Photohadronic processes and neutrinos Summer school “High energy astrophysics” August 22-26, 2011 Weesenstein, Germany Walter Winter Universität Würzburg Contents Lecture 1 (non-technical) Introduction, motivation Particle production (qualitatively) Neutrino propagation and detection Comments on expected event rates Lecture 2 Tools (more specific) Photohadronic interactions, decays of secondaries, pp interactions A toy model: Magnetic field and flavor effects in n fluxes Glashow resonance? (pp versus pg) Neutrinos and the multi-messenger connection 2 Lecture 1 Introduction Neutrino production in astrophysical sources max. center-of-mass energy ~ 103 TeV (for 1012 GeV protons) Example: Active galaxy (Halzen, Venice 2009) 4 Different messengers Shock accelerated protons lead to p, g, n fluxes p: Cosmic rays: affected by magnetic fields g: Photons: easily absorbed/scattered n: Neutrinos: direct path (Teresa Montaruli, NOW 2008) 5 Evidence for proton acceleration, hints for neutrino production Observation of cosmic rays: need to accelerate protons/hadrons somewhere The same sources should produce neutrinos: in the source (pp, pg interactions) Proton (E > 6 1010 GeV) on CMB GZK cutoff + cosmogenic neutrino flux galactic extragalactic UHECR In the source: Ep,max up to 1012 GeV? GZK cutoff? (Source: F. Halzen, Venice 2009) 6 Example: Gamma-ray bursts Direct+cosmogenic fluxes come typically together: Neutrons from same interactions escape the sources cosmogenic neutrino flux Neutrino flux produced within source (Ahlers, Gonzales-Garcia, Halzen, 2011) 7 Neutrino detection: IceCube Example: IceCube at South Pole Detector material: ~ 1 km3 antarctic ice Completed 2010/11 (86 strings) Recent data releases, based on parts of the detector: Point sources IC-40 [IC-22] arXiv:1012.2137, arXiv:1104.0075 GRB stacking analysis IC-40 arXiv:1101.1448 Cascade detection IC-22 arXiv:1101.1692 Have not seen anything (yet) What does that mean? Are the models wrong? Which parts of the parameter space does IceCube actually test? http://icecube.wisc.edu/ 8 Neutrino astronomy in the Mediterranean: Examples: ANTARES, KM3NeT http://antares.in2p3.fr/ 9 When do we expect a n signal? [some personal comments] Unclear if specific sources lead to neutrino production and at what level; spectral energy distribution can be often described by other radiation processes processes as well (e.g. inverse Compton scattering, proton synchrotron, …) However: whereever cosmic rays are produced, neutrinos should be produced to some degree There are a number of additional candidates, e.g. „Hidden“ sources (e.g. „slow jet supernovae“ without gamma-ray counterpart) (Razzaque, Meszaros, Waxman, 2004; Ando, Beacom, 2005; Razzaque, Meszaros, 2005; Razzaque, Smirnov, 2009) What about Fermi-LAT unidentified/unassociated sources? From the neutrino point of view: „Fishing in the dark blue sea“? Looking at the wrong places? Need for tailor-made neutrino-specific approaches? [unbiased by gamma-ray and cosmic ray observations] Also: huge astrophysical uncertainties; try to describe at least the particle physics as accurate as possible! 10 The parameter space? Model-independent (necessary) condition: Emax ~ Z e B R „Test points“ (?) (Larmor-Radius < size of source) Particles confined to within accelerator! Sometimes: define acceleration rate t-1acc = h Z e B/E (h: acceleration efficiency) Caveat: condition relaxed if source heavily Lorentzboosted (e.g. GRBs) Protons to 1020 eV (Hillas, 1984; version adopted from M. Boratav)11 Simulation of sources (qualitatively) Photohadronics (primitive picture) If neutrons can escape: Source of cosmic rays Neutrinos produced in ratio (ne:nm:nt)=(1:2:0) Cosmogenic neutrinos Delta resonance approximation: p+/p0 determines ratio between neutrinos and gamma-rays High energetic gamma-rays; might cascade down to lower E Cosmic messengers 13 Photohadronics (more realistic) D res. Multi-pion production Resonant production, direct production (Photon energy in nucleon rest frame) (Mücke, Rachen, Engel, Protheroe, Stanev, 2008; SOPHIA) Different characteristics (energy loss of protons; energy dep. cross sec.) 14 Meson photoproduction Starting point: D(1232)resonance approximation Limitations: No p- production; cannot predict p+/ p- ratio (affects neutrino/antineutrino) High energy processes affect spectral shape (X-sec. dependence!) Low energy processes (t-channel) enhance charged pion production Charged pion production underestimated compared to p0 production by factor of 2.4 (independent of input spectra!) Solutions: SOPHIA: most accurate description of physics Mücke, Rachen, Engel, Protheroe, Stanev, 2000 Limitations: Often slow, difficult to handle; helicity dep. muon decays! from: Parameterizations based on SOPHIA Hümmer, Rüger, Kelner, Aharonian, 2008 Spanier, Winter, Fast, but no intermediate muons, pions (cooling cannot be included) ApJ 721 (2010) 630 Hümmer, Rüger, Spanier, Winter, 2010 Fast (~3000 x SOPHIA), including secondaries and accurate p+/ p- ratios; T=10 eV also individual contributions of different processes (allows for comparison More tomorrow with D-resonance!) Engine of the NeuCosmA („Neutrinos from Cosmic Accelerators“) software 15 Typical source models Protons typically injected with power law (Fermi shock acceleration!) ? Target photon field typically: Put in by hand (e.g. obs. spectrum: GRBs) Thermal target photon field From synchrotron radiation of coaccelerated electrons/positrons (AGN-like) From a more complicated combination of radiation processes (see other lectures) Minimal set of assumptions for n production? tomorrow! 16 Secondary decays and magnetic field effects Described by kinematics of weak decays (see e.g. Lipari, Lusignoli, Meloni, 2007) Complication: Magnetic field effects Pions and muons loose energy through synchroton radiation for higher E before they decay – aka „muon damping“ Affect spectral shape and flavor composition of neutrinos significantly peculiarity for neutrinos (p0 are electrically neutral!) … more tomorrow … Dashed: no losses Solid: with losses (example from Reynoso, Romero, 2008) 17 Flavor composition at the source (Idealized – energy independent) Astrophysical neutrino sources produce certain flavor ratios of neutrinos (ne:nm:nt): Pion beam source (1:2:0) Standard in generic models Muon damped source (0:1:0) at high E: Muons lose energy before they decay Muon beam source (1:1:0) Cooled muons pile up at lower energies (also: heavy flavor decays) Neutron beam source (1:0:0) Neutron decays from pg (also possible: photo-dissociation of heavy nuclei) At the source: Use ratio ne/nm (nus+antinus added) 18 Neutrino propagation and detection Neutrino propagation (vacuum) Key assumption: Incoherent propagation of neutrinos (see Pakvasa review, arXiv:0803.1701, and references therein) Flavor mixing: Example: For q13 =0, q23=p/4: NB: No CPV in flavor mixing only! But: In principle, sensitive to Re exp(-i d) ~ cosd 20 Earth attenuation High energy neutrinos interact in the Earth: (C. Quigg) Earth Detector However: Tau neutrino regeneration through nt t (17%) m + nm + nt 21 Neutrino detection (theory) Muon tracks from nm Effective area dominated! (interactions do not have do be within detector) Electromagnetic showers (cascades) from ne Effective volume dominated! nt: Effective volume dominated Low energies (< few PeV) typically hadronic shower (nt track not separable) Higher Energies: nt track separable Double-bang events Lollipop events Glashow resonace for electron antineutrinos at 6.3 PeV NC showers t nt nt e ne m nm (Learned, Pakvasa, 1995; Beacom et al, hep-ph/0307025; many others) 22 Neutrino detection: Muon tracks Number of events depends on neutrino effective area and observ. time texp: [cm-2 s-1 GeV-1] Neutrino effective area ~ detector area x muon range (E); but: cuts, uncontained events, … Time-integrated point source search, IC-40 nt: via tm (arXiv:1012.2137) Earth opaque to nm 23 Computation of limits (1) Number of events N can be translated into limit by Feldman-Cousins approach (Feldman, Cousins, 1998) This integral limit is a single number given for particular flux, e.g. E-2, integrated over a certain energy range 24 Computation of limits (2) Alternative: Quantify contribution of integrand in when integrating over log E: Differential limit: 2.3 E/(Aeff texp) Is a function of energy, applies to arbitrary fluxes if limit and fluxes sufficiently smooth over ~ one decade in E 25 Comparison of limits (example) (arXiv:1103.4266) Differential limit Fluxes typically below that IC-40 nm Integral limit Applies to E-2 flux only NB: Spectral shape important because of instrument response! Energy range somewhat arbitrary (e.g. 90% of all events) 26 Neutrino detection: backgrounds Backgrounds domination: Earth Atmospheric neutrino dominated Detector Cosmic muon dominated Background suppression techniques: Angular resolution (point sources) Timing information from gamma-ray counterpart (transients, variable sources) Cuts of low energy part of spectrum (high energy diffuse fluxes) 27 Measuring flavor? (experimental) In principle, flavor information can be obtained from different event topologies: Muon tracks - nm Cascades (showers) – CC: ne, nt, NC: all flavors Glashow resonance (6.3 PeV): ne Double bang/lollipop: nt (sep. tau track) t (Learned, Pakvasa, 1995; Beacom et al, 2003) nt In practice, the first (?) IceCube „flavor“ analysis appeared recently – IC-22 cascades (arXiv:1101.1692) Flavor contributions to cascades for E-2 extragalatic test flux (after cuts): Electron neutrinos 40% Tau neutrinos 45% Muon neutrinos 15% Electron and tau neutrinos detected with comparable efficiencies Neutral current showers are a moderate background 28 Flavor ratios at detector At the detector: define observables which take into account the unknown flux normalization take into account the detector properties Example: Muon tracks to showers Do not need to differentiate between electromagnetic and hadronic showers! Flavor ratios have recently been discussed for many particle physics applications (for flavor mixing and decay: Beacom et al 2002+2003; Farzan and Smirnov, 2002; Kachelriess, Serpico, 2005; Bhattacharjee, Gupta, 2005; Serpico, 2006; Winter, 2006; Majumar and Ghosal, 2006; Rodejohann, 2006; Xing, 2006; Meloni, Ohlsson, 2006; Blum, Nir, Waxman, 2007; Majumar, 2007; Awasthi, Choubey, 2007; Hwang, Siyeon,2007; Lipari, Lusignoli, Meloni, 2007; Pakvasa, Rodejohann, Weiler, 2007; Quigg, 2008; Maltoni, Winter, 2008; Donini, Yasuda, 2008; Choubey, Niro, Rodejohann, 2008; Xing, Zhou, 2008; Choubey, Rodejohann, 2009; Esmaili, Farzan, 2009; Bustamante, Gago, Pena-Garay, 2010; Mehta, Winter, 2011…) 29 New physics in R? Energy dependence flavor comp. source Energy dep. new physics (Example: [invisible] neutrino decay) 1 Stable state 1 Unstable state Mehta, Winter, JCAP 03 (2011) 041; see also Bhattacharya, Choubey, Gandhi, Watanabe, 2009/2010 30 How many neutrinos do we expect to see? Upper bound from cosmic rays Injection of CR protons inferred from observations: (caveats: energy losses, distribution of sources, …) Can be used to derive upper bound for neutrinos (Waxman, Bahcall, 1998 + later; Mannheim, Protheroe, Rachen, 1998) Typical assumptions: Protons lose fraction fp<1 into pion production within source About 50% charged and 50% neutral pions produced Pions take 20% of proton energy Leptons take about ¼ of pion energy Muon neutrinos take 0.05 Ep fp = 1 fp ~ 0.2 Warning: bound depends on flavors considered, and whether flavor mixing is taken into account! 32 Comments on statistics At the Waxman-Bahcall bound: O(10) events in full-scale IceCube per year Since (realistically) fp << 1, probably Nature closer to O(1) event Do not expect significant statistics from single (cosmic ray) source! Need dedicated aggregation methods: Diffuse flux measurement Stacking analysis, uses gamma-ray counterpart (tomorrow) However: WB bound applies only to accelerators of UHECR! Only protons! 33 Diffuse flux (e.g. AGNs) (Becker, arXiv:0710.1557) Comoving volume Single source spectrum Source distribution in redshift, luminosity Decrease with luminosity distance Advantage: optimal statistics (signal) Disadvantage: Backgrounds (e.g. atmospheric) 34 Consequences of low statistics [biased] Neutrinos may tell the nature (class) of the cosmic ray sources, but not where exactly they come from Consequence: It‘s a pity, since UHECR experiments will probably also not tell us from which sources they come from … Comparison to g-rays: Neutrino results will likely be based on accumulated statistics. Therefore: use input from g-ray observations (tomorrow …) Clues for hadronic versus leptonic models? Again: probably on a statistical basis … Consequences for source simulation? Time-dependent effects will not be observable in neutrinos Spectral effects are, however, important because of detector response 35 Summary (lecture 1) Neutrino observations important for Nature of cosmic ray sources Hadronic versus leptonic models Neutrino observations are qualitatively different from CR and g-ray observations: Low statistics, conclusions often based on aggregated fluxes Charged secondaries lead to neutrino production: flavor and magnetic field effects 36