Cecilia Lunardini Arizona State University RIKEN BNL Research Center SUPERNOVA NEUTRINOS AT FUTURE DETECTORS

Transcription

1 Cecilia Lunardini Arizona State University RIKEN BNL Research Center SUPERNOVA NEUTRINOS AT FUTURE DETECTORS The SeaBle, July

2 20 years back: the impact of SN1987A What did we learn?

3 Plot from: Inverse beta decay: anr ν e + p n + e +

4 ~ 1 Kt water/scinrllator detectors Bionta et al., PRL 58,1987, Hirata et al., PRL 58,1987, Alekseev et al. JETP LeB. 45 (1987)

5 First confirmaron of theory Luminosity ~ total energy budget Energy emibed is of gravita)onal nature: L ν ~ G M 2 f/r f G M 2 i/r i ~ ergs (R f ~ 10 Km) Energy spectrum: ~ Fermi Dirac (thermal) E ~ 3.15 T ~ MeV DuraRon of neutrino burst ~ diffusion Rme Time ~ (size 2 )/(mean free path) ~ 10 s

6 Open quesrons Precision? Time structure (accreron, cooling, ) OscillaRons (MSW, neutrino neutrino,..) Model discriminaron (Eq. of state, neutrino transport, ) New physics Total energy? All neutrino species What is typical?

7 The situaron now: opening a new phase

8 New focus on supernovae Solar, atmospheric fluxes down to precision phase (~10 40%) Time to approach more distant, more complex sources: supernovae, GRBs, Dark MaBer, Solar/atmospheric become backgrounds! New phase of detectors coming Larger (0.1 1 Mt) & more sensirve Clip art from M. Vagins

9 DUSEL The next generaron LANNDD Water Cherenkov, Mt HyperK, UNO, MEMPHYS, DeepTITAND Liquid scin)llator, kt LENA, Hano Hano Liquid Argon, kt LANNDD, GLACIER

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11 Looking farther 1 5 Mt mass ~ few Mpc reach ~ 1 SN every decade! Ando, Beacom & Yuksel, PRL95, 2005

12 and in more detail Events for Galac=c SN (K. Scholberg, talk at Neutrino 2006, Sante Fe, NM)

13 Themes for the future: what will we learn?

14 Timing Pons et al., Phys.Rev.Lett.86,2001 Late Rme evoluron new phases of maber TransiRon to transparency

15 SASI (Standing AccreRon Shock Instability) OscillaRons of shock front modulates neutrino luminosity Probes large scale convecron Blondin, Mezzacappa & DeMarino, ApJ 584 Marek, Janka & Mueller, Astron. Astrophys. 496, 475 (2009) T. Lund, A. Marek. C.L., H.T. Janka & G. Raffelt, arxiv:

16 ν e sensirvity Detector type process Expected mass Number of events (galac=c SN) Water Cherenkov ν e ( 16 O, 16 F)e ~1 Mt O(10^3 ) Liquid Argon ν e ( 40 Ar, 40 K)e <100 Kt < O(10^3 ) ScinRllator ν e ( 12 C, 12 B)e < 50 kt < O(10^2 )

17 H 2 O Fogli et al., JCAP 0504:002,2005

18 Total energy of SN Eq. of state NeutronizaRon/ deleptonizaron e (p,n) ν e Survival of neutroniza)on burst in ONeMg Sne! P(ν e ν e ) OscillaRon effects Neutrino mass spectrum flavor mixings progenitor type Duan et al.,prl.100,2008 C.L., B. Mueller, H.T. Janka PRD, 2008

19 OscillaRons: spectral distorrons p = survival probability Harder spectrum! Depends on masses, mixings

20 Star Neutrino oscillarons 10 8 g cm g cm g cm -3 vacuum Earth Neutrino-neutrino high MSW low (solar) MSW low (solar) MSW MaBer effects: Unique of supernovae! supernovae refracron frequency vacuum frequency Neutrino neutrino, neutrino electron

21 High MSW: θ 13 dependence test tan 2 θ 13 down to 10 5! Transition probability P H C. L. and A. Y. Smirnov, Nucl. Phys. B 616, 307 (2001), JCAP 0306, 009(2003);

22 Neutrino neutrino: spectral swaps Step like probability as funcron of energy Groups: Munich, UCSD, LANL, NCS, Trieste, Bari, Orsay, Arizona, Tata Inst., Dasgupta et al., arxiv:

23 SRll, a galacrc SN might take a while Clip art from M. Vagins

24 Diffuse flux: everything and now Sum over all SNe in the universe

25 Now: alterna)ve to a galac)c supernova! ConRnuous flux, no wai)ng )me might be everyday physics in future! ~20 events/year at Mt water Cherenkov Everything: probes the whole supernova popula)on of the universe What s typical? Cosmological SNe Diversity: Fe core, ONeMg core, black hole core,

26 Cosmological rate of SNe increases with z Horiuchi, Beacom & Dwek, 2009

27 Example: failed SNe M > M sun, 9 22% of collapses Too rare to have a galac)c one! S EOS LS EOS Collapse directly into black hole, no explosion Neutrinos hooer and more luminous Liebendörfer et al., ApJS, 150, 263, K. Sumiyoshi et al., PRL97, (2006), T. Fischer et al., (2008), , K. Nakazato et al., PRD78, (2008)

28 failed SNe may dominate! Best case: srff EoS, 22% failed SNe, maximum Close to SK limit! BH AnR nue flux NS C.L., arxiv: , Phys. Rev. LeB., 2009, J. G. Keehn and C.L., in prepararon

29 Best: ~ 100% enhancement Total NS BH

30 SN archaeology ScaOering of SN neutrinos change the chemical composi)on of the Earth! Radiochemical searches of SNe? W. C. Haxton and C. W. Johnson, Nature 333 (1988)

31 High energy threshold needed to suppress solar background Solar GalacRc SN, Rme averaged R.Lazauskas,C.L. and C.Volpe, JCAP 0904, 029 (2009)

32 97 Tc accumulates in molybdenum rocks: ν e ( 98 Mo,n e ) 97 Tc, ν e ( 97 Mo, e ) 97 Tc LifeRme: years (can t be primordial!) High energy threshold Haxton & Johnson, Nature, 1988 Spin dipole + mulrpoles QRPA GT+IAS, allowed approximaron R.Lazauskas,C.L. and C.Volpe, JCAP 0904, 029 (2009)

33 ~ 10 kt of rock needed IniRal experimental efforts made ~1988 K. Wolfsberg (LANL), unpublished, Wrong credit

34 Clues of Stellar Explosions Found Deep in Mine, Scien)sts Say, the New York Times, May 26, 1988 Moly techne)um used to track elusive neutrinos Focus: Advanced Materials, American Metal Market, Sept 11, 1991.

35 10 kt Mo ore, expected: Atoms of 97 Tc Solar only SN only Total % effect! Comparable to errors More precise cross secron and solar flux needed! R.Lazauskas,C.L. and C.Volpe, JCAP 0904, 029 (2009)

36 Wrap up

37 The post solar phase: supernovae, etc.. ~2020. : Discovery diffuse SN neutrino flux SN neutrinos become everyday physics Complement SN1987A Cosmological supernovae Averaged over whole SN popularon No precision!

38 The post solar phase: supernovae, etc.. ~ 2100: Precision Galac)c supernova All flavor detecron Model discriminaron Timing OscillaRon effects New physics Precision!

39 backup

40 Data (sparse) vs theory.. ~ 1 Kt water detectors Kamiokande Bionta et al., PRL 58,1987, Hirata et al., PRL 58,1987, PRD 38,1988 sin 2 θ 13 =10-4 Garching/ORNL Lawrence Livermore Arizona E/MeV IMB IMB 7/6/10 40

41 5 parameters fit, with oscillarons, marginalized (C.L., Astropart.Phys.,2006. ) 68,90,99% CL Lawrence Livermore Arizona Garching Totani et al., Astrophys. J. 496 (1998) Thompson, Burrows & Pinto, Astrophys. J. 592 (2003) Keil, Raffelt & Janka, Astrophys. J. 590 (2003)

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43 Upper limits and backgrounds SuperKamiokande (Malek et al., PRL, 2003): Energy window Red dashed: Homestake Solid, grey: Kamioka

44 Time integrated fluxes Shen et al. (S) EoS BH NS Progenitor: M=40 M sun, from Woosley & Weaver, 1995 K. Nakazato et al., PRD78, (2008)

45 La}mer Swesty. (LS) EoS

46 A two popularon model: diffuse flux C.L., arxiv: , Phys. Rev. LeB., 2009 anr ν e survival probability (Rme averaged, constant in energy)

47 Stronger cosmological (z>1) contriburon Black hole forming: 58% (32%) above 10 MeV (20 MeV) Neutron star forming: <30% (<15%) above 10 MeV (20 MeV) total total z=0 1

48 Larger energy window NS only: NS+BH: Red dashed: Homestake Solid, grey: Kamioka

49 Fun stuff

50 Did SN neutrinos kill the dinosaurs? if you stand really close (few pc) ν produce Atom recoil DNA damage 7/6/10 50

51 SN neutrinos the origin of homochirality? Chirality of aminoacids due to chiral symmetry breaking of weak interacron D.B. Cline, Eur. Review 13, 2005

52 Do neutrinos get to your head? Signal in brain/eyes? hbp://