DOCSLIB.ORG

Probing New Physics with Atmospheric Neutrinos at Km3net-ORCA Joao

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Probing New Physics with Atmospheric Neutrinos at Km3net-ORCA Joao Probing new physics with atmospheric neutrinos at KM3NeT-ORCA João A. B. Coelho for the KM3NeT Collaboration APC Laboratory [email protected] • 5.7 Mton detector • Atmospheric neutrinos traverse large KM3Net DOM • 115 lines amounts of dense matter inside the earth. 31x3’’ PMTs • 18 DOMs per line • 31 PMTs per DOM • 200 Matter effects can significantly alter the ̴ neutrino oscillation probabilities. • 1 DOM ~ 3 kton equiv. m • 1 line ~ 50 kton equiv. • A Mton size detector with good energy and angle resolution can take advantage of For Comparison: these substantial matter effects to look for • Super-K: 25 kton physics beyond the Standard Model. • NOvA: 10 kton 43 cm • MINOS: 4 kton Sterile Neutrinos Non-Standard Interactions • Almost all neutrino oscillation data can be well • Matter effects arise from coherent CC forward described by a set of 3 neutrino mass eigenstates scattering of neutrinos on electrons in the coupling to the 3 charged leptons according to the earth’s interior, introducing a flavour imbalance. PMNS matrix. • If additional neutrino-electron interactions exist • Some hints of a 4th neutrino mass eigenstate, with beyond the Standard Model, they may modify very weak coupling to the charged leptons have the neutrino effective propagation Hamiltonian. been found, most notably by the LSND [1] and MiniBooNE [2] collaborations. • Strong bounds exist on some NSI couplings, e e e • This new, eV scale, mass eigenstate changes the but limits on ee, et and tt are currently effective oscillation Hamiltonian and generates larger than GF [4]. new resonant transition • Atmospheric neutrinos provide effects due to propagation an excellent probe of these NSI, in matter [3]. since strong matter effects are expected to occur at the scale of [1] Phys. Rev. D 64, 112007 (2001) the Fermi interaction. [2] Phys. Rev. Lett. 110, 161801 (2013) [3] JHEP 0712, 014 (2007) 9 [4] Rept. Prog. Phys. 76, 044201 (2013) m vertical spacing m vertical Standard Osc. Sterile (3+1) Examples: Examples: Non-Std. Int. Standard Osc. • E = 24 GeV • E = 5.3 GeV 2 2 • Dm 41 = 0.3 eV 2 • |Ue4| = 0.04 • eet = 0.2 2 • |Um4| = 0.02 • ett = 0.04 2 • |Ut4| = 0.18 • eee = 0 Scan for animations Scan for animations • In ORCA, the dominant effect of adding a eV scale sterile neutrino • ORCA can probe NSI by searching would be the suppression of n to ̴20 m for changes in the oscillation m pattern due to resonant transitions nt oscillation at ~20 GeV. horizontal in both the n and n channels. spacing m e • This effect arises from an interplay of the CC and NC contributions to • The dominant effects would occur the matter potential. in the same energy range used to study the neutrino mass hierarchy, but a different zenith angle • Resonant nm to nt transitions from 100 GeV to the TeV scale also occur. dependence is expected. • The suppression described above is • strongly dependent on the Ut4 With 1 year of data, ORCA would be sensitive to NSI effects more than an element of the mixing matrix. order of magnitude smaller than their current limits. • With 1 year of data, ORCA would • NSI can give rise to a very rich 2 be sensitive to |Ut4| values 5x phenomenology and the interplay of smaller than current limits set by the different NSI parameters needs Super-Kamiokande [5]. to be studied carefully. [5] Phys. Rev. D 91, 052019 (2015) • Constraints from long-baseline experiments will pin down the CAVEATS vacuum oscillation parameters, which is essential for achieving • Sensitivities in this poster are ORCA’s full potential. based on a simplified analysis and do NOT make use of the full KM3NeT-ORCA MC simulation. • Detector response has been parameterised to approximately match the performance from MC studies performed by the KM3NeT Collaboration [6]. Read the KM3NeT Letter of Intent [6] J. Phys. G: Nucl. Part. Phys. 43, 084001 (2016) .
Load more

Recommended publications
  • Km3net/ORCA Telescopes
    Search for light sterile neutrinos with ANTARES and KM3NeT/ORCA telescopes A. Domi1,2, J. A. B. Coelho3, T. Thakore4, for the ANTARES and KM3NeT Collaborations 1 Università degli Studi di Genova, Genoa (Italy) - [email protected] 2 INFN-Genova, Genoa (Italy) 3 LAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, Orsay (France) - [email protected] 4 University of Cincinnati, Ohio (United States) - [email protected] VLVnT Workshop - 19/05/2021 1 Where are we with light sterile neutrinos? • Majority of experiments have confirmed the 3 flavour neutrino oscillations. • In parallel, anomalies observed in some oscillation experiments: Anomalies in Short baseline (SBL) Ref: Prog.Part.Nucl.Phys. 111 (2020) 103736 experiments •LSND: �� -> �e •MINIBooNE: �� -> �e / �� -> �e Gallium Anomalies: �e disappearance Reactor anomalies: e disappearance � Disagreement between appearance and disappearance NO ANOMALIES observed in / disappearance. Further observations needed! �� �� 2 Where are we with light sterile neutrinos? Cosmology • Constrains the effective number of relativistic species (Neff) in our universe. • A SBL neutrino would require Neff=4. • Measured Neff compatible with 3. -> Tension with SBL anomalies. • Tension relaxes when cosmological data are combined with astrophysical data. • Cosmological data alone can be compatible with • an eV-mass sterile neutrino only if its contribution to Neff is very small, • a larger Neff only if it comes from a nearly massless sterile particle. We need further observations: neutrino telescopes make it possible! 3 Sterile Neutrinos • Oscillations in the presence of sterile neutrinos are solutions of: 2 • Adding one sterile neutrino introduces 6 more free parameters: �m41 , 3 mixing angles (�14,�24,�34) and 2 more CP phases (�14, �24).
    [Show full text]
  • The ANTARES and Km3net Neutrino Telescopes: Status and Outlook for Acoustic Studies
    EPJ Web of Conferences 216, 01004 (2019) https://doi.org/10.1051/epjconf/201921601004 ARENA 2018 The ANTARES and KM3NeT neutrino telescopes: Status and outlook for acoustic studies Véronique Van Elewyck1,2, for the ANTARES and KM3NeT Collaborations 1APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, France 2Institut Universitaire de France, 75005 Paris, France Abstract. The ANTARES detector has been operating continuously since 2007 in the Mediterranean Sea, demonstrating the feasibility of an undersea neutrino telescope. Its superior angular resolution in the reconstruction of neutrino events of all flavors results in unprecedented sensitivity for neutrino source searches in the southern sky at TeV en- ergies, so that valuable constraints can be set on the origin of the cosmic neutrino flux discovered by the IceCube detector. The next generation KM3NeT neutrino telescope is now under construction, featuring two detectors with the same technology but different granularity: ARCA designed to search for high energy (TeV-PeV) cosmic neutrinos and ORCA designed to study atmospheric neutrino oscillations at the GeV scale, focusing on the determination of the neutrino mass hierarchy. Both detectors use acoustic devices for positioning calibration, and provide testbeds for acoustic neutrino detection. 1 Introduction Neutrinos have long been proposed as a complementary probe to cosmic rays and photons to explore the high-energy (HE) sky, as they can emerge from dense media and travel across cosmological dis- tances without being deflected by magnetic fields nor absorbed by inter- and intra-galactic matter and radiation. HE (>TeV) neutrinos are expected to be emitted in a wide range of astrophysical objects.
    [Show full text]
  • Pos(ICHEP2020)886
    The Outer Detector (OD) system for the Hyper-Kamiokande experiment PoS(ICHEP2020)886 Stephane Zsoldos0,1,2,∗ 0Department of Physics, King’s College London, Strand, London WC2R 2LS, United Kingdom 1Department of Physics, University of California, Berkeley, CA 94720, Berkeley, USA 2Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720-8153, USA E-mail: [email protected], [email protected] Hyper-Kamiokande, scheduled to begin construction as soon as 2020, is a next generation under- ground water Cherenkov detector, based on the highly successful Super-Kamiokande experiment. It will serve as a far detector, 295 km away, of a long baseline neutrino experiment for the upgraded J-PARC beam in Japan. It will also be a detector capable of observing — far beyond the sensitivity of the Super-Kamiokande detector — proton decay, atmospheric neutrinos, and neutrinos from astronomical sources. An Outer Detector (OD) consisting of PMTs mounted behind the inner detector PMTs and facing outwards to view the outer shell of the cylindrical tank, would provide topological information to identify interactions originating from particles outside the inner detector. Any optimization would lead to a significant improvement for the physics goals of the experiment, which are the measurement of the CP leptonic phase and the determination of the neutrino mass hierarchy. An innovative new setup using small 3" PMTs is being proposed for the Hyper-Kamiokande OD. They would give better redundancy, spatial, and angular resolution, as there would be twice or three times more photosensors that the original 8" design proposal of the experiment, and for a reduced cost.
    [Show full text]
  • Ankur Sharma
    Ankur Sharma Date of Birth 2nd August 1991 Gender Male Nationality Indian Phone +46 76 447 51 45 Address Eklundshovsvägen 4B, Lgh 1104 Email [email protected] 752 37, Uppsala, Sweden [email protected] Research Interests Phenomenological studies of VHE emission from jets of AGNs; multi-messenger and multi-wavelength connection in blazars with neutrino, gamma-ray and X-ray data; gamma-ray astronomy; observability of point sources with Cherenkov neutrino telescopes; detection strategies for ultra-high energy neutrinos Education Jan 2017 - PhD in Physics - University of Pisa (Italy) Present Area of study - Astroparticle Physics, Neutrino Astrophysics - Astroparticles, Experimental Astrophysics & Astroparticle Physics - High Energy Experimental Physics Thesis Title - Analyzing the high energy activity of candidate blazars to constrain their observability by neutrino telescopes Supervisor - Dr. Antonio Marinelli ([email protected]) Aug 2009 - Integrated M.Sc. (M.Sc. + B.Sc.) in Applied Physics - Indian Institute of Technology (ISM), Dhanbad Feb 2015 Area of study - Applied Physics - Nuclear & Particle Physics, Classical Mechanics, Quantum Mechanics, Electrodynamics - Computer Networks, Microprocessors, C++, ForTran Sept 2013 - Erasmus Mundus India4EU II Exchange Mobility - University of Porto (Portugal) July 2014 Area of study - Master Thesis, Astronomy - Stellar Structure & Evolution, Cosmology - Optical Communication, Measurement Techniques & Instrumentation Thesis Title - Constraining the Parameter Space of Dynamical
    [Show full text]
  • Geo-Neutrino Program at Baksan Neutrino Observatory Geoneutrino
    Neutrino Geoscience 2019 Prague / Book of Abstracts The deep-sea neutrino detector KM3NeT/ORCA, currently being built in the Mediterranean Seanear Toulon (France), is optimized for the study of oscillations of atmospheric neutrinos in the few-GeV energy range, with the main goal to determine the neutrino mass hierarchy. This is possible due to matter effects that modify the probability of neutrino oscillations along their path through theEarth. Measuring the energy and angular distributions of neutrinos with ORCA can therefore also provide tomographic information on the Earth’s interior and more specifically on the electron density along the trajectory of the detected neutrino, complementary to standard geophysics methods. In this contribution the latest results of a study of the potential of ORCA for Earth tomography are presented. They are based on a full Monte Carlo simulation of the detector response and including systematic effects. It is shown that after ten years of operation ORCA can measure the electron density in both the lower mantle and the outer core with a precision of a few percent in the case of normal neutrino mass hierarchy. 40 Geo-neutrino program at Baksan Neutrino Observatory Authors: Albert Gangapshev1 ; Andrey Sidorenkov2 ; Bayarto Lubsandorzhiev2 ; Daniil Kudrin2 ; Dmitry Voronin2 ; Evgeny Veretenkin2 ; Evgeny Yanovich2 ; Galina Novikova2 ; Makhti Kochkarov2 ; Nikita Ushakov2 ; Tatiana Ibragimova2 ; Valery Kuzminov1 ; Valery Petkov3 ; Vladimir Gavrin2 ; Vladimir Kazalov2 ; Yury Gavrilyuk2 ; Yury Malyshkin4 1 INR RAS, KBSU 2 INR RAS 3 INR RAS, IA RAS 4 INR RAS, INFN A new neutrino program has been recently lunched at Baksan Neutrino Observatory. It is planned to deploy a 10-kiloton scale detector based on liquid scintillator in the existing shaft at a depth of 4800 m.w.e.
    [Show full text]
  • Sensitivity to Light Sterile Neutrino Mixing Parameters with Km3net/ORCA
    Sensitivity to light sterile neutrino mixing parameters with KM3NeT/ORCA S. Aielloa, A. Albertbb,b, M. Alshamsic, S. Alves Garred, Z. Alye, A. Ambrosonef,g, F. Amelih, M. Andrei, G. Androulakisj, M. Anghinolfik, M. Anguital, G. Antonm, M. Ardidn, S. Ardidn, J. Aublinc, C. Bagatelasj, B. Baretc, S. Basegmez du Preeo, M. Bendahmanc,p, F. Benfenatiq,r, E. Berbeeo, A. M. van den Bergs, V. Bertine, S. Biagit, M. Bissingerm, M. Boettcheru, M. Bou Cabov, J. Boumaazap, M. Boutaw, M. Bouwhuiso, C. Bozzax, H.Br^anza¸sy, F. Bretaudeauz, R. Bruijno,aa, J. Brunnere, R. Brunoa, E. Buisab, R. Buompanef,ac, J. Bustoe, B. Caiffik, D. Calvod, S. Campionad,h, A. Caponead,h, V. Carreterod, P. Castaldiq,ae, S. Celliad,h, M. Chababaf, N. Chauc, A. Chenag, S. Cherubinit,ah, V. Chiarellaai, T. Chiarusiq, M. Circellaaj, R. Cocimanot, J. A. B. Coelhoc,˚, A. Coleiroc, M. Colomer Mollac,d, R. Coniglionet, P. Coylee, A. Creusotc, A. Cruzak, G. Cuttonet, R. Dallierz, B. De Martinoe, M. De Palmaaj,al, I. Di Palmaad,h, A. F. D´ıazl, D. Diego-Tortosan, C. Distefanot, A. Domik,am,˚, C. Donzaudc, D. Dornice, M. D¨orran, D. Drouhinbb,b, T. Eberlm, A. Eddyamouip, T. van Eedeno, D. van Eijko, I. El Bojaddainiw, D. Elsaesseran, A. Enzenh¨ofere, V. Espinosan, P. Fermaniad,h, G. Ferrarat,ah, M. D. Filipovi´cao, F. Filippiniq,r, L. A. Fuscoe, T. Galm, J. Garc´ıaM´endezn, A. Garcia Sotoo, F. Garufif,g, Y. Gateletc, N. Geißelbrechtm, L. Gialanellaf,ac, E. Giorgiot, S. R. Gozziniad,h, R. Graciao, K. Grafm, G. Grellaap, D.
    [Show full text]
  • The Hyper-Kamiokande Experiment Francesca Di Lodovico Queen Mary University of London
    The Hyper-Kamiokande Experiment Francesca Di Lodovico Queen Mary University of London On behalf of the Hyper-K UK collaboration PPAP Meeting July 26, 2016 A Multi-purpose Experiment Comprehensive study of oscillation • CPV Supernova • Mass hierarchy with beam+atmosph. • 23 octant • Test of exotic scenarios Nucleon decay discovery potential Sun • All visible modes including p → 푒+ 0 + Accelerator and p→휈 퐾 can be advanced beyond (J-PARC) SK. • Reaching 1035yrs sensitivity Unique Astrophysics T2HK • Precision measurement of solar • High statistics Supernova with pointing capability and energy info. • Supernova relic (non-burst ) Proton observation is also possible decay Earth core's chemical composition Etc. 2 Inaugural Symposium of the HK proto- collaboration@Kashiwa, Jan-2015 12 countries, ~250 members and growing KEK-IPNS and • Proto-collaboration formed. UTokyo-ICRR • International steering group signed a MoU for • International conveners cooperation • International chair for international on the Hyper- board of representative (IBR) Kamiokande project. 26/July/2016 The Hyper-Kamiokande Experiment 3 Proto-Collaboration IRFU, CEA Saclay (France) Gifu University (Japan) Laboratoire Leprince-Ringuet, Ecole Polytechnique (France) High Energy Accelerator Research Organization (KEK) (Japan) Lancaster University (UK) Kobe University (Japan) Los Alamos National Laboratory (USA) Kyoto University (Japan) Louisiana State University (USA) Miyagi University of Education (Japan) National Centre for Nuclear Research (Poland) Nagoya University
    [Show full text]
  • Icecube and Km3net: Lessons and Relations
    Elsevier Science 1 Journal logo IceCube and KM3NeT: Lessons and Relations Christian Spiering DESY, Platanenallee 6, Zeuthen, 15738 Germany Elsevier use only: Received date here; revised date here; accepted date here Abstract This talk presents conclusions for KM3NeT which may be drawn from latest IceCube results and from optimization studies of the IceCube configuration. It discusses possible coordinated efforts between IceCube and KM3NeT (or, for the time being, IceCube and ANTARES). Finally, it lists ideas for formal relations between neutrino telescopes on the cubic kilometer scale. © 2001 Elsevier Science. All rights reserved Keywords: Neutrino Telescopes 1. Introduction The IceCube neutrino telescope at the South Pole Assuming one detector on the Southern is approaching its completion and meanwhile has hemisphere (IceCube) and one or more detectors at provided first results from data taken with initial the Northern hemisphere (by now ANTARES [10] configurations [1]. KM3NeT will act as IceCube’s and NT200 [11], in the future KM3NeT [12] and counterpart on the Northern hemisphere, with a GVD [13]), various possibilities for coordinated sensitivity “substantially exceeding that of all physics programs and analyses open up. They are existing neutrino telescopes including IceCube” [2]. discussed in sections 3 and 4. KM3NeT is just finishing its design phase [3], but Finally, section 5 lists formal and procedural has not yet converged to a final configuration. The possibilities of cooperation between KM3NeT and cited sensitivity requirement results not only from IceCube. gamma ray observations and their phenomenological interpretation (see e.g. [4-9]), but also from early IceCube data. The first section of this paper is 2.
    [Show full text]
  • 35. Particle Detectors for Non-Accelerator Physics
    1 35. Particle Detectors for Non-Accelerator Physics 35. Particle Detectors for Non-Accelerator Physics 35.1 Introduction . 1 35.2 High-energy cosmic-ray hadron and gamma-ray detectors . 2 35.2.1 Atmospheric fluorescence detectors . 2 35.2.2 Atmospheric Cherenkov telescopes for high-energy gamma ray astronomy . 5 35.3 Large neutrino detectors . 8 35.3.1 Deep liquid detectors for rare processes . 8 35.3.2 Neutrino telescopes . 12 35.3.3 Radio emission from (ultra-)high energy particle showers . 20 35.4 Large time-projection chambers for rare event detection . 27 35.4.1 Dark matter and other low energy signals . 28 35.4.2 0νββ Decay . 31 35.5 Sub-Kelvin detectors . 32 35.5.1 Equilibrium thermal detectors . 32 35.5.2 Nonequilibrium Detectors . 34 35.6 Low-radioactivity background techniques . 36 35.6.1 Defining the problem . 37 35.6.2 Environmental radioactivity . 37 35.6.3 Radioactive impurities in detector and shielding components . 39 35.6.4 Radon and its progeny . 40 35.6.5 Cosmic rays . 41 35.6.6 Neutrons . 42 35.1 Introduction Non-accelerator experiments have become increasingly important in particle physics. These include cosmic ray experiments (with surface, space and underground detectors), neutrino oscilla- tion measurements with solar and atmospheric neutrinos in underground laboratories, searches for neutrino-less double beta decays and dark matter candidates again in underground laboratories, and searches for more exotic phenomena. The detectors are in the majority of the cases differ- ent from those used at accelerators. Even when the detectors are based on the same physics (e.
    [Show full text]
  • Groupe Neutrino
    Groupe Neutrino HCERES Report 2013-17 Present Composition •[9] permanents –Stavros Katsanevas* (Prof),Antoine Kouchner* (Prof), Thomas Patzak* (Prof), Véronique Van Elewyck (MC), Alessandra Tonazzo* (Prof) –Anatael Cabrera (CR), Jaime Dawson(CR), Davide Franco*(CR) –Thierry Lasserre* (DR CEA) [*HDR] •[4] postdocs –Marco Grassi, LiquidO, Marie Curie, –Anthony Onillon, Double Chooz, IN2P3, 15/09/2015 – 14/09/2018 –Christine Nielson, KM3NeT/ORCA, 09/2017 – –Stefan Wagner, LiquidO, CDD, July. 2017 – June. 2018 •[5] PhD students –Theodoros Avgitas*, CD , Antoine Kouchner, 11/2014 – 11/2017 –Simon Bourret*, AMX, Veronique Van Elewyk (Eduoard Kaminksi), 09/2015 –2018 –Timothée Gregoire*, CDE , Antoine Kouchner, 10/2015- 2018 –Yan Han, CSC, Anatael Cabrera, 09/2017 – 2020 –Andrea Scarpelli, CD , Thomas Patzak & Alessandra Tonazzo, 10/2016 – 2019 [*aussi membres du groupe Haute Energies – KM3NET] Recent Evolution (last 5 years) - I •Permanents Christiano Galbiati, DarkSide, invited professeur UPSC, 03/2016 – 12/2016 Fumihiko Suekane, LiquidO, chair Blaise-Pascal , 04/2017 – 11/2018 Michel Cribier (CEA DR), emeritus 2009 Herve de Kerret (DR), emeritus 2014 Francois Vannucci (PR), emeritus 2012 Daniel Vignaud (DR), emeritus 2007 Didier Kryn (CR), retired 2013 Michel Obolensky (CR), retired 2015 •Postdocs Hector Gomez, DoubleChooz/MuonTomography, labex UnivEarth (E4), 09/2014 - 09/2017 Joao de Abreu Barbosa Coelho, KM3NET ORCA, labex UnivEarth (E4), 12/2015 – 09/2017 Quentin Riffard, DarkSide, UnivEarth (E4), 11/2015 – 09/2017 Romain Roncin, Borexino/SOX,
    [Show full text]
  • Neutrino Beam from Protvino to Km3net/ORCA
    Neutrino Beam from Protvino to KM3NeT/ORCA Contact : J. Brunner Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France December 18, 2018 Abstract The Protvino accelerator facility located in the Moscow region, Russia, is in a good position to enable a rich experimental research program in the field of neutrino physics. Of particular interest is the possibility to direct a neutrino beam from Protvino towards the KM3NeT/ORCA detector which is currently under construction in the Mediterranean sea 40 km offshore Toulon, France. Such an experiment, nicknamed P2O (Protvino-to-ORCA), would yield an unparalleled sensitivity to matter effects in the Earth, allowing to determine the neutrino mass ordering with a high level of certainty due to its baseline of 2595 km after only few years of running time at a modest beam intensity up to 100 kW. A second phase of the experiment, comprizing a further intensity upgrade of the accelerator complex and a significant densification of the ORCA detector would allow for a competitive and complementary measurement of the leptonic CP- violating Dirac phase with a Mton detector but avoiding underground excavation costs. The initial composition and energy spectrum of the neutrino beam would need to be monitored by a near detector, to be constructed several hundred meters downstream from the proton beam target. The same neutrino beam and near detector set-up would also allow for neutrino-nuclei cross section measurements to be conducted. 1 1 Introduction Neutrino physics is one of the most actively developing branches of particle physics, with many fundamental parameters still awaiting to be experimentally determined, as well as great promise for new insights into physics beyond the Standard Model.
    [Show full text]
  • Performance Studies for the Km3net Neutrino Telescope
    Performance Studies for the KM3NeT Neutrino Telescope Der Naturwissenschaftlichen Fakult¨at der Friedrich-Alexander-Universit¨at Erlangen-Nu¨rnberg zur Erlangung des Doktorgrades vorgelegt von Claudio Kopper aus Erlangen Als Dissertation genehmigt von der Naturwissenschaftlichen Fakult¨at der Friedrich-Alexander-Universit¨at Erlangen-Nurnberg¨ Tag der mundlichen¨ Prufung:¨ 12. M¨arz 2010 Vorsitzender der Promotionskommission: Prof. Dr. Eberhard B¨ansch Erstberichterstatter: Prof. Dr. Ulrich Katz Zweitberichterstatter: Prof. Dr. Christian Stegmann Meinen Eltern Contents Introduction9 I Basics 13 1 High energy cosmic neutrinos 15 1.1 Neutrinos in the Standard Model.................... 15 1.2 Cosmic accelerators............................ 16 1.2.1 The cosmic ray spectrum.................... 16 1.2.2 Particle acceleration....................... 17 1.2.3 Neutrino production....................... 20 1.2.4 Source candidates........................ 21 2 Neutrino telescopes 25 2.1 Detection mechanism........................... 25 2.1.1 Neutrino interaction....................... 25 2.1.2 Cherenkov radiation from charged particles.......... 29 2.1.3 Muon propagation........................ 29 2.1.4 Electromagnetic and hadronic cascades............ 30 2.1.5 Light propagation........................ 31 2.1.6 Light detection.......................... 32 2.1.7 Triggering............................. 33 2.1.8 Muon track reconstruction.................... 33 2.1.9 Background............................ 34 2.2 Existing neutrino telescopes......................
    [Show full text]