DOCSLIB.ORG

Neutrinoless Double Beta Decay Beyond the “Lobster” Plot and Its Connection to Cosmology

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Neutrinoless Double Beta Decay Beyond the “Lobster” Plot and Its Connection to Cosmology Neutrinoless double beta decay beyond the “lobster” plot and its connection to cosmology Julia Harz ACFI Snowmass Workshop 2020 Neutrinos – what do we know? Illustration by Sandbox Studio, Chicago “Neutrinos, the Standard Model misfits” Julia Harz BSM theory overview of neutrinoless double beta decay 2 Neutrinos – what do we know? ● Neutrinos in the Standard Model are massless ● Neutrino mixing ● Neutrino oscillations require massive neutrinos ● Normal vs. inverted hierarchy How do neutrinos get their masses? What nature do neutrinos have? Are they their own anti-particles? Julia Harz BSM theory overview of neutrinoless double beta decay 3 Why Lepton-Number Violation? ● Masses of the active neutrinos cannot be explained within the SM ● BUT right-handed neutrinos could help Dirac mass Majorana mass 1/2 -1/2 0 0 0 hypercharge -1/2 1/2 ● tiny Yukawa couplings 1/21/2 -1/2 1/2 not at tree-level within the SM possible ● Lepton number no accidental symmetry anymore ● higher dimensional operator ● Lepton number violation (LNV) Julia Harz BSM theory overview of neutrinoless double beta decay 4 Lepton-Number Violation ● LNV occurs only at odd mass dimension: 3/2 3/2 1 1 mass dimension Babu, Leung (2001), de Gouvea, Jenkins (2007), Deppisch, Graf, JH, Huang (2017) Julia Harz BSM theory overview of neutrinoless double beta decay 5 Radiative neutrino mass generation ● LNV occurs only at odd mass dimension: Deppisch, Graf, JH, Huang (2017) Julia Harz BSM theory overview of neutrinoless double beta decay 6 Probing LNV interactions – 0vββ decay Neutrinoless double beta decay Most stringent limits are currently set by GERDA and Kamland-Zen: u u d d nuclear matrix element d d particle physics u u phase space factor standard mass mechanism long range contribution short range contribution ? = 0vββ decay probes only first generation! Julia Harz BSM theory overview of neutrinoless double beta decay 7 Schechter-Valle Theorem – Black Box Theorem Schechter, Valle (1982) Any ΔL = 2 operator that leads to 0vbb will induce a Majorana mass contribution via loop Dürr, Merle, Lindner (2011) 9-dim ΔL = 2 operator will lead to 0vbb but only tiny contribution to neutrino mass Observation of 0vββ decay does not imply that the mass mechanism is the dominant contribution. Julia Harz BSM theory overview of neutrinoless double beta decay 8 Constraining LNV interactions long range contribution standard mass mechanism ? ? = = Leptonic and hadronic current with different chirality structure: Deppisch, Hirsch, Päs (2012) Julia Harz BSM theory overview of neutrinoless double beta decay 9 Scales of New Physics 1st generation couplings 7-dim Non-standard 9-dim mechanism 11-dim effective coupling can be related to the scale of the operator only mass mechanism Deppisch, Graf, JH, Huang (2017) Deppisch, JH, Huang, Hirsch, Päs (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 10 Scales of New Physics 3rd generation couplings only mass mechanism 7-dim 9-dim non-standard mechanism 11-dim Deppisch, Graf, JH, Huang (2017) Deppisch, JH, Huang, Hirsch, Päs (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 11 Uncertainties of Nuclear Matrix Elements nuclear physics ● Dependence on isotope and specific operator ● Differences between different nuclear models ● “the gA problem” quenching of the axial-vector coupling? e.g. Suhonen et al., Engel et al., and many more Engel, Menendez (2016) Julia Harz BSM theory overview of neutrinoless double beta decay 12 Topologies for Neutrinoless Double Beta Decay Bonnet, Hirsch, Ota, Winter (2014) Julia Harz BSM theory overview of neutrinoless double beta decay 13 Neutrinoless Double Beta Decay at the LHC Example: Left-Right Symmetric Model Helo, Kovalenko, Hirsch, Päs (2013) Julia Harz BSM theory overview of neutrinoless double beta decay 14 Neutrinoless Double Beta Decay at the LHC Different possible contributions to 0vbb: Corresponding process at LHC: Helo, Kovalenko, Hirsch, Päs (2013) Julia Harz BSM theory overview of neutrinoless double beta decay 15 Neutrinoless Double Beta Decay at the LHC Different possible contributions to 0vbb: Corresponding process at LHC: Helo, Kovalenko, Hirsch, Päs (2013) Julia Harz BSM theory overview of neutrinoless double beta decay 16 Neutrinoless Double Beta Decay at the LHC Refined study of one model: Including: ● SM + detector background ● running of the operators ● long distance contributions Peng, Ramsey-Musolf, Winslow (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 17 QCD corrections and running Leading order QCD corrections to the complete set of the short-range d = 9 0νββ-operators covering the low-energy limits of any possible underlying high-energy scale model e.g. Gonzalez, Hirsch, Kovalenko (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 18 QCD corrections and running ● QCD corrections can give sizeable impact to short range contribution Gonzalez, Hirsch, Kovalenko (2015) ● QCD corrections sub-dominant for long range contribution (less than 60%) Arbelaez, Gonzalez, Hirsch, Kovalenko (2016) ● Extrapolation of perturbative results to sub-GeV non-perturbative scales on the basis of QCD coupling constant “freezing” behavior using Background Perturbation Theory → only moderate dependence Gonzalez, Hirsch, Kovalenko (2018) Julia Harz BSM theory overview of neutrinoless double beta decay 19 “Master formula” Cirigliano, Dekens, de Vries, Graesser, Mereghetti (2017, 2018) Graf, Deppisch, Iachello, Kotila (2018) Julia Harz BSM theory overview of neutrinoless double beta decay 20 “Master formula” Cirigliano, Dekens, de Vries, Graesser, Mereghetti (2017, 2018) Graf, Deppisch, Iachello, Kotila (2018) Julia Harz BSM theory overview of neutrinoless double beta decay 21 A new leading contribution to 0vββ Cirigliano, Dekens, de Vries, Graesser, Mereghetti, Pastore, van Kolck (2018) Julia Harz BSM theory overview of neutrinoless double beta decay 22 Implications on Leptogenesis ● generation of lepton asymmetry via heavy neutrino decays ● competition with lepton number violating (LNV) washout processes ● conversion to baryon asymmetry via sphaleron processes Fukugita et al. 1986 source of CP violation L H L L H N N N N N sphaleron processes H H L L H N Q N L L L L H L H H N H N washout N u Q L u H H H processesL L H scattering processes washout processes Julia Harz BSM theory overview of neutrinoless double beta decay 23 Implications on Leptogenesis The generation of a baryon asymmetry – baryogenesis – can be created by a lepton asymmetry – leptogenesis: baryon asymmetry SM processes Possible tight link to neutrino physics lepton asymmetry lepton lepton Possibly asymmetry asymmetry at high generation washout scales (CPV and LNV) (LNV) In turn, lepton number violation (LNV) can destroy a lepton asymmetry, and thus even a baryon asymmetry! Julia Harz BSM theory overview of neutrinoless double beta decay 24 Lepton Asymmetry Washout ● LNV operator would cause washout of pre-existing net lepton asymmetry in the early Universe operator specific factor ● washout efficient if lepton density If 0vßß is observed, washout efficient in the temperature interval Julia Harz BSM theory overview of neutrinoless double beta decay 25 0vββ and Baryogenesis limit above which the washout is highly effective Potential to falsify baryogenesis models! Deppisch, Graf, JH, Huang (2018) Deppisch, JH, Huang, Hirsch, Päs (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 26 Lepton asymmetry washout 1st generation couplings 7-dim 9-dim 11-dim Deppisch, Graf, JH, Huang (2017) Deppisch, JH, Huang, Hirsch, Päs (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 27 Distinguishing different operators Dell’Oro, Marcocci, Viel, Vissani (2016) ● discrepancy between sum of neutrino masses from cosmology and 0vββ half life measurements could indicate non-standard mechanism ● Angular distributions allows to discriminate O7 - + from others, due to e R and e L in the final state Ali, Borisov, Zhuridov (2006), SuperNemo, Arnold et al. (2010) Julia Harz BSM theory overview of neutrinoless double beta decay 28 Distinguishing different operators ● distinguishing between different mechanisms via measurements in different isotopes Deppisch, Päs (2006) Gehmann, Elliot (2007) ● observation of 0vββ via O9 and O11 will imply observation of LNV at LHC Julia Harz BSM theory overview of neutrinoless double beta decay 29 Probing LNV interactions – LHC Washout processes could be observable at the LHC LNV Observation of any washout process at LHC would falsify high scale baryogenesis! (scale of asymmetry generation above M ) Deppisch, JH, Hirsch, Phys. Rev. Lett. (2014) X Deppisch, JH, Hirsch, Päs, Int. J. Mod. Phys. A (2015) Julia Harz BSM theory overview of neutrinoless double beta decay 30 Combining LHC & 0vββ collider 0vββ washout too big to generate collider Comprehensive analysis confirms EFT results and shows interesting interplay between collider and 0vββ reach. JH, Ramsey-Musolf, Shen, Urrutia, in preparation Julia Harz BSM theory overview of neutrinoless double beta decay 31 Constraining LNV interactions with rare kaon decays u K+ π+ u u K+ π+ u s d s d ● GIM suppressed ● No GIM suppression Not explicit LNV! ● Includes first and second generation How are higher dimensional operators constraint by rare kaon decays? Deppisch, Fridell, JH (2020) Julia Harz BSM theory overview of neutrinoless double beta decay 32 Constraining power at E949 ● SM, lepton number conserving vector current Deppisch, JH, Fridell (2020) signal region 1 SR 2
Load more

Recommended publications
  • The Gran Sasso Underground Laboratory Program
    The Gran Sasso Underground Laboratory Program Eugenio Coccia INFN Gran Sasso and University of Rome “Tor Vergata” [email protected] XXXIII International Meeting on Fundamental Physics Benasque - March 7, 2005 Underground Laboratories Boulby UK Modane France Canfranc Spain INFN Gran Sasso National Laboratory LNGSLNGS ROME QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. L’AQUILA Tunnel of 10.4 km TERAMO In 1979 A. Zichichi proposed to the Parliament the project of a large underground laboratory close to the Gran Sasso highway tunnel, then under construction In 1982 the Parliament approved the construction, finished in 1987 In 1989 the first experiment, MACRO, started taking data LABORATORI NAZIONALI DEL GRAN SASSO - INFN Largest underground laboratory for astroparticle physics 1400 m rock coverage cosmic µ reduction= 10–6 (1 /m2 h) underground area: 18 000 m2 external facilities Research lines easy access • Neutrino physics 756 scientists from 25 countries Permanent staff = 66 positions (mass, oscillations, stellar physics) • Dark matter • Nuclear reactions of astrophysics interest • Gravitational waves • Geophysics • Biology LNGS Users Foreigners: 356 from 24 countries Italians: 364 Permanent Staff: 64 people Administration Public relationships support Secretariats (visa, work permissions) Outreach Environmental issues Prevention, safety, security External facilities General, safety, electrical plants Civil works Chemistry Cryogenics Mechanical shop Electronics Computing and networks Offices Assembly halls Lab
    [Show full text]
  • Radiochemical Solar Neutrino Experiments, "Successful and Otherwise"
    BNL-81686-2008-CP Radiochemical Solar Neutrino Experiments, "Successful and Otherwise" R. L. Hahn Presented at the Proceedings of the Neutrino-2008 Conference Christchurch, New Zealand May 25 - 31, 2008 September 2008 Chemistry Department Brookhaven National Laboratory P.O. Box 5000 Upton, NY 11973-5000 www.bnl.gov Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-AC02-98CH10886 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This preprint is intended for publication in a journal or proceedings. Since changes may be made before publication, it may not be cited or reproduced without the author’s permission. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors.
    [Show full text]
  • Astrophysical Neutrinos at the Low and High Energy Frontiers by Lili Yang A
    Astrophysical neutrinos at the low and high energy frontiers by Lili Yang A Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy Approved November 2013 by the Graduate Supervisory Committee: Cecilia Lunardini, Chair Ricardo Alarcon Igor Shovkovy Francis Timmes Tanmay Vachaspati ARIZONA STATE UNIVERSITY December 2013 ABSTRACT For this project, the diffuse supernova neutrino background (DSNB) has been calcu- lated based on the recent direct supernova rate measurements and neutrino spectrum from SN1987A. The estimated diffuse n¯ flux is 0.10 – 0.59 cm 2s 1 at 99% confi- e ⇠ − − dence level, which is 5 times lower than the Super-Kamiokande 2012 upper limit of 3.0 2 1 cm− s− , above energy threshold of 17.3 MeV. With a Megaton scale water detector, 40 events could be detected above the threshold per year. In addition, the detectability of neutrino bursts from direct black hole forming col- lapses (failed supernovae) at Megaton detectors is calculated. These neutrino bursts are energetic and with short time duration, 1s. They could be identified by the time coin- ⇠ cidence of N 2 or N 3 events within 1s time window from nearby (4 – 5 Mpc) failed ≥ ≥ supernovae. The detection rate of these neutrino bursts could get up to one per decade. This is a realistic way to detect a failed supernova and gives a promising method for studying the physics of direct black hole formation mechanism. Finally, the absorption of ultra high energy (UHE) neutrinos by the cosmic neutrino background, with full inclusion of the effect of the thermal distribution of the back- ground on the resonant annihilation channel, is discussed.
    [Show full text]
  • THE BOREXINO IMPACT in the GLOBAL ANALYSIS of NEUTRINO DATA Settore Scientifico Disciplinare FIS/04
    UNIVERSITA’ DEGLI STUDI DI MILANO DIPARTIMENTO DI FISICA SCUOLA DI DOTTORATO IN FISICA, ASTROFISICA E FISICA APPLICATA CICLO XXIV THE BOREXINO IMPACT IN THE GLOBAL ANALYSIS OF NEUTRINO DATA Settore Scientifico Disciplinare FIS/04 Tesi di Dottorato di: Alessandra Carlotta Re Tutore: Prof.ssa Emanuela Meroni Coordinatore: Prof. Marco Bersanelli Anno Accademico 2010-2011 Contents Introduction1 1 Neutrino Physics3 1.1 Neutrinos in the Standard Model . .4 1.2 Massive neutrinos . .7 1.3 Solar Neutrinos . .8 1.3.1 pp chain . .9 1.3.2 CNO chain . 13 1.3.3 The Standard Solar Model . 13 1.4 Other sources of neutrinos . 17 1.5 Neutrino Oscillation . 18 1.5.1 Vacuum oscillations . 20 1.5.2 Matter-enhanced oscillations . 22 1.5.3 The MSW effect for solar neutrinos . 26 1.6 Solar neutrino experiments . 28 1.7 Reactor neutrino experiments . 33 1.8 The global analysis of neutrino data . 34 2 The Borexino experiment 37 2.1 The LNGS underground laboratory . 38 2.2 The detector design . 40 2.3 Signal processing and Data Acquisition System . 44 2.4 Calibration and monitoring . 45 2.5 Neutrino detection in Borexino . 47 2.5.1 Neutrino scattering cross-section . 48 2.6 7Be solar neutrino . 48 2.6.1 Seasonal variations . 50 2.7 Radioactive backgrounds in Borexino . 51 I CONTENTS 2.7.1 External backgrounds . 53 2.7.2 Internal backgrounds . 54 2.8 Physics goals and achieved results . 57 2.8.1 7Be solar neutrino flux measurement . 57 2.8.2 The day-night asymmetry measurement . 58 2.8.3 8B neutrino flux measurement .
    [Show full text]
  • Measurement of Muon Neutrino Disappearance with the Nova Experiment Luke Vinton
    Measurement of Muon Neutrino Disappearance with the NOvA Experiment Luke Vinton Submitted for the degree of Doctor of Philosophy University of Sussex 14th February 2018 Declaration I hereby declare that this thesis has not been and will not be submitted in whole or in part to another University for the award of any other degree. Signature: Luke Vinton iii UNIVERSITY OF SUSSEX Luke Vinton, Doctor of Philosophy Measurement of muon neutrino disappearance with the NOvA experiment Abstract The NOvA experiment consists of two functionally identical tracking calorimeter detectors which measure the neutrino energy and flavour composition of the NuMI beam at baselines of 1 km and 810 km. Measurements of neutrino oscillation parameters are extracted by comparing the neutrino energy spectrum in the far detector with predictions of the oscil- lated neutrino energy spectra that are made using information extracted from the near detector. Observation of muon neutrino disappearance allows NOvA to make measure- 2 ments of the mass squared splitting ∆m32 and the mixing angle θ23. The measurement of θ23 will provide insight into the make-up of the third mass eigenstate and probe the muon-tau symmetry hypothesis that requires θ23 = π=4. This thesis introduces three methods to improve the sensitivity of NOvA's muon neut- rino disappearance analysis. First, neutrino events are separated according to an estimate of their energy resolution to distinguish well resolved events from events that are not so well resolved. Second, an optimised neutrino energy binning is implemented that uses finer binning in the region of maximum muon neutrino disappearance. Third, a hybrid selection is introduced that selects muon neutrino events with greater efficiency and purity.
    [Show full text]
  • The Search for 0Νββ Decay in 130Te with CUORE-0 by Jonathan Loren
    The Search for 0νββ Decay in 130Te with CUORE-0 by Jonathan Loren Ouellet Ph.D. Thesis Department of Physics University of California, Berkeley Berkeley, Ca 94720 and Nuclear Science Division Ernest Orlando Lawrence National Laboratory Berkeley, Ca 94720 Spring 2015 This material is based upon work supported by the US Department of Energy (DOE) Office of Science under Contract No. DE-AC02-05CH11231 and by the National Science Foundation under Grant Nos. NSF-PHY-0902171 and NSF-PHY-1314881. DISCLAIMER This document was prepared as an account of work sponsored by the United States Gov- ernment. While this document is believed to contain correct information, neither the United States Government nor any agency thereof, nor the Regents of the University of California, nor any of their employees, makes any warranty, express or implied, or assumes any legal responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by its trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof, or the Regents of the University of California. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof or the Regents of the University of California. The Search for 0νββ Decay in 130Te with CUORE-0 by Jonathan Loren Ouellet A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Yury Kolomensky, Chair Professor Gabriel Orebi Gann Professor Eric B.
    [Show full text]
  • Retrospect of GALLEX/GNO
    10th Int. Conf. on Topics in Astroparticle and Underground Physics (TAUP2007) IOP Publishing Journal of Physics: Conference Series 120 (2008) 052013 doi:10.1088/1742-6596/120/5/052013 Retrospect of GALLEX/GNO Till Kirsten Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany E-mail: [email protected] Abstract. After the completion of the gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso (GALLEX, GNO), we shortly summarize the major achievements. Among them are the first observation of solar pp-neutrinos and the recognition of a substantial (40%) deficit of sub-MeV solar neutrinos that called for νe transformations enabled by non- vanishing neutrino masses. We also inform about a recent complete re-analysis of the GALLEX data evaluation and reflect on the causes for the termination of GNO. From our gallium data we extract the e-e survival probability Pee for pp-neutrinos after subtraction of the 8B and 7Be contributions based on the experimentally determined 8B- (SNO/SK) and 7Be- (Borexino) neutrino fluxes as Pee(pp only) = 0.52 ± 0.12. 1. Introduction The Gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso have been terminated for external non-scientific reasons. This triggers a short retrospect of the achievements of GALLEX and GNO (Section 2). In Section 3 we report on a recent update that is based on data that were impossible to acquire before completion of the low rate measurement phase (solar runs). After some reflections on the causes for the termination of the gallium experiments at Gran Sasso (Section 4), I give a first quantitative estimate of the separate pp solar neutrino production (Section 5).
    [Show full text]
  • Current Research on Neutrinos
    UNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos Stefania Ricciardi HEP PostGraduate Lectures 2016 University of London 1 Neutrino Sources • Artificial: SUN – nuclear reactors First detected neutrinos – particle accelerators • Natural: – Sun Atmosphere – Atmosphere – SuperNovae – fission in the Earth core (geoNeutrinos) – Astrophysical origin (Old supernovae, AGN, etc.) Expected, but undetected so far,: – relic neutrinos from BigBang (~300/cm3 ) SuperNovae Neutrinos are everywhere! 2 Neutrino Flux vs Energy The Sun is the most intense detected source with a flux on Earth of of 6 1010 n/cm2s Abundant Detection of solar but challenging and atmospheric detection neutrino has provided the first compelling evidence of neutrino oscillations Below detection threshold of current experiments 3 D.Vignaud and M. Spiro, Nucl. Phys., A 654 (1999) 350 Atmospheric Neutrinos 4 Neutrino Production in the Atmosphere Absolute n flux has ~10% uncertainty But muon/electron neutrino ratio is known with ~3% uncertainty. Expected: (n n ) 2 (ne n e) 5 6 Cosmic Flux Isotropy We expect an isotropic Flux of neutrinos at high energies (earth magnetic field deviate path of low-momentum secondaries only : East-West effects) For En > a few GeV, and a given n flavour (Up-going / down-going) ~ 1.0 with <1 % uncertainty Note the baseline (= distance nproduction-ndetection) spans 3 order of magnitudes! 7 Atmospheric neutrino detectors Neutrinos in 100 MeV – 10 GeV energy. Flux ~ 1 event/(cm2 sr sec) Quasi-elastic interaction region Small cross-section Massive Detector (kTons) Background from charged cosmic rays deep underground location:mines, caverns under mountains, provide >1 Km rock overburden necessary to reduce the muon flux by 5-6 orders of magnitude 2 detection techniques: - Calorimetric - iron and tracking detectors (Nusex, Frejus, Soudan) - Cherenkov - water (Kamiokande, IMB) First detectors built to search for proton-decay.
    [Show full text]
  • Detecting Fast Time Variations in the Supernova Neutrino Flux with Hyper-Kamiokande
    Max-Planck-Institut für Physik Technische Universität München (Werner-Heisenberg-Institut) Fakultät für Physik Abschlussarbeit im Masterstudiengang Physik Detecting Fast Time Variations in the Supernova Neutrino Flux with Hyper-Kamiokande Suche nach hochfrequenten Oszillationen des Supernovaneutrino-Flusses mit Hyper-Kamiokande Jost Migenda 2015-06-22 arXiv:1609.04286v1 [physics.ins-det] 14 Sep 2016 “However big you think supernovae are, they’re bigger than that.” — Donald Spector [1] Themensteller: Prof. Dr. Lothar Oberauer Betreuer: Dr. habil. Georg G. Raffelt Datum des Kolloquiums: 8. Juli 2015 Abstract For detection of neutrinos from galactic supernovae, the planned Hyper- Kamiokande detector will be the first detector that delivers both a high event rate (about one third of the IceCube rate) and event-by-event energy information. In this thesis, we use a three-dimensional computer simulation by the Garching group to find out whether this additional information can be used to improve the detection prospects of fast time variations in the neutrino flux. We find that the amplitude of SASI oscillations of the neutrino number flux is energy-dependent. However, in this simulation, the larger amplitude in some energy bins is not sufficient to counteract the increased noise caused by the lower event rate. Finally, we derive a condition describing when it is advantageous to consider an energy bin instead of the total signal and show that this condition is satisfied if the oscillation of the mean neutrino energy is increased slightly. iii Contents Abstract ........................................ iii 1 Introduction .....................................1 2 Core-Collapse Supernovae ............................5 2.1 Classification of Supernovae . .5 2.1.1 Spectral Classification .
    [Show full text]
  • Redalyc.Neutrino Physics (Rapporteur Talk)
    Brazilian Journal of Physics ISSN: 0103-9733 [email protected] Sociedade Brasileira de Física Brasil Nakahata, Masayuki Neutrino Physics (Rapporteur talk) Brazilian Journal of Physics, vol. 44, núm. 5, 2014, pp. 465-482 Sociedade Brasileira de Física Sâo Paulo, Brasil Available in: http://www.redalyc.org/articulo.oa?id=46432476005 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative Braz J Phys (2014) 44:465–482 DOI 10.1007/s13538-014-0228-4 PARTICLES AND FIELDS Neutrino Physics (Rapporteur talk) Masayuki Nakahata Received: 28 April 2014 / Published online: 31 May 2014 © Sociedade Brasileira de F´ısica 2014 Abstract Papers related to neutrino physics, submitted in in this short rapporteur report, only papers that have notable the categories NU-EX (experimental results), NU-IN (meth- results have been selected. ods, techniques, and instrumentation) and NU-TH (theory, model, and simulations) are reviewed with a brief introduc- tion on the current understanding of neutrino masses and 2 Neutrino Masses and Mixings mixings. Before discussing the contributed papers at ICRC2013, our Keywords Neutrino current understanding of neutrino masses and mixings will be described. The relation between the mass eigenstates (ν1, ν2,andν3) and the weak interaction (flavor) eigenstates (νe, 1 Introduction νμ,andντ ) can be written: ⎛ ⎞ ⎛ ⎞ ⎛ ⎞ The categories NU-EX, NU-IN, and NU-TH at ICRC2013 νe Ue1 Ue2 Ue3 ν1 ⎝ ⎠ = ⎝ ⎠ ⎝ ⎠ cover neutrino physics over a wide energy range.
    [Show full text]
  • The Variation of the Solar Neutrino Fluxes Over Time in the Homestake, GALLEX(GNO) and Super-Kamiokande Experiments
    The Variation of the Solar Neutrino Fluxes over Time in the Homestake, GALLEX(GNO) and Super-Kamiokande Experiments K. Sakurai1,3, H. J. Haubold2 and T. Shirai1 1. Institute of Physics, Kanagawa University, Yokohama 221-8686, Japan 2. Office for Outer Space Affairs, United Nations, P. O. Box 500, A-1400, Vienna, Austria 3. Advanced Research Institute for Science and Engineering, Waseda University, Shinjuku, Tokyo 169-8555, Japan Abstract Using the records of the fluxes of solar neutrinos from the Homestake, GALLEX (GNO), and Super-Kamiokande experiments, their statistical analyses were performed to search for whether there existed a time variation of these fluxes. The results of the analysis for the three experiments indicate that these fluxes are varying quasi-biennially. This means that both efficiencies of the initial p-p and the PP-III reactions of the proton-proton chain are varying quasi-biennially together with a period of about 26 months. Since this time variation prospectively generated by these two reactions strongly suggests that the efficiency of the proton-proton chain as the main energy source of the Sun has a tendency to vary quasi-biennially due to some chaotic or non-linear process taking place inside the gravitationally stabilized solar fusion reactor. It should be, however, remarked that, at the present moment, we have no theoretical reasoning to resolve this mysterious result generally referred to as the quasi-biennial periodicity in the time variation of the fluxes of solar neutrinos. There is an urgent need to search for the reason why such a quasi-biennial periodicity is caused through some physical process as related to nuclear fusion deep inside the Sun.
    [Show full text]
  • Direct Measurement of the Pp Solar Neutrino Interaction Rate in Borexino
    University of Massachusetts Amherst ScholarWorks@UMass Amherst Doctoral Dissertations Dissertations and Theses Spring August 2014 Direct Measurement of the pp Solar Neutrino Interaction Rate in Borexino Keith Otis University of Massachusetts Amherst Follow this and additional works at: https://scholarworks.umass.edu/dissertations_2 Part of the Elementary Particles and Fields and String Theory Commons, and the The Sun and the Solar System Commons Recommended Citation Otis, Keith, "Direct Measurement of the pp Solar Neutrino Interaction Rate in Borexino" (2014). Doctoral Dissertations. 123. https://doi.org/10.7275/nh2x-z694 https://scholarworks.umass.edu/dissertations_2/123 This Open Access Dissertation is brought to you for free and open access by the Dissertations and Theses at ScholarWorks@UMass Amherst. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. DIRECT MEASUREMENT OF THE PP SOLAR NEUTRINO INTERACTION RATE IN BOREXINO A Dissertation Presented by KEITH OTIS Submitted to the Graduate School of the University of Massachusetts Amherst in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY May 2014 Physics c Copyright by Keith Otis 2014 All Rights Reserved DIRECT MEASUREMENT OF THE PP SOLAR NEUTRINO INTERACTION RATE IN BOREXINO A Dissertation Presented by KEITH OTIS Approved as to style and content by: Andrea Pocar, Chair Laura Cadonati, Member Krishna Kumar, Member Grant Wilson, Member Rory Miskimen, Department Chair Physics To my family; you have each helped me become who I am today. FOREWORD The results of this dissertaion are self contained and all the information needed to reach its conclustions has been presented in detail.
    [Show full text]