Looking Beyond the Standard Model with Energetic Cosmic Particles Andreas Ringwald http://www.desy.de/ ringwald DESY Seminar Universität Dortmund June 13, 2006, Dortmund, Germany
1. Introduction Looking Beyond the Standard Model 1 There is a high energy universe: Gamma rays have been identified up to energies E < few 10 3 GeV Cosmic rays have been observed up to energies E < few 10 11 GeV It is under active observation: Gamma ray observatories: e.g. H.E.S.S., MAGIC Air shower detectors: e.g. Pierre Auger Observatory Neutrino telescopes: e.g. IceCube Attack fundamental questions: What is it made of? What are the cosmic accelerators? Can we exploit them also for particle physics? [M. Martinez 05]
1. Introduction Looking Beyond the Standard Model 2 There is a high energy universe: Gamma rays have been identified up to energies E < few 10 3 GeV Cosmic rays have been observed up to energies E < few 10 11 GeV It is under active observation: Gamma ray observatories: e.g. H.E.S.S., MAGIC Air shower detectors: e.g. Pierre Auger Observatory Neutrino telescopes: e.g. IceCube Attack fundamental questions: What is it made of? What are the cosmic accelerators? Can we exploit them also for particle physics? [T. K. Gaisser 05]
1. Introduction Looking Beyond the Standard Model 3 There is a high energy universe: Gamma rays have been identified up to energies E < few 10 3 GeV Cosmic rays have been observed up to energies E < few 10 11 GeV It is under active observation: Gamma ray observatories: e.g. H.E.S.S., MAGIC Air shower detectors: e.g. Pierre Auger Observatory Neutrino telescopes: e.g. IceCube Attack fundamental questions: What is it made of? What are the cosmic accelerators? Can we exploit them also for particle physics? [www.auger.org]
1. Introduction Looking Beyond the Standard Model 4 There is a high energy universe: Gamma rays have been identified up to energies E < few 10 3 GeV Cosmic rays have been observed up to energies E < few 10 11 GeV It is under active observation: Gamma ray observatories: e.g. H.E.S.S., MAGIC Air shower detectors: e.g. Pierre Auger Observatory Neutrino telescopes: e.g. IceCube Attack fundamental questions: What is it made of? What are the cosmic accelerators? Can we exploit them also for particle physics? [icecube.wisc.edu]
Looking Beyond the Standard Model 5 Outline: 2. Ultrahigh energy cosmic rays and neutrinos 3. TeV scale physics with ultrahigh energy neutrinos 4. GUT scale physics with extremely energetic neutrinos 5. Conclusions
Looking Beyond the Standard Model 6 2. Ultrahigh energy cosmic rays and neutrinos CR spectrum: Large statistical and systematic uncertainties low flux energy from shower simulations Crucial improvement by PAO: huge size better statistics hybrid observations better energy calibration through Fly s Eye technique, direction from ground array It works [Ahlers et al. 05]
Looking Beyond the Standard Model 7 2. Ultrahigh energy cosmic rays and neutrinos CR spectrum: Large statistical and systematic uncertainties low flux energy from shower simulations Crucial improvement by PAO: huge size better statistics hybrid observations better energy calibration through Fly s Eye technique, direction from ground array It works [www.auger.org]
Looking Beyond the Standard Model 8 2. Ultrahigh energy cosmic rays and neutrinos CR spectrum: Large statistical and systematic uncertainties low flux energy from shower simulations Crucial improvement by PAO: huge size better statistics hybrid observations better energy calibration through Fly s Eye technique, direction from ground array It works [Ahlers et al. 05]
Looking Beyond the Standard Model 9 2. Ultrahigh energy cosmic rays and neutrinos CR spectrum: Large statistical and systematic uncertainties low flux energy from shower simulations Crucial improvement by PAO: huge size better statistics hybrid observations better energy calibration through Fly s Eye technique, direction from ground array It works [Ahlers et al. 05]
2. Ultrahigh energy cosmic rays and neutrinos Looking Beyond the Standard Model 10 CR angular distribution: isotrop CR composition: Large uncertainty studies rely on simulations Cosmic rays above > 10 8.6 GeV, the second knee, dominantly protons Assume that CR s in 10 [8.6,11] GeV range originate from isotropically distributed extragalactic proton sources, with simple power-law injection spectra E γ i (1 + z) n [Berezinsky,.. 02-05;...;Ahlers et al. 05] 24 h GC h 12 +60 60 o o C +30 30 o o 0 h AGASA Good fit; inelastic interactions with CMB (e + e dip ; π bump ) visible; some post-gzk events? A. Ringwald (DESY) [Greisen;Zatsepin,Kuzmin 67] Seminar, Dortmund, June 2006
2. Ultrahigh energy cosmic rays and neutrinos Looking Beyond the Standard Model 11 CR angular distribution: isotrop CR composition: Large uncertainty studies rely on simulations Cosmic rays above > 10 8.6 GeV, the second knee, dominantly protons Assume that CR s in 10 [8.6,11] GeV range originate from isotropically distributed extragalactic proton sources, with simple power-law injection spectra E γ i (1 + z) n [Berezinsky,.. 02-05;...;Ahlers et al. 05] Good fit; inelastic interactions with CMB (e + e dip ; π bump ) visible; some post-gzk events? A. Ringwald (DESY) [Greisen;Zatsepin,Kuzmin 67] Seminar, Dortmund, June 2006 X max (g/cm 2 ) 1000 900 800 700 600 500 400 Fly s Eye HiRes-MIA HiRes 2004 Yakutsk 2001 Yakutsk 2005 CASA-BLANCA HEGRA-AIROBICC SPASE-VULCAN DICE TUNKA gamma proton iron gamma with preshower DPMJET 2.55 nexus 2 QGSJET 01c QGSJET II SIBYLL 2.1 nexus 3 10 14 10 15 10 16 10 17 10 18 10 19 10 20 10 21 E lab (ev) [Heck 05]
2. Ultrahigh energy cosmic rays and neutrinos Looking Beyond the Standard Model 12 CR angular distribution: isotrop CR composition: Large uncertainty studies rely on simulations Cosmic rays above > 10 8.6 GeV, the second knee, dominantly protons Assume that CR s in 10 [8.6,11] GeV range originate from isotropically distributed extragalactic proton sources, with simple power-law injection spectra E γ i (1 + z) n [Berezinsky,.. 02-05;...;Ahlers et al. 05] Good fit; inelastic interactions with CMB (e + e dip ; π bump ) visible; some post-gzk events? [Ahlers et al. 05] A. Ringwald (DESY) [Greisen;Zatsepin,Kuzmin 67] Seminar, Dortmund, June 2006
2. Ultrahigh energy cosmic rays and neutrinos Looking Beyond the Standard Model 13 CR angular distribution: isotrop CR composition: Large uncertainty studies rely on simulations Cosmic rays above > 10 8.6 GeV, the second knee, dominantly protons Assume that CR s in 10 [8.6,11] GeV range originate from isotropically distributed extragalactic proton sources, with simple power-law injection spectra E γ i (1 + z) n [Berezinsky,.. 02-05;...;Ahlers et al. 05] Good fit; inelastic interactions with CMB (e + e dip ; π bump ) visible; some post-gzk events? [Ahlers et al. 05] A. Ringwald (DESY) [Greisen;Zatsepin,Kuzmin 67] Seminar, Dortmund, June 2006
Looking Beyond the Standard Model 14 Possible sources of these protons: GRB, AGN,... Shock acceleration: p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Neutrinos as diagnostic tool: ν s from sources (pγ n + π s) close to be measured Cosmogenic neutrino flux (from pγ CMB Nπ s) dominates above 10 9 GeV
Looking Beyond the Standard Model 15 Possible sources of these protons: GRB, AGN,... Shock acceleration: e e + µ + ν e ν µ ν µ p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) ν e ν µ ν µ µ π p n p π + SHOCK Neutrinos as diagnostic tool: ν s from sources (pγ n + π s) close to be measured Cosmogenic neutrino flux (from pγ CMB Nπ s) dominates above 10 9 GeV [Ahlers PhD in prep.]
Looking Beyond the Standard Model 16 Possible sources of these protons: GRB, AGN,... Shock acceleration: p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Neutrinos as diagnostic tool: ν s from sources (pγ n + π s) close to be measured Cosmogenic neutrino flux (from pγ CMB Nπ s) dominates above 10 9 GeV log(magnetic field, gauss) -9 15 9 3-3 Hillas-plot (candidate sites for E=100 EeV and E=1 ZeV) Neutron star GRB White dwarf Fe (100 EeV) Protons (100 EeV) E max~ ZBL E ~ ZBL Γ max Protons (1 ZeV) Colliding galaxies nuclei SNR jets Galactic disk halo Active galaxies hot-spots lobes 1 au 1 pc 1 kpc 1 Mpc log(size, km) Clusters 3 6 9 12 15 18 21 (Fermi) (Ultra-relativistic shocks-grb) [Pierre Auger Observatory]
Looking Beyond the Standard Model 17 Possible sources of these protons: GRB, AGN,... Shock acceleration: p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Neutrinos as diagnostic tool: ν s from sources (pγ n + π s) close to be measured Cosmogenic neutrino flux (from pγ CMB Nπ s) dominates above 10 9 GeV [Ahlers PhD in prep.] n e + µ + ν µ p π + ν e ν µ SHOCK
Looking Beyond the Standard Model 18 Possible sources of these protons: GRB, AGN,... Shock acceleration: p s, confined by magnetic fields, accelerate through repeated scattering by plasma shock fronts production of π s and n s through collisions of the trapped p s with ambient plasma produces γ s, ν s and CR s (n diffusion from source) Neutrinos as diagnostic tool: ν s from sources (pγ n + π s) close to be measured Cosmogenic neutrino flux (from pγ CMB Nπ s) dominates above 10 9 GeV [Ahlers et al. 05]
Looking Beyond the Standard Model 19 3. TeV scale physics with ultrahigh energy neutrinos Cν s with E ν > 10 8 GeV probe νn scattering at s νn > 14 TeV (LHC) Perturbative Standard Model (SM) under control ( HERA) [Gandhi et al. 98; Glück et al. 98;...] Search for enhancements in σ νn beyond (perturbative) SM: Electroweak sphaleron production (B + L violating processes in SM) Kaluza-Klein, black hole, p-brane or string ball production in TeV scale gravity models... [Ahlers et al. 05]
Looking Beyond the Standard Model 20 3. TeV scale physics with ultrahigh energy neutrinos Cν s with E ν > 10 8 GeV probe νn scattering at s νn > 14 TeV (LHC) Perturbative Standard Model (SM) under control ( HERA) [Gandhi et al. 98; Glück et al. 98;...] Search for enhancements in σ νn beyond (perturbative) SM: Electroweak sphaleron production (B + L violating processes in SM) Kaluza-Klein, black hole, p-brane or string ball production in TeV scale gravity models... [Tu 04]
Looking Beyond the Standard Model 21 3. TeV scale physics with ultrahigh energy neutrinos Cν s with E ν > 10 8 GeV probe νn scattering at s νn > 14 TeV (LHC) Perturbative Standard Model (SM) under control ( HERA) [Gandhi et al. 98; Glück et al. 98;...] Search for enhancements in σ νn beyond (perturbative) SM: Electroweak sphaleron production (B + L violating processes in SM) Kaluza-Klein, black hole, p-brane or string ball production in TeV scale gravity models... [Fodor,Katz,AR,Tu 03; Han,Hooper 03]
Looking Beyond the Standard Model 22 3. TeV scale physics with ultrahigh energy neutrinos Cν s with E ν > 10 8 GeV probe νn scattering at s νn > 14 TeV (LHC) Perturbative Standard Model (SM) under control ( HERA) [Gandhi et al. 98; Glück et al. 98;...] Search for enhancements in σ νn beyond (perturbative) SM: Electroweak sphaleron production (B + L violating processes in SM) Kaluza-Klein, black hole, p-brane or string ball production in TeV scale gravity models... [AR,Tu 01; Tu 04]
Looking Beyond the Standard Model 23 Model-independent upper bounds on σ νn dn dt de ν F ν (E ν )σ νn (E ν ) Non-observation of deeply-penetrating particles, together with lower bound on F ν (e.g. cosmogenic ν s) upper bound on σ νn [Berezinsky,Smirnov 74; Morris,AR 94; Tyler,Olinto,Sigl 01;..] Recent quantitative analysis: [Anchordoqui,Fodor,Katz,AR,Tu 04] Best current limits from exploitation of RICE search results [Kravchenko et al. [RICE] 02,03] Auger will improve these limits by one order of magnitude [Anchordoqui,Fodor,Katz,AR,Tu 04]
Looking Beyond the Standard Model 24 Model-independent upper bounds on σ νn dn dt de ν F ν (E ν )σ νn (E ν ) Non-observation of deeply-penetrating particles, together with lower bound on F ν (e.g. cosmogenic ν s) upper bound on σ νn [Berezinsky,Smirnov 74; Morris,AR 94; Tyler,Olinto,Sigl 01;..] Recent quantitative analysis: [Anchordoqui,Fodor,Katz,AR,Tu 04] Best current limits from exploitation of RICE search results [Kravchenko et al. [RICE] 02,03] Auger will improve these limits by one order of magnitude [Anchordoqui,Fodor,Katz,AR,Tu 04]
Looking Beyond the Standard Model 25 Strongly interacting neutrino scenarios Bounds exploiting searches for deeply-penetrating particles applicable as long as σ νn < (0.5 1) mb For even higher cross sections, e.g. via sphaleron or brane production: Strongly interacting neutrino scenario for the post-gzk events Quantitative analysis: [Berezinsky,Zatsepin 69] [Fodor,Katz,AR,Tu 03; Ahlers,AR,Tu 05] Very good fit to CR data Need steeply rising cross section, otherwise clash with nonobservation of deeply-penetrating particles
Looking Beyond the Standard Model 26 Strongly interacting neutrino scenarios Bounds exploiting searches for deeply-penetrating particles applicable as long as σ νn < (0.5 1) mb For even higher cross sections, e.g. via sphaleron or brane production: Strongly interacting neutrino scenario for the post-gzk events Quantitative analysis: [Berezinsky,Zatsepin 69] [Fodor,Katz,AR,Tu 03; Ahlers,AR,Tu 05] Very good fit to CR data Need steeply rising cross section, otherwise clash with nonobservation of deeply-penetrating particles [Ahlers,AR,Tu 05]
Looking Beyond the Standard Model 27 Strongly interacting neutrino scenarios Bounds exploiting searches for deeply-penetrating particles applicable as long as σ νn < (0.5 1) mb For even higher cross sections, e.g. via sphaleron or brane production: Strongly interacting neutrino scenario for the post-gzk events Quantitative analysis: [Berezinsky,Zatsepin 69] [Fodor,Katz,AR,Tu 03; Ahlers,AR,Tu 05] Very good fit to CR data Need steeply rising cross section, otherwise clash with nonobservation of deeply-penetrating particles [Ahlers,A.R.,Tu 05] [AR 03;Han,Hooper 04] - - - sphalerons [Anchordoqui,Feng,Goldberg 02] p-branes [Burgett,Domokos,Kovesi-Domokos 04]...string excitations
Looking Beyond the Standard Model 28 Strongly interacting neutrino scenarios Bounds exploiting searches for deeply-penetrating particles applicable as long as σ νn < (0.5 1) mb For even higher cross sections, e.g. via sphaleron or brane production: Strongly interacting neutrino scenario for the post-gzk events Quantitative analysis: [Berezinsky,Zatsepin 69] [Fodor,Katz,AR,Tu 03; Ahlers,AR,Tu 05] Very good fit to CR data Need steeply rising cross section, otherwise clash with nonobservation of deeply-penetrating particles [Ahlers,A.R.,Tu 05] [AR 03;Han,Hooper 04] - - - sphalerons [Anchordoqui,Feng,Goldberg 02] p-branes [Burgett,Domokos,Kovesi-Domokos 04]...string excitations
Looking Beyond the Standard Model 29 Long-lived staus at IceCube In most SUSY extensions of SM, lightest superpartner (LSP) stable neutralino dark matter gravitino dark matter Gravitino LSP interacts only gravitationally next-to-lightest SUSY particle (NLSP) long-lived If NLSP charged, e.g. stau τ, it can possibly be collected in collider experiments. Observation of stau decays indirect discovery of the gravitino [Buchmüller et al. 04,...,Feng et al. 04,...]. [Ahlers,Kersten,AR 06]
Looking Beyond the Standard Model 30 Long-lived staus at IceCube Long-lived stau NLSPs resulting from cosmic νn interactions inside Earth can be detected in ice or water Cherenkov neutrino telescopes [Albuquerque,Burdman,Chacko 03; Ahlers,Kersten,AR 06;...] SUSY cross-section smaller than SM Stau has small energy loss in matter effective detection volume for stau much larger than for muon Staus always produced in pairs nearly parallel muon-like tracks in the detector, in contrast to SM, where single muons dominate IceCube: Up to 50 τ pair events/yr [Ahlers,Kersten,AR 06]
Looking Beyond the Standard Model 31 Long-lived staus at IceCube Long-lived stau NLSPs resulting from cosmic νn interactions inside Earth can be detected in ice or water Cherenkov neutrino telescopes [Albuquerque,Burdman,Chacko 03; Ahlers,Kersten,AR 06;...] SUSY cross-section smaller than SM Stau has small energy loss in matter effective detection volume for stau much larger than for muon Staus always produced in pairs nearly parallel muon-like tracks in the detector, in contrast to SM, where single muons dominate IceCube: Up to 50 τ pair events/yr [Ahlers,Kersten,AR 06]
Looking Beyond the Standard Model 32 4. GUT scale physics with extremely energetic neutrinos Existing observatories for Extremely High Energy Cosmic neutrinos provide upper bounds up to GUT scale Upcoming decade: Improved sensitivity by many orders of magnitude E 10 7 GeV: Astrophysics of cosmic rays E 10 8 GeV: Particle physics beyond LHC E 10 12 GeV: Cosmology: relics of GUT phase transitions; absorption on big bang relic neutrinos [AR,L.Schrempp 06]
Looking Beyond the Standard Model 33 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with 10 12 GeV < m X < 10 16 GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field super-gzk ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects, formed during preheating, into their constituents super-gzk ν s from topological defects [Kolb,Chung,Riotto 98]
Looking Beyond the Standard Model 34 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with 10 12 GeV < m X < 10 16 GeV, produced during and after inflation through e.g. t=252 50 t=280 50 particle creation in time-varying gravitational field super-gzk ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects from late phase transitions into their constituents super-gzk ν s from topological defects 0 t=328 50 0 0 0 50 50 0 t=330 [Tkachev,Khlebnikov,Kofman,Linde 98] 50 0 0 0 50 50
Looking Beyond the Standard Model 35 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with 10 12 GeV < m X < 10 16 GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field super-gzk ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects from late phase transitions into their constituents super-gzk ν s from topological defects [Ringeval,Sakellariadou,Bouchet 06]
tot I halo I halo N I extr p I Looking Beyond the Standard Model 36 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with 10 12 GeV < m X < 10 16 GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field super-gzk ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects from late phase transitions into their constituents super-gzk ν s from topological defects log 10 (E 3 I); m?2 s?1 sr?1 ev 2 28 27 26 25 24 23 22 log (E=eV) 10 21 18 19 20 21 22 [Berezinsky,Kachelriess,Vilenkin 97]
Looking Beyond the Standard Model 37 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with 10 12 GeV < m X < 10 16 GeV, produced during and after inflation through e.g. particle creation in time-varying gravitational field super-gzk ν s from decay or annihilation of superheavy dark matter (for τ X > τ U ) decomposition of topological defects from late phase transitions into their constituents super-gzk ν s from constituent decay [Bhattacharjee,Hill,Schramm 92]
Looking Beyond the Standard Model 38 Top-down scenarios for super-gzk neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p 1/σ had dσ/dx 1/σ had dσ/dx 1/σ had dσ/dx 300 100 30 10 3 1 0.3 0.1 0.03 0.01 30 10 3 1 0.3 0.1 0.03 0.01 30 10 3 1 0.3 0.1 0.03 π ± ( s = 91 GeV) π ± ( s = 29 GeV) π ± ( s = 10 GeV) K ± ( s = 91 GeV) K ± ( s = 29 GeV) K ± ( s = 10 GeV) p, _ p ( s = 91 GeV) p, _ p ( s = 29 GeV) p, _ p ( s = 10 GeV) (a) (b) (c) 0.01 0.005 0.01 0.02 0.05 0.1 0.2 0.5 1 x p = p/p beam [Particle Data Group 04]
Ü Ô Õ Ü Å µ Looking Beyond the Standard Model 39 Top-down scenarios for super-gzk neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p 1000 100 10 1 0.1 0.01 0.001 this work 0.0001 Barbot-Drees Sarkar-Toldra 1e-05 1e-05 0.0001 0.001 0.01 0.1 1 Ü Å ½ ½¼ ½ [Aloisio,Berezinsky,Kachelriess 04] Î
Looking Beyond the Standard Model 40 Top-down scenarios for super-gzk neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p [Aloisio,Berezinsky,Kachelriess 04]
 µ Î ¾ Ñ ¾ ½ Ö ½ µ Looking Beyond the Standard Model 41 Top-down scenarios for super-gzk neutrinos Injection spectra: fragmentation functions D i (x,µ), i = p, e,γ,ν, determined via Monte Carlo generators DGLAP evolution from experimental initial distributions at e.g. µ = m Z to µ = m X Reliably predicted! Spectra at Earth: for superheavy dark matter, injection nearby: j ν j γ j p for topological defects, injection far away: j ν j γ j p 1e+27 1e+26 1e+25 1e+24 1e+23 Å ½ ½¼ ½ Ô Î 1e+22 1e+18 1e+19 1e+20 1e+21 1e+22 ε [Aloisio,Berezinsky,Kachelriess 04] Ô
Looking Beyond the Standard Model 42 Top-down scenarios for super-gzk neutrinos How generic? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, including fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings
Looking Beyond the Standard Model 43 Top-down scenarios for super-gzk neutrinos How generic? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, and even fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings x z Imφ Reφ y [Rajantie 03]
Looking Beyond the Standard Model 44 Top-down scenarios for super-gzk neutrinos How generic? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or quasi-stable Topological defects: generic prediction of symmetry breaking (SB) in GUT s, and even fundamental string theory, e.g. G H U(1) SB: monopoles U(1) SB: ordinary or superconducting strings G H U(1) H Z N SB: monopoles connected by strings M M M NECKLACE M M MS NETWORK M [Berezinsky 05]
Looking Beyond the Standard Model 45 Top-down scenarios for super-gzk neutrinos How generic? Superheavy dark matter: need symmetry to prevent fast X decay gauge X stable discrete stable or1 quasi-stable Topological defects: generic prediction 1 of symmetry breaking 1 (SB) 4 in GUT s, C 2 L 2 including R fundamental string theory, e.g. 1 G H U(1) SB: 1 (1,2) monopoles G U(1) SB: ordinary or superconducting strings SM (Z 2 ) G H U(1) H Z N SB: monopoles connected by strings SO(10) 3 C 2 L 2 R 1 B L 4 C 2 L 1 R 1 2 (2) 3 C 2 L 1 R 1 B L G SM (Z 2 ) 2 (2) G SM (Z 2 ) 1 3 C 2 L 1 R 1 B L 2 (2) G SM (Z 2 ) 2 (2) G SM (Z 2 ) 2 (2) 3 C 2 L 1 R 1 B L G SM (Z 2 ) [Jeannerot,Rocher,Sakellariadou 03]
Looking Beyond the Standard Model 46 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Fodor,Katz,AR,Weiler,Wong,in prep.]
Looking Beyond the Standard Model 47 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Fodor,Katz,AR,Weiler,Wong,in prep.]
Looking Beyond the Standard Model 48 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Barbot,Drees 02]
Looking Beyond the Standard Model 49 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background [Tu 04]
Looking Beyond the Standard Model 50 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background (CνB)
Looking Beyond the Standard Model 51 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background (CνB) [Fodor,Katz,AR,Weiler,Wong,in prep.]
Looking Beyond the Standard Model 52 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background (CνB) [Fodor,Katz,AR,Weiler,Wong,in prep.]
Looking Beyond the Standard Model 53 Top-down scenarios for super-gzk neutrinos Strong impact of measurement for particle physics GUT parameters, e.g. m X particle content of the desert, e.g. SM vs. MSSM νn scattering at s LHC cosmology window on early phase transition Hubble expansion rate H(z) existence of the big bang relic neutrino background (CνB) [AR,L. Schrempp 06]
Looking Beyond the Standard Model 54 5. Conclusions Exciting times for ultrahigh energy cosmic rays and neutrinos: many observatories under construction appreciable event samples Expect strong impact on astrophysics particle physics cosmology