Looking Beyond the Standard Model with Energetic Cosmic Particles
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1 Looking Beyond the Standard Model with Energetic Cosmic Particles Andreas Ringwald ringwald DESY Seminar Universität Dortmund June 13, 2006, Dortmund, Germany
2 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 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]
3 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 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]
4 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 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? [
5 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 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]
6 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
7 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]
8 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 [
9 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]
10 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]
11 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 > 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, ;...;Ahlers et al. 05] 24 h GC h o o C 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
12 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 > 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, ;...;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 ) 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 E lab (ev) [Heck 05]
13 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 > 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, ;...;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
14 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 > 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, ;...;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
15 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
16 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.]
17 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) 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 (Fermi) (Ultra-relativistic shocks-grb) [Pierre Auger Observatory]
18 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
19 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]
20 Looking Beyond the Standard Model 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]
21 Looking Beyond the Standard Model 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]
22 Looking Beyond the Standard Model 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]
23 Looking Beyond the Standard Model 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]
24 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]
25 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]
26 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
27 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]
28 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
29 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
30 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]
31 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]
32 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]
33 Looking Beyond the Standard Model 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 GeV: Cosmology: relics of GUT phase transitions; absorption on big bang relic neutrinos [AR,L.Schrempp 06]
34 Looking Beyond the Standard Model 33 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with GeV < m X < 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]
35 Looking Beyond the Standard Model 34 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with GeV < m X < GeV, produced during and after inflation through e.g. t= t= 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= t=330 [Tkachev,Khlebnikov,Kofman,Linde 98]
36 Looking Beyond the Standard Model 35 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with GeV < m X < 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]
37 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 GeV < m X < 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 log (E=eV) [Berezinsky,Kachelriess,Vilenkin 97]
38 Looking Beyond the Standard Model 37 Top-down scenarios for super-gzk neutrinos Existence of superheavy particles with GeV < m X < 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]
39 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 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) x p = p/p beam [Particle Data Group 04]
40 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 this work Barbot-Drees Sarkar-Toldra 1e-05 1e Ü Å ½ ½¼ ½ [Aloisio,Berezinsky,Kachelriess 04] Î
41 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]
42  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
43 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
44 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]
45 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]
46 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]
47 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.]
48 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.]
49 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]
50 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]
51 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)
52 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.]
53 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.]
54 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]
55 Looking Beyond the Standard Model 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
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