Analysis of supernova neutrino fluxes and neutron star properties - PowerPoint PPT Presentation

Analysis of supernova neutrino fluxes and neutron star properties Andrea Gallo Rosso Gran Sasso Science Institute Astroparticule et Cosmologie (APC) Advisors: F. Vissani and C. Volpe 5 th April 2019

List of publications A. Gallo Rosso et al . JCAP 1812 (2018) no.12, 006. V. Gentile et al . JCAP 2018 (2018) no.08, 015. Theoretical Papers A. Gallo Rosso et al . JCAP 1804 (2018) no.04, 040. A. Gallo Rosso et al . JCAP 1711 (2017) no.11, 036. A. Gallo Rosso et al . EPJ Plus 133 (2018) no.7, 267. Theoretical Reviews G. Fantini et al . [ISBN:9789813226081]. E. Aprile et al. Phys.Rev.Lett. 122 (2019) 071301. E. Aprile et al. Phys.Rev.Lett. 121 (2018) no.11, 111302. E. Aprile et al. Phys.Rev. D97 (2018) no.9, 092007. E. Aprile et al. Phys.Rev. D96 (2017) no.12, 122002. E. Aprile et al. Eur.Phys.J. C77 (2017) no.12, 881. XENON collaboration E. Aprile et al. Eur.Phys.J. C78 (2018) no.2, 132. E. Aprile et al. Phys.Rev.Lett. 119 (2017) no.18, 181301. E. Aprile et al. Phys.Rev. D96 (2017) no.4, 042004. E. Aprile et al. Eur.Phys.J. C77 (2017) no.12, 890. … 1

Introduction

Before After SN 1987A

Introduction SN H no yes SN I SN II He H dominant dominant Si yes SN IIb SN IIL (linear) no SN Ia SN IIF (faint) SN IIpec (peculiar) He rich poor SN IIP (plateau) SN IIn (narrow) SN Ib SN Ic 3 THERMONUCLEAR CORE COLLAPSE

Introduction CORE-COLLAPSE SUPERNOVA EXPLOSION • Longstanding open question in astrophysics • ∼ 10 53 erg gravitational binding energy • 99% emitted in neutrinos • ∼ 10 s signal • Delayed-accretion paradigm • From Wilson (1971) & Bethe and Wilson (1985) • To 2D & 3D numerical simulations 4

Introduction DELAYED EXPLOSION 1. Instability & collapse 2. Bounce & shock propagation 3. Stallation & accretion 4. Cooling T. Totani et al., Astrophys. J. 496 (1998). 5

Introduction NEUTRINO MESSENGERS • Weakly interacting • 99% of binding energy emitted in neutrinos • 6 flavors: ν e ν µ ν τ ν e ν µ ν τ • Flavor transformation • Vacuum: determined with good accuracy • Matter conversion: Mikheyev-Smirnov-Wolfenstein effect (MSW) [1] • Self-interaction effects in dense media still studied 1 L. Wolfenstein, Phys. Rev. D17 (1978). S.P. Mikheyev and A.Y. Smirnov, Sov. J. Nucl. Phys. 42 (1985). 6

Introduction WHAT CAN WE LEARN FROM SUPERNOVA NEUTRINOS? • Star properties • Pointing and alert (SNEWS) • Standard candle ( ν e burst) • Explosion mechanism • Particle properties • Flavor conversion in dense media • Non-standard properties 7

Introduction SN 1987A: THE ONLY NEUTRINO SIGNAL (SO FAR) • Large Magellanic Cloud (51 . 4 kpc) • Kamiokande-II, IMB, Baksan • About 25 ν e neutrino events • Inverse Beta Decay Only • ν e ν µ ν τ ν µ ν τ still missing • Good agreement with expectations • F. Vissani, J. Phys. G 42, 013001 (2015). • Radiated ν e energy ( 4 . 8 + 2 . 3 − 1 . 0 ) × 10 52 erg • ν e temperature ( 3 . 9 + 0 . 5 − 0 . 3 ) MeV 8

Introduction Kamiokande-II ∼ 10 × Super-Kamiokande ∼ 10 × Hyper-Kamiokande MANY DETECTION CHANNELS — ENERGY, TIME, FLAVOR 9

Introduction Time integrated flux [ 10 10 MeV - 1 cm - 2 ] 2.5 ν e ν e 2.0 ν x = ν μ , ν μ , ν τ , ν τ 1.5 1.0 0.5 0.0 0 10 20 30 40 Neutrino energy [ MeV ] TIME INTEGRATED FLUX (FLUENCE) Total energy E normalization ⇔ 1 st moment Mean energy ⟨ E ⟩ ⇔ Pinching α width ⇔ 3 PARAMETERS × 3 SPECIES = 9 D.O.F. 10

Introduction TIME INTEGRATED FLUX (FLUENCE) Total energy E normalization ⇔ 1 st moment Mean energy ⟨ E ⟩ ⇔ Pinching α width ⇔ 3 PARAMETERS × 3 SPECIES = 9 D.O.F. 10

Introduction NUMBER OF PARAMETERS ARBITRARILY REDUCED • Lu et al. [2] JUNO detector • Importance of combining channels • E ν e up to 5% @ 90% C.L. • ⟨ E ν e ⟩ up to 1% @ 90% C.L. with MSW transformation w/o equipartition ( E tot ̸ = E i / 6) E tot known up to 13% but for spectral shape (i.e. pinching) fully known 2 Lu et al. Phys. Rev. D 94, 023006 (2016). 11

Introduction DIFFICULTY IN RECONSTRUCTING THE BINDING ENERGY • H. Minakata et al. [3] • Hyper-Kamiokande • only ν e + p → e + + n • If pinching unknown • E ν e acc. 50% @ 3 σ • ⟨ E ν e ⟩ acc. 4% @ 3 σ • Parameter degeneracy 3 H. Minakata et al. , JCAP 0812, 006 (2008). 12

WHAT CAN WE LEARN FROM SUPERNOVA NEUTRINOS? • How well can we reconstruct the neutrino fluxes without any usual assumptions? • Will the uncertainty on the pinching compromise the determination of key properties? • What is the impact of including other detection channels? • What can we infer on the neutron star properties? 13

1. FLUX RECONSTRUCTION AND M – R RELATION OF THE NEUTRON STAR • Monte Carlo based likelihood analyses • Without usual assumptions • Shape α unknown • Three detection channels (9 d.o.f.) • ν e + p → e + + n (IBD) • ν + e − → ν + e − (ES) • ν + 16 O → ν + X + γ (OS) REFERENCE PAPERS • A. Gallo Rosso, F. Vissani, M.C. Volpe, JCAP 1711 (2017) no.11, 036 • A. Gallo Rosso, F. Vissani, M.C. Volpe, JCAP 1804 (2018) no.04, 040 14

2. LATE-TIME SIGNAL AND PROTO-NEUTRON STAR RADIUS • First analysis of its kind • Neutrino signal alone • Reference model • Exploration of extended theories of gravity REFERENCE PAPER • A. Gallo Rosso, S. Abbar, F. Vissani, M.C. Volpe, JCAP 1812 (2018) no.12, 006 15

1. Flux reconstruction

1. Flux reconstruction Hypotheses and method

Hypotheses and method SUPERNOVA PARAMETERS • Distance D ∗ = 10 kpc • Total energy E ∗ = 3 × 10 53 erg DETECTORS • Super-Kamiokande • 22 . 5 kton (fiducial mass) • Hyper-Kamiokande • 374 kton (fiducial mass) • 5 MeV threshold • 100% efficiency 16

Hypotheses and method Time integrated flux [ 10 10 MeV - 1 cm - 2 ] TIME-INTEGRATED FLUXES (FLUENCES) 2.5 ν e ν e 2.0 ν x = ν μ , ν μ , ν τ , ν τ • Quasi-thermal alpha-fit [4] 1.5 1.0 • 3 neutrino species ( ν e , ν e , ν x ) 0.5 0.0 • 3 parameters ( E , ⟨ E ⟩ , α ) 0 10 20 30 40 Neutrino energy [ MeV ] d F 0 ( α i + 1 ) ( α i + 1 ) E α i − ( α i + 1 ) E [ ] E i i = ⟨ E i ⟩ α i + 2 exp d E ν 4 π D 2 Γ( α i + 1 ) ⟨ E i ⟩ • Agreement with SN 1987A data • Good description of simulations 4 M.T. Keil et al., Astrophys. J. 590 (2003). 17

Hypotheses and method NEUTRINO FLAVOR TRANSFORMATIONS IN SUPERNOVAE • Normal mass hierarchy • Mikheyev-Smirnov-Wolfenstein (MSW) effect F ν e = F 0 { x F ν e = | U e 1 | 2 · F 0 ν e + ( 1 − | U e 1 | 2 ) · F 0 x • Neutrino self-interaction neglected 18

Hypotheses and method TOTAL ENERGIES i = 0 . 5 × 10 53 erg • E ∗ MEAN ENERGIES • ⟨ E ν e ⟩ ∗ = 9 . 5 MeV • ⟨ E ν e ⟩ ∗ = 12 MeV • ⟨ E ν x ⟩ ∗ = 15 . 6 MeV PINCHING PARAMETERS • α ∗ i = 2 . 5 C. Lujan-Peschard et al., JCAP (2014). Teun Hocks, Measuring 19

Hypotheses and method — HYPER-KAMIOKANDE EXTRACTED EVENTS — × 10 3 600 Expected distribution True distribution 10 Extracted events Extracted events 500 8 400 6 300 4 200 2 100 10 20 30 40 50 60 0 5 10 15 20 25 30 35 E e [ MeV ] K e [ MeV ] ν + e − → ν + e − ν e + p → e + + n (76 × 10 3 expected events) (4 × 10 3 expected events) 20

Hypotheses and method ν + 16 O → ν + X + γ 3 • γ within (4 ÷ 9) MeV Signal [a.u.] 2 • ∼ 800 OS • ∼ 8000 IBD+ES 1 • Non-Gaussian smearing • No disentangling IBD+ES 0 • Neutral-Current Region 0 5 10 15 20 25 Energy [MeV] → NCR = IBD + ES + OS ֒ K. Langanke et al., Phys. Rev. Lett. 76 (1996). 21

Hypotheses and method NEUTRINO-OXYGEN CROSS SECTION σ OS ( E ν ) ≈ κ · σ 0 · ( E ν / MeV − 15 ) 4 [5] • measurements expected [6] • 10% uncertainty (optimistic) 10th parameter κ • Systematic ∼ Gauss( κ ∗ = 1, σ κ = 0 . 1) • Results weakly concerned 5 J.F. Beacom and P. Vogel, PRD 58 (1998) 053010. 6 K. Scholberg, talk at CNNP2017. 22

Analysis of supernova neutrino fluxes and neutron star properties - PowerPoint PPT Presentation

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