Charged Cosmic Rays and Neutrinos

Transcription

1 Charged Cosmic Rays and Neutrinos Michael Kachelrieß NTNU, Trondheim []

2 Introduction Outline of the talk 1 Introduction talk by F. Halzen 2 SNRs as Galactic CR sources 3 Extragalactic CRs transition anisotropies composition measurements 4 Astrophysical source models talks of S. Ando & F. Halzen 5 Cosmogenic neutrinos 6 Summary Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

3 Introduction Outline of the talk 1 Introduction talk by F. Halzen 2 SNRs as Galactic CR sources 3 Extragalactic CRs transition anisotropies composition measurements 4 Astrophysical source models talks of S. Ando & F. Halzen 5 Cosmogenic neutrinos 6 Summary Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

4 Introduction Outline of the talk 1 Introduction talk by F. Halzen 2 SNRs as Galactic CR sources 3 Extragalactic CRs transition anisotropies composition measurements 4 Astrophysical source models talks of S. Ando & F. Halzen 5 Cosmogenic neutrinos 6 Summary Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

5 Introduction The CR γ ν connection: HE neutrinos and HE photons are unavoidable byproducts of HECRs astrophysical models, direct flux: strongly model dependent fluxes Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

6 Introduction The CR γ ν connection: HE neutrinos and HE photons are unavoidable byproducts of HECRs astrophysical models, direct flux: strongly model dependent fluxes astrophysical models, cosmogenic flux: ratio Iν /I N determined by nuclear composition and source evolution Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

7 Introduction The CR γ ν connection: HE neutrinos and HE photons are unavoidable byproducts of HECRs astrophysical models, direct flux: strongly model dependent fluxes astrophysical models, cosmogenic flux: ratio Iν /I N determined by nuclear composition and source evolution top-down models: large fluxes with Iν I p ratio Iν /I p fixed by fragmentation Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

8 Introduction The CR γ ν connection: HE neutrinos and HE photons are unavoidable byproducts of HECRs astrophysical models, direct flux: strongly model dependent fluxes astrophysical models, cosmogenic flux: ratio Iν /I N determined by nuclear composition and source evolution top-down models: large fluxes with Iν I p ratio Iν /I p fixed by fragmentation prizes to win: astronomy above 0 TeV identification of CR sources determine galactic extragalactic transition of CRs test/discover new particle physics Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

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10 Diffusive shock acceleration in test particle picture: energy spectrum dn/de 1/E 2 escape flux dn/dr exp( (r R sh )/x 0 ) for r > R sh []

11 SNRs as CR sources SNR: Leptonic versus hadronic models [ Giordano ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

12 SNRs as CR sources SNR: Leptonic versus hadronic models [ Giordano ] combining Fermi and IACT contrains models tightly Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

13 SNRs as CR sources Maximal energy of SNR: Lagage-Cesarsky limit acceleration rate β acc = de dt = 3Ev2 sh acc ζd(e), ζ 8 20 Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

14 SNRs as CR sources Maximal energy of SNR: Lagage-Cesarsky limit acceleration rate β acc = de dt = 3Ev2 sh acc ζd(e), ζ 8 20 assume Bohm diffusion D(E) = cr L /3 E and B µg Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

15 SNRs as CR sources Maximal energy of SNR: Lagage-Cesarsky limit acceleration rate β acc = de dt = 3Ev2 sh acc ζd(e), ζ 8 20 assume Bohm diffusion D(E) = cr L /3 E and B µg E max ev Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

16 SNRs as CR sources Maximal energy of SNR: [Bell, Luzcek 02, Bell 04 ] (resonant) coupling CR Alfven waves Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

17 SNRs as CR sources Maximal energy of SNR: [Bell, Luzcek 02, Bell 04 ] (resonant) coupling CR Alfven waves non-linear non-resonant magnetic field amplification Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

18 SNRs as CR sources Maximal energy of SNR: [Bell, Luzcek 02, Bell 04 ] (resonant) coupling CR Alfven waves non-linear non-resonant magnetic field amplification observational evidence for B mg in young SNR rims Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

19 SNRs as CR sources SNR RX J changes on δt 1 yr imply B 1mG E max 16 ev for protons Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

20 SNRs as CR sources Tycho observations by VERITAS Γ = 1.95 ± 0.51 stat ± 0.30 sys Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

21 SNRs as CR sources Tycho observations by VERITAS Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

22 SNRs as CR sources Tycho observations by VERITAS CRs escape before Sedov phase Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW 2012 / 25

23 SNRs as CR sources Tycho observations by VERITAS CRs escape before Sedov phase E γ,max > TeV requires: protons with E > 0 TeV Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW 2012 / 25

24 SNRs as CR sources Tycho observations by VERITAS CRs escape before Sedov phase E γ,max > TeV requires: protons with E > 0 TeV electrons, ICS on CMB E γ = 4 ε γ Ee 2 3 m 2 e 3 GeV ( ) 2 Ee 1TeV Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW 2012 / 25

25 SNRs as CR sources Tycho observations by VERITAS CRs escape before Sedov phase E γ,max > TeV requires: protons with E > 0 TeV electrons, ICS on CMB E γ = 4 ε γ Ee 2 3 m 2 e electrons with E > 50 TeV 3 GeV ( ) 2 Ee 1TeV Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW 2012 / 25

26 SNRs as CR sources Tycho: Leptonic versus hadronic models [Morlino, Capriolo 11 ] Log Ν FΝ Jy Hz Radio Suzaku FermiLAT VERITAS Log Ν Hz Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

27 SNRs as CR sources Why is there a universal CR spectrum? age-limited CRs are advected down-stream, released at end of Sedov phase adiabatic losses, reduced E max, no B amplification Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

28 SNRs as CR sources Why is there a universal CR spectrum? age-limited CRs escape up-stream: standard approach: homogeneous field & free escape boundary Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

29 SNRs as CR sources Why is there a universal CR spectrum? age-limited CRs escape up-stream: standard approach: homogeneous field & free escape boundary filamentation instability: [Reville, Bell 11 ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

30 SNRs as CR sources Why is there a universal CR spectrum? age-limited CRs escape up-stream: standard approach: homogeneous field & free escape boundary filamentation instability: [Reville, Bell 11 ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

31 Transition from Galactic to extragalactic CRs Nuclear composition Transition KASCADE Grande data s -1 sr -1 ev -2 E [m ] di/de Grande QGSJETII, all-particle (this work) Grande QGSJETII, hydrogen (this work) Grande QGSJETII, He+C+Si (this work) Grande QGSJETII, iron (this work) KASCADE QGSJETII, all-particle (this work) KASCADE QGSJETII, hydrogen (this work) KASCADE QGSJETII, He+C+Si (this work) KASCADE QGSJETII, iron (this work) EAS-TOP, all-particle Akeno, all-particle HiRes II, all-particle GAMMA, all-particle Tibet, all-particle 19 energy (ev/particle) 20 Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

32 Transition from Galactic to extragalactic CRs Nuclear composition Transition KASCADE Grande data s -1 sr -1 ev -2 E [m ] di/de Grande QGSJETII, all-particle (this work) Grande QGSJETII, hydrogen (this work) Grande QGSJETII, He+C+Si (this work) Grande QGSJETII, iron (this work) KASCADE QGSJETII, all-particle (this work) KASCADE QGSJETII, hydrogen (this work) KASCADE QGSJETII, He+C+Si (this work) KASCADE QGSJETII, iron (this work) rising proton fraction E > 17 ev? 18 EAS-TOP, all-particle Akeno, all-particle HiRes II, all-particle GAMMA, all-particle Tibet, all-particle 19 energy (ev/particle) 20 Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

33 Transition from Galactic to extragalactic CRs Anisotropies PAO result on dipole anisotropy: Amplitude Rayleigh Analysis East/West Analysis E [EeV] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

34 Transition from Galactic to extragalactic CRs Anisotropies PAO result on dipole anisotropy: Phase [ ] East/West analysis Rayleigh analysis E [EeV] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

35 Transition from Galactic to extragalactic CRs Anisotropies Anisotropy of protons at E = 18 ev [Giacinti et al. 11 ] Dipole amplitude (percent) Profile 2, 200 pc Profile 1, 200 pc Profile 2, 500 pc Profile 1, 500 pc B 0 (µg) protons excluded for all reasonable parameters measuring protons at E = 18 ev means fixing transition energy Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

36 Nuclear composition Energy spectrum PAO confirmed the GZK-suppression seen first by HiRes Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

37 Nuclear composition Energy spectrum PAO confirmed the GZK-suppression seen first by HiRes interpretation: Emax of sources? does not fix composition: proton GZK, Fe photo disintegration Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

38 Nuclear composition Determining nuclear composition: X max and RMS(X max ) Bethe-Heitler model: N max E 0 and X max ln(e 0 ) Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

39 Nuclear composition Determining nuclear composition: X max and RMS(X max ) Bethe-Heitler model: N max E 0 and X max ln(e 0 ) superposition model: nuclei = A shower with E = E 0 /A X max ln(a) and RMS(X max ) reduced Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

40 Nuclear composition Determining nuclear composition: X max and RMS(X max ) Bethe-Heitler model: N max E 0 and X max ln(e 0 ) superposition model: nuclei = A shower with E = E 0 /A X max ln(a) and RMS(X max ) reduced Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

41 Nuclear composition Determining nuclear composition: X max and RMS(X max ) Bethe-Heitler model: N max E 0 and X max ln(e 0 ) superposition model: nuclei = A shower with E = E 0 /A X max ln(a) and RMS(X max ) reduced Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

42 Nuclear composition Determining nuclear composition: X max and RMS(X max ) Bethe-Heitler model: N max E 0 and X max ln(e 0 ) superposition model: nuclei = A shower with E = E 0 /A X max ln(a) and RMS(X max ) reduced RMS(X max ) has smaller theoretical error than X max Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

43 Nuclear composition Nuclear composition via X max : ] 2 <X max > [g/cm QGSJET01 QGSJETII Sibyll2.1 EPOSv1.99 proton iron Auger 2009 HiRes ApJ 2005 Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

44 Nuclear composition Nuclear composition via RMS(X max ) from Auger: ] 2 ) [g/cm max proton 19 E [ev] RMS(X iron 19 E [ev] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

45 Nuclear composition Mixed composition: 0.12 Mean RMS % proton 30% iron sum X max [g/cm ] σ 2 = f i σi 2 + f i f j (X max,i X max,j ) 2 i i<j Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

46 Nuclear composition What goes wrong? internal discrepancy in PAO: AGN correlations favor protons RMS(Xmax ) favors heavy energy spectrum, Xmax and RMS(X max ) difficult to fit experimental discrepancy: HiRes/TA Auger Xmax RMS(Xmax ) discrepancy experiment theory: energy ground array/fluoresence 1.2 muon number exp/mc Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

47 Nuclear composition What goes wrong? internal discrepancy in PAO: AGN correlations favor protons RMS(Xmax ) favors heavy energy spectrum, Xmax and RMS(X max ) difficult to fit experimental discrepancy: HiRes/TA Auger Xmax RMS(Xmax ) discrepancy experiment theory: energy ground array/fluoresence 1.2 muon number exp/mc Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

48 Nuclear composition What goes wrong? internal discrepancy in PAO: AGN correlations favor protons RMS(Xmax ) favors heavy energy spectrum, Xmax and RMS(X max ) difficult to fit experimental discrepancy: HiRes/TA Auger Xmax RMS(Xmax ) discrepancy experiment theory: energy ground array/fluoresence 1.2 muon number exp/mc Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

49 Nuclear composition Comparison of MCs to LHC data: Energy flow PYTHIA as typical HEP model Cosmic ray interaction models Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

50 Cosmogenic neutrinos Limit from EGRB Fermi-LAT limit for cosmogenic neutrinos: [Berezinsky et al.,... ] E 2 J(E), ev cm -2 s -1 sr -1 4 z max =2, E max = 21 ev Fermi LAT 2 0 p HiRes E, ev Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

51 Cosmogenic neutrinos Limit from EGRB Fermi-LAT limit for cosmogenic neutrinos: [Berezinsky et al.,... ] -1 m -2 sec -1 ster 2 J(E) ev 3 E HiRes II 21 z max =2; E max = ev; m=0 HiRes I p Σν i E, ev Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

52 Cosmogenic neutrinos Limit from EGRB Fermi-LAT limit for cosmogenic neutrinos: [Berezinsky et al.,... ] -4 E max = 21 ev 6 5 (m), ev/cm3 cas x m =2.0 g =2.6 g Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

53 Cosmogenic neutrinos Limit from EGRB Fermi-LAT limit for cosmogenic neutrinos: [Berezinsky et al.,... ] E 2 J(E), evcm -2 s -1 sr Auger diff. RICE BAIKAL ANITA-lite Auger E -2 cascade JEM-EUSO IceCube 5yr 20 m=3 21 ANITA e = tilted E, ev nadir 22 Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

54 Cosmogenic neutrinos Limit from EGRB Fermi-LAT limit for cosmogenic neutrinos: [Berezinsky et al.,... ] 0.01 ng E 2 J (E), ev cm -2 s -1 sr ng m=0, g =2.0, z max =2, E max = 21 ev E, ev Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

55 Cosmogenic neutrinos Dependence on composition Cosmogenic neutrinos: proton vs. Fe [Anchordoqui et al. 07 ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

56 Summary Summary Galactic CRs: Tycho: room left for leptonic models marginal UHECRs: understanding differences PAO vs. TA and MC vs. experiment extensions (HEAT, Amiga, infill array) allow cross checks test of MC models against LHC data proton dominance at 18 ev fixes transition energy cosmogenic neutrino flux is low, because of Fermi limit 2 Icecube events: start of neutrino astronomy? Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

57 New TA data for X max : Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

58 Zenith angle dependence, TA scintillator: Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

59 Zenith angle dependence, TA scintillator: Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

60 Icecube events Icecube events 2 cascade events close to E min = 15 ev, bg = 0.14 energy distributions of neutrinos reaching to the IceCube Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

61 Icecube events Icecube events 2 cascade events close to E min = 15 ev, bg = 0.14 Glashow resonance very narrow if W qq, detected energy too low Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

62 Icecube events Icecube events 2 cascade events close to E min = 15 ev, bg = 0.14 Glashow resonance cosmogenic neutrinos: < 1 events/yr [Anchordoqui et al. 07 ] Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

63 Icecube events Icecube events 2 cascade events close to E min = 15 ev, bg = 0.14 Glashow resonance cosmogenic neutrinos: < 1 events/yr extragalactic sources: extension to higher energies? if yes, then diffuse flux Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25

64 Icecube events Icecube events 2 cascade events close to E min = 15 ev, bg = 0.14 Glashow resonance cosmogenic neutrinos: < 1 events/yr extragalactic sources: extension to higher energies? if yes, then diffuse flux Galactic point sources: SNR with d 50 pc Michael Kachelrieß (NTNU Trondheim) Cosmic Rays and Neutrinos NOW / 25