxes: parametrization List of fit parameters for W and G models 48

49 JUNO: ν-proton elastic scattering (pes) ( ) νe,μ,τ + p > ( ) νe,μ,τ + p dn pes de vis = N p Z +1 0 dt 0 p dt p dt 0 p W (T 0 p,e vis ) Z 1 E 0 de F pes (E ) d pes(e,t p ) dt p F pes 4F 0 x + F 0 e + F 0 e W (T 0 p,e vis )= exp( (T 0 p E vis) 2 2 E 2 p 2 E ) E E vis =0.03 p E vis /MeV 49

50 Hyper-Kamiokande: inverse β decay νe + p > e + + n dn IBD de vis = N p Z 1 E T de F IBD (E ) IBD (E ) W (E MeV, E vis ) F IBD 8 < : 0.7F 0 e +0.3F 0 x matter e ects only, with NO F 0 x 0.33F 0 e +0.66F 0 x flavor eq. matter e ects only, with IO E E vis =0.6 p E vis /MeV 50

51 DUNE: ν-cc scattering on 40 Ar (ArCC) dn ArCC de vis F ArCC = N Ar 8 < : F 0 x N ex X i=1 νe + 40 Ar > e K* Z 1 0 de F ArCC (E ) i ArCC(E ) W (E vis,t e ) matter e ects only, with NO 0.3F 0 e +0.7F 0 x matter e ects only, with IO 0.33F 0 e +0.66F 0 x flavor equalization E =0.11 p E vis /MeV E vis /MeV 51

52 Reconstructing ν flux from pes We define the extrema and midpoint for the neutrino qenergy bins as [E i ν,e i+1 ν] and E i ν, respectively, where E i = Tpm i p /2 d F pes de Ē N = N N pes K NN 0 1 d F pes de Ē i i pes + X j>i d F pes de Ē j K ij A /K i,i, K i,j = N p T 0i p dt p dt 0 p T 0i p d pes (E,T p ) dt p ( T 0i p,ēj ) 52

53 Reconstructing ν flux from IBD and ArCC d F IBD de Ē i = N p 1 tot IBD (Ēi) N i IBD E i vis d F ArCC de Ē i = N Ar 1 tot ArCC (Ēi) N i ArCC E i vis 53

54 Flux ratios: R and R, normal ordering 54

55 Flux ratios: R and R, inverted ordering 55