Solar neutrinos: The Beginning at MPIK. W. Hampel
|
|
|
- Melinda Hunt
- 5 years ago
- Views:
Transcription
1 Solar neutrinos: The Beginning at MPIK W. Hampel
2 : Geochemical Bromine-Krypton Experiment : Gallium Pilot experiment with 1.26 tons of Gallium : Transition phase from the pilot experiment to GALLEX
3 Geochemical Bromine Krypton Solar Neutrino Experiment Basic idea: Extract 81 Kr from about 10 tons of Bromine which has been produced over about 10 6 years in 10 tons of natural Bromine by solar 7 Be neutrinos log ft =? (4-6) threshold 490 kev Isotopic composition of Bromine: 79 Br 50.7% 81 Br 49.3%
4 Potassium salt deposits in Northern Germany Sylvite (KCl) Carnallite (KMgCl 3 *6 H 2 O) Kainite (KMg[Cl SO 4 ]*2.75 H 2 O) Langbeinite (K 2 Mg 2 (SO 4 ) 3 ) Kali- und Salz AG Mine at Bad Salzdetfurth (between Hannover and Kassel) Mining down to a depth of 900 m Daily output: ~ 5000 tons of potassium salt Bromine content 0,2% (corresponds to 10 tons of Br) Kassel Hannover Salzdetfurth Expected: about cc STP 81 Kr (for an assumed log ft value of 5) can in principle be measured by mass spectrometry)
5 Results (mainly from the PhD thesis K. Büchler 1980): Retention age for Krypton > 1 million years: ok We tried to measure the log ft value for the relevant transition: result >3.3 (expected 4-6) Muon-induced production at 900 m depth: about cc STP 81 Kr (same as solar-neutrino-produced 81 Kr) Mining not deep enough Dissolved stable Krypton in salt: 2x10-10 cc STP/g This leads to a ratio 81 Kr/ 82 Kr of not possible to be measured without isotopic separation Background by (α,p)(p,n) reactions through uranium and thorium: For a 10% bkg: 0.5 ppb U Measured 9 ppb in one case, mostly > 200 ppb much too high Kassel Hannover Salzdetfurth
6 Talk of T.Kirsten at the Informal Conference on Status and Future of Solar Neutrino Research (organized by Ray Davis and his collaborators in January 1978): Further consideration of the 81 Br- 81 Kr system At this time: it was clear that the Br-Kr experiment was not feasable with the potassium salt target of Salzdetfurth However: after the conference we were invited by R. Davis and his collaborators to discuss a possible participation in a Gallium solar neutrino experiment: this led to the Gallium Pilot experiment Collaboration
7 Visit of Ray Davis jr. at Heidelberg in 1978 Donald D. Clayton (Humboldt Research Awardee MPG) Oliver A. Schaeffer (External Scientific Member MPIK)
8 Thanks to an agreement between Raymond Davis and Till Kirsten: 1978/1979: Stay at the Chemistry Department, Brookhaven National Laboratory, Upton, New York, USA. Group of Raymond Davis Ge extraction from GaCl 3 solution Tritium-free GeCl 4 conversion to GeH 4 Counter construction and filling Raymond Davis jr. Physics Nobel Prize 2002 Data evaluation for the Chlorine experiment: Maximum Likelihood Method Monte Carlo Calculations Bruce T. Cleveland
9 March 1979 Meeting at BNL which led to the contract between BNL and MPIK to perform a pilot experiment with 1.26 tons of gallium
10 Pilot experiment with 1.26 tons of Gallium Collaboration Brookhaven National Laboratory, Upton, NY (Ga 2/3) Max-Planck-Institut für Kernphysik Heidelberg (Ga 1/3) Weizmann Institute Rehovot Institute for Advanced Studies Princeton University of Pennsylvania at Philadelphia
11 Four members of the pilot experiment collaboration Ray Davis jr. Israel Dostrovsky Keith Rowley John Bahcall (also GALLEX member) (also GALLEX member)
12 Pilot experiment installation in the basement of the Chemistry Department at Brookhaven National Laboratory 2.8 m 3 tank with Kynar and teflon lining 1.26 tons Gallium 4.65 tons of GaCl 3 solution
13 April 1980: Pilot tank is filled with 4.65 tons of GaCl 3 solution Very first Ge extraction from the pilot tank 99.6% of the germanium initially present in the GaCl 3 solution of the pilot tank (~200 mg) have been extracted in a 32-hour sweep
14 Low Level Proportional Counter Davis-type Similar to the counters used by Ray Davis in the Chlorine experiment Davis type Counter type used for counting GeH 4 samples from the pilot tank. Gerd Heusser has used this type of counter already a few years before the pilot experiment for the measurement of 37 Ar and 39 Ar in meteorite samples..
15 Run 7 of the pilot experiment Measurement of the 71 Ge production rate by cosmic rays in the pilot tank 110 ± Ge atoms /day (Shielding: a few meters of water equivalent) Here we used about 3 mg of Ge carrier this results in about 1 cm 3 of GeH 4 Counting gas is pure GeH 4 Non-linear energy scale
16 Outcome of the Pilot experiment: A full scale solar neutrino experiment with 30 tons of gallium is feasible!
17 After the end of the pilot experiment: Plans to perform a full scale experiment (share of gallium costs: ¾ BNL, ¼ MPIK) First step: perform a 51 Cr source experiment with 12.8 tons of gallium in the Asarco zinc mine in Tennessee (500m underground) Second step: full scale experiment with 50 tons of gallium in the Homestake mine BNL requested in several proposals to the Department of Energy and to the National Science Foundation to finance the US share of Gallium: they all failed BNL director: decided to stop working on the gallium experiment (January 1984) End of the pilot experiment collaboration
18 Reduction factor for 2ν vacuum maximal mixing as a function of m 2 for the chlorine and gallium solar neutrino detectors Vacuum neutrino oscillations: have in principle long been on the list of possible explanations for the low solar neutrino capture rate in the Cl experiment However: substantial reduction for the Cl signal needs very specific and rather low m 2 values (close to ev 2 )
19 The Mikheyev-Smirnov-Wolfenstein Effect 10th International Workshop on Weak Interactions (WIN 1985) June, 1985, Savonlinna, Finland Talk given by Alexei Smirnov (authors Stanislav Mikheyev and Alexei Smirnov) on a new effect concerning neutrino mixing in matter based on earlier work of Lincoln Wolfenstein (later called the Mikeyev-Smirnov-Wolfenstein effect) Bogdan Povh (former director of the MPIK) visited this conference. He recognized the importance of this work for the gallium experiment and reported this to us. This triggered extensive numerical calculations by the Saclay group and our group on the MSW effect, especially for the Gallium solar neutrino detector: J. Bouchez, M. Cribier, W. Hampel, J. Rich, M. Spiro and D. Vignaud: Matter effects for solar neutrino oscillations Z. Phys. C32, (1986). M. Cribier, W. Hampel, J. Rich and D. Vignaud: MSW Regeneration of Solar ν e in the Earth, Phys. Lett. B182, (1986).
20 Contour lines for possible gallium detector results as a function of the mixing angle Θ and the squared mass difference m 2 Final result: GALLEX/GNO: 69.3 ± 5.5 SNU WH 1986 Current Large mixing angle solution for 2ν mixing: { m 2 = 4.7 x 10-5 ev 2 sin 2 2Θ = 0.85
21 After the end of the Pilot Experiment Collaboration: Till Kirsten investigated the possibilities to perform the Gallium solar neutrino experiment in Europe. His efforts were successful in all aspects: The European GALLEX Collaboration was formed (1984) Funding for 30 tons of Gallium through the combined efforts of MPIK Heidelberg, Max Planck Society, Krupp Foundation and the German Federal Ministry of Research and Technology was assured (December 1985) The italian INFN assigned the required underground space in the newly constructed Laboratori Nazionali del Gran Sasso (1985)
22 Heidelberg Low Level Proportional Counter Development 1985: after the GALLEX collaboration was formed: tried to improve our low-level counters Intermediate step: HD-1 HD-1 Aluminum cathode evaporated onto the inside of the quartz body in order to minimize the dead volume. Stop cock close to the counting volume Final type: HD-2 (which was used in GALLEX) HD-2 First stage of the preamplifier close to the counting volume
23 1986: The Heidelberg GALLEX group with the counting shield still sitting in Heidelberg
24 First visit of the GALLEX Collaboration at the Laboratori Nazionali del Gran Sasso, April 1985 At this visit: (1) Hall B was already complete (2) excavation of hall A just had started (3) there was no hall C yet
25 Many thanks to Till Kirsten: Through his long-lasting efforts the GALLEX solar neutrino experiment became reality! this enabled many of us to take part in this fundamental and successful experiment of astrophysics!
26
Radiochemical solar neutrino experiments, successful and otherwise
Radiochemical solar neutrino experiments, successful and otherwise Richard L Hahn 1 Neutrinos/Nuclear-Chemistry Group, Chemistry Department, Brookhaven National Laboratory (BNL), Upton, NY 11973, USA E-mail:
D. VIGNAUD DAPNIA/SPP. CEA/Saclay Gif-sur-Yvette, France
FINAL RESULTS OF THE GALLEX SOLAR NEUTRINO EXPERIMENT D. VIGNAUD DAPNIA/SPP CEA/Saclay 91191 Gif-sur-Yvette, France For the GALLEX Collaboration The radiochemical GALLEX experiment is based on the reaction
The Solar Neutrino Problem. There are 6 major and 2 minor neutrino producing reactions in the sun. The major reactions are
The Solar Neutrino Problem There are 6 major and 2 minor neutrino producing reactions in the sun. The major reactions are 1 H + 1 H 2 H + e + + ν e (PP I) 7 Be + e 7 Li + ν e + γ (PP II) 8 B 8 Be + e +
arxiv: v1 [hep-ex] 22 Jan 2009
![arxiv: v1 [hep-ex] 22 Jan 2009](/thumbs/96/128991927.jpg "arxiv: v1 [hep-ex] 22 Jan 2009")
Solar neutrino detection Lino Miramonti Physics department of Milano University and INFN arxiv:0901.3443v1 [hep-ex] 22 Jan 2009 Abstract. More than 40 years ago, neutrinos where conceived as a way to test
Radiochemical Solar Neutrino Experiments, Successful and Otherwise
Radiochemical Solar Neutrino Experiments, Successful and Otherwise Richard L. (Dick) Hahn Solar-Neutrino & Nuclear-Chemistry Group * Chemistry Department, BNL Upton NY 11973 *Research sponsored by the
1. Neutrino Oscillations
Neutrino oscillations and masses 1. Neutrino oscillations 2. Atmospheric neutrinos 3. Solar neutrinos, MSW effect 4. Reactor neutrinos 5. Accelerator neutrinos 6. Neutrino masses, double beta decay 1.
GALLEX-GNO. GNO experiments: status and reports. Second International Summer Student School on Neutrino Physics in Memory of Bruno Pontecorvo
GALLEX-GNO GNO experiments: status and reports R. Bernabei Univ. Roma - Tor Vergata and INFN-Roma2 Second International Summer Student School on Neutrino Physics in Memory of Bruno Pontecorvo September
Neutrino oscillation experiments: Recent results and implications
Title transparency Neutrino oscillation experiments: Recent results and implications W. Hampel MPI Kernphysik Heidelberg Motivation for talk On the way from the Standard Model to String Theory: appropriate
Solar Neutrinos. Learning about the core of the Sun. Guest lecture: Dr. Jeffrey Morgenthaler Jan 26, 2006
Solar Neutrinos Learning about the core of the Sun Guest lecture: Dr. Jeffrey Morgenthaler Jan 26, 2006 Review Conventional solar telescopes Observe optical properties of the Sun to test standard model
Hydrogen Burning in More Massive Stars.
Hydrogen Burning in More Massive Stars http://apod.nasa.gov/apod/astropix.html 2 min For temperatures above 18 million K, the CNO cycle dominates energy production 10 min 14 CNO N CNO CYCLE (Shorthand)
arxiv: v1 [hep-ex] 15 Jan 2010
![arxiv: v1 [hep-ex] 15 Jan 2010](/thumbs/74/70372370.jpg "arxiv: v1 [hep-ex] 15 Jan 2010")
Reanalysis of the Gallex solar neutrino flux and source experiments F. Kaether, W. Hampel, G. Heusser, J. Kiko, T. Kirsten Max Planck Institute for Nuclear Physics, P.O. Box 1398, D-6929 Heidelberg, Germany
Solar Neutrinos & MSW Effect. Pouya Bakhti General Seminar Course Nov IPM
Solar Neutrinos & MSW Effect Pouya Bakhti General Seminar Course Nov. 2012 - IPM Outline Introduction Neutrino Oscillation Solar Neutrinos Solar Neutrino Experiments Conclusions Summary Introduction Introduction
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. Sakurai 1,3, H. J. Haubold and T. Shirai 1 1. Institute of Physics, Kanagawa University,
Study of Solar Neutrinos at Super Kamiokande
Study of Solar Neutrinos at Super Kamiokande Yusuke Koshio University of Tokyo April 1998 Abstract Super-Kamiokande started taking data on the 1st of April in 1996. The data used for the analysis of solar
Solar Neutrinos John N. Bahcall
SOLAR NEUTRINOS 1 Solar Neutrinos John N. Bahcall How does the Sun shine? How well do we understand the evolution and ages of stars? Does the neutrino have a mass? Can a neutrino change its lepton number
Hydrogen Burning in More Massive Stars and The Sun.
Hydrogen Burning in More Massive Stars and The Sun http://apod.nasa.gov/apod/astropix.html 2 min For temperatures above 18 million K, the CNO cycle dominates energy production 10 min CNO 14 N CNO CYCLE
14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009 BNO INR V.N. Gavrin. The Solar Neutrinos
14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009 BNO INR V.N. Gavrin The Solar Neutrinos 14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009
Neutrino Physics: an Introduction
Neutrino Physics: an Introduction Lecture 2: Neutrino mixing and oscillations Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research, Mumbai SERC EHEP School 2017 NISER Bhubaneswar,
PHYS 5326 Lecture #6. 1. Neutrino Oscillation Formalism 2. Neutrino Oscillation Measurements
PHYS 5326 Lecture #6 Wednesday, Feb. 14, 2007 Dr. 1. Neutrino Oscillation Formalism 2. Neutrino Oscillation Measurements 1. Solar Neutrinos 2. Atmospheric neutrinos 3. Accelerator Based Oscillation Experiments
SOLAR NEUTRINOS REVIEW Revised December 2007 by K. Nakamura (KEK, High Energy Accelerator Research Organization, Japan).
1 SOLAR NEUTRINOS REVIEW Revised December 2007 by K. Nakamura (KEK, High Energy Accelerator Research Organization, Japan). 1. Introduction The Sun is a main-sequence star at a stage of stable hydrogen
arxiv:hep-ph/ v1 16 May 1997
Solutions to the Solar Neutrino Anomaly Naoya Hata 1 and Paul Langacker 2 1 Institute for Advanced Study Princeton, NJ 08540 2 Department of Physics, University of Pennsylvania, Philadelphia, Pennsylvania
11 Neutrino astronomy. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
11 Neutrino astronomy introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 11.1 The standard solar model As we discussed in stellar evolution III, to obtain a reliable model for the sun, we
Solar spectrum. Nuclear burning in the sun produce Heat, Luminosity and Neutrinos. pp neutrinos < 0.4 MeV
SOLAR NEUTRINOS Solar spectrum Nuclear burning in the sun produce Heat, Luminosity and Neutrinos pp neutrinos < 0.4 MeV Beryllium neutrinos 0.86 MeV Monochromatic since 2 body decay 2 kev width due to
Solar Neutrino Oscillations
Solar Neutrino Oscillations ( m 2, θ 12 ) Background (aka where we were): Radiochemical experiments Kamiokande and Super-K Where we are: Recent results SNO and KamLAND Global picture Where we are going:
Status of Solar Neutrino Oscillations
Status of Solar Neutrino Oscillations With many thanks to Dave Wark - RAL/ University of Sussex and Stephen Brice - Fermilab The Solar Neutrino Problem Next three plots adapted from http://www.sns.ias.edu/~jnb/
Radio-chemical method
Neutrino Detectors Radio-chemical method Neutrino reactions: n+ν e => p+e - p+ν e => n+e + Radio chemical reaction in nuclei: A N Z+ν e => A-1 N(Z+1)+e - (Electron anti-neutrino, right) (Z+1) will be extracted,
4p 4 He + 2e + +2ν e. (1)
1 SOLAR NEUTRINOS Revised September 2001 by K. Nakamura (KEK, High Energy Accelerator Research Organization, Japan). 1. Introduction: The Sun is a main-sequence star at a stage of stable hydrogen burning.
LOW ENERGY SOLAR NEUTRINOS WITH BOREXINO. Lea Di Noto on behalf of the Borexino collaboration
LOW ENERGY SOLAR NEUTRINOS WITH BOREXINO Lea Di Noto on behalf of the Borexino collaboration Vulcano Workshop 20 th -26 th May 2018 [cm -2 s -1 MeV -1 ] SOLAR NEUTRINOS Electrons neutrinos are produced
Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University
Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University 1 Outline 2 Lecture 1: Experimental Neutrino Physics Neutrino Physics and Interactions Neutrino Mass Experiments Neutrino Sources/Beams and
Oklahoma State University. Solar Neutrinos and their Detection Techniques. S.A.Saad. Department of Physics
Oklahoma State University Solar Neutrinos and their Detection Techniques S.A.Saad Department of Physics Topics to be covered Solar Neutrinos Solar Neutrino Detection Techniques Solar Neutrino Puzzle and
Review of Solar Neutrinos. Alan Poon Institute for Nuclear and Particle Astrophysics & Nuclear Science Division Lawrence Berkeley National Laboratory
Review of Solar Neutrinos Alan Poon Institute for Nuclear and Particle Astrophysics & Nuclear Science Division Lawrence Berkeley National Laboratory Solar Neutrinos pp chain: 4p + 2e 4 He + 2ν e + 26.7
arxiv:hep-ex/ Jun 2000
GNO SOLAR NEUTRINO OBSERVATIONS: RESULTS FOR GNO I GNO COLLABORATION arxiv:hep-ex/0006034 29 Jun 2000 M. Altmann a, M. Balata b, P. Belli c, E. Bellotti d, R. Bernabei c, E. Burkert e, C. Cattadori d,
Two Neutrino Double Beta (2νββ) Decays into Excited States
Two Neutrino Double Beta (2νββ) Decays into Excited States International School of Subnuclear Physics 54 th Course: The new physics frontiers in the LHC-2 era Erice, 17/06/2016 Björn Lehnert TU-Dresden,
Cosmogenic background for the GERDA experiment. Luciano Pandola INFN, Laboratori del Gran Sasso, Italy
Cosmogenic background for the GERDA experiment Luciano Pandola INFN, Laboratori del Gran Sasso, Italy Cosmogenic Activity and Background Workshop, Berkeley April 15 th, 2011 GERDA experiment at LNGS The
Neutrino mixing II. Can ν e ν µ ν τ? If this happens:
Can ν e ν µ ν τ? If this happens: Neutrino mixing II neutrinos have mass (though there are some subtleties involving the MSW mechanism) physics beyond the (perturbative) Standard Model participates Outline:
ν?? Solar & Atmospheric Oscillation Experiments Greg Sullivan University of Maryland Aspen Winter Conference January 21, 1999 )Past )Present )Future
Solar & Atmospheric Oscillation Experiments Greg Sullivan of Maryland Aspen Winter Conference January 21, 1999 ν?? e )Past z Neutrino Mass Mass & Oscillations )Present z Atmospheric neutrinos z Solar Solar
THE BEGINNING OF THE END OF AN ERA: Analysis After the Shutdown of the Sudbury Neutrino Observatory
THE BEGINNING OF THE END OF AN ERA: Analysis After the Shutdown of the Sudbury Neutrino Observatory Introduction Highlights of SNO Results NCD Phase Update Future Analysis Plan Keith Rielage on behalf
- The CONUS Experiment - COherent elastic NeUtrino nucleus Scattering
- The CONUS Experiment - COherent elastic NeUtrino nucleus Scattering C. Buck, J. Hakenmüller, G. Heusser, M. Lindner, W. Maneschg, T. Rink, H. Strecker, T. Schierhuber and V. Wagner Max-Planck-Institut
XENONNT AND BEYOND. Hardy Simgen. WIN 2015 MPIK Heidelberg. Max-Planck-Institut für Kernphysik Heidelberg
XENONNT AND BEYOND Hardy Simgen Max-Planck-Institut für Kernphysik Heidelberg WIN 2015 MPIK Heidelberg THE XENON PROGRAM FOR DIRECT DARK MATTER SEARCH 1 THE PRESENT: XENON1T! LXe TPC under construction
Studies of the XENON100 Electromagnetic Background
Studies of the XENON100 Electromagnetic Background Daniel Mayani Physik-Institut University of Zurich PhD Seminar PSI, August 26-27, 2015 Searching for elusive particles The main challenge for experiments
A multipurpose detector for low energy
A multipurpose detector for low energy neutrino physics: Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München DPG Teilchenphysik Heidelberg, 09.03.07
Direct dark matter search using liquid noble gases
Direct dark matter search using liquid noble gases Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Physik Institut Universität Zürich Texas Symposium 2010, Heidelberg, 09.11.2010 Teresa Marrodán Undagoitia
Outline. The Sun s Uniqueness. The Sun among the Stars. Internal Structure. Evolution. Neutrinos
Lecture 2: The Sun as a Star Outline 1 The Sun s Uniqueness 2 The Sun among the Stars 3 Internal Structure 4 Evolution 5 Neutrinos What makes the Sun Unique? Some Answers Sun is the closest star Only star
The Problem of the Missing Neutrinos
The Problem of the Missing Neutrinos Kerstin Falk 20.10.2005 Project of the Space Physics Course 2005 Umeå University 1 Contents 1. Introduction 3 2. Solar model and solar neutrinos 3 3. The Solar Neutrino
Neutrinoless Double Beta Decay for Particle Physicists
Neutrinoless Double Beta Decay for Particle Physicists GK PhD Presentation Björn Lehnert Institut für Kern- und Teilchenphysik Berlin, 04/10/2011 About this talk Double beta decay: Particle physics implications
The Evolution of Neutrino Astronomy
The Evolution of Neutrino Astronomy John N. Bahcall Institute for Advanced Study, Olden Lane, Princeton, NJ 08540 and Raymond Davis, Jr. Department of Physics and Astronomy, University of Pennsylvania,
The GERmanium Detector Array
The GERmanium Detector Array n n ν=v p e - e - p Outline: Exp. issues of 0νββ-decay of 76 Ge Concept of GERDA Status of the experiment Summary and conclusions Kevin Kröninger (Max-Planck-Institut für Physik,
Discovery of the Neutrino Mass-I. P1X* Frontiers of Physics Lectures October 2004 Dr Paul Soler University of Glasgow
-I P1X* Frontiers of Physics Lectures 19-0 October 004 Dr Paul Soler University of Glasgow Outline 1. Introduction: the structure of matter. Neutrinos:.1 Neutrino interactions. Neutrino discovery and questions.3
Nuclear Astrophysics Underground Status & Future
Nuclear Astrophysics Underground Status & Future Frank Strieder South Dakota School of Mines & Technology XV International Symposium on Nuclei in the Cosmos Laboratori Nazionali del Gran Sasso, Assergi,
Does the Sun appear brighter at night in neutrinos?
PHYSICAL REVIEW C VOLUME 56, NUMBER 5 NOVEMBER 1997 Does the Sun appear brighter at night in neutrinos? J. N. Bahcall and P. I. Krastev School of Natural Sciences, Institute for Advanced Study, Princeton,
arxiv:astro-ph/ v1 14 Nov 2003
Astrophysical Neutrino Telescopes A. B. McDonald SNO Institute, Queen s University, Kingston, Canada K7L 3N6 C. Spiering DESY Zeuthen, Platanenallee 6, D-15738 Zeuthen, Germany S. Schönert Max-Planck-Institut
PLAN. Lecture I: Lecture II: Neutrino oscillations and the discovery of neutrino masses and mixings. Lecture III: The quest for leptonic CP violation
PLAN Lecture I: Neutrinos in the SM Neutrino masses and mixing: Majorana vs Dirac Lecture II: Neutrino oscillations and the discovery of neutrino masses and mixings Lecture III: The quest for leptonic
Hint of CPT Violation in Short-Baseline Electron Neutrino Disappearance
Journal of Physics: Conference Series 335 (011) 01054 doi:10.1088/174-6596/335/1/01054 Hint of CPT Violation in Short-Baseline Electron Neutrino Disappearance Carlo Giunti INFN, Sezione di Torino, and
The Search for Dark Matter with the XENON Experiment
The Search for Dark Matter with the XENON Experiment Elena Aprile Columbia University Paris TPC Workshop December 19, 2008 World Wide Dark Matter Searches Yangyang KIMS Homestake LUX SNOLAB DEAP/CLEAN
Neutrinos in Astrophysics and Cosmology
Crab Nebula Neutrinos in Astrophysics and Cosmology Introductory Remarks Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany Periodic System of Elementary Particles Quarks Charge -1/3 Charge
So, you want to build a neutrino detector?
Neutrino Detectors So, you want to build a neutrino detector? How many events do you need to do the physics? Determines detector mass Determines the target type What kind of interaction? e,, CC, NC? What
Purification of Liquid Scintillator and Monte Carlo Simulations of Relevant Internal Backgrounds in SNO+
Purification of Liquid Scintillator and Monte Carlo Simulations of Relevant Internal Backgrounds in SNO+ by Sarah Elizabeth Quirk A thesis submitted to the Department of Physics, Engineering Physics and
Neutrino Oscillations
Neutrino Oscillations Supervisor: Kai Schweda 5/18/2009 Johannes Stiller 1 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions
Results from Borexino 26th Rencontres de Blois
Results from Borexino 26th Rencontres de Blois - 2014 Marco G. Giammarchi Istituto Nazionale di Fisica Nucleare Via Celoria 16 20133 Milano (Italy) marco.giammarchi@mi.infn.it http://pcgiammarchi.mi.infn.it/giammarchi/
Dark matter search with the SABRE experiment
Dark matter search with the SABRE experiment Giulia D Imperio* for the SABRE collaboration *INFN Roma 1 25-07-2017 TAUP 2017 Sudbury, Canada 1 Dark matter detection through annual modulation WIMP is one
Solar Neutrinos: Status and Prospects. Marianne Göger-Neff
Solar Neutrinos: Status and Prospects Marianne Göger-Neff NIC 2014, Debrecen TU München Solar Neutrinos Objective of the first solar neutrino experiment: to see into the interior of a star and thus verify
Metallicities in stars - what solar neutrinos can do
- what solar neutrinos can do Institute for Nuclear and Particle Physics, Technical University Dresden, 01069 Dresden, Germany E-mail: zuber@physik.tu-dresden.de New elemental abundance determinations
The SOX experiment. Stefano Davini (on behalf of the Borexino-SOX collaboration) Brussels, December 1 st 2017
The SOX experiment Stefano Davini (on behalf of the Borexino-SOX collaboration) Brussels, December 1 st 2017 Beyond the Standard model with Neutrinos Neutrino masses call for physics beyond Standard model
Where do we stand with solar neutrino oscillations?
PHYSICAL REVIEW D, VOLUME 58, 096016 Where do we stand with solar neutrino oscillations? J. N. Bahcall School of Natural Sciences, Institute for Advanced Study, Princeton, New Jersey 08540 P. I. Krastev
Direct Dark Matter and Axion Detection with CUORE
Direct Dark Matter and Axion Detection with CUORE Europhysics Conference on High-Energy Physics 2011 Cecilia G. Maiano on behalf of CUORE collaboration Contents The Bolometric Technique The CUORE experiment
Raymond Davis Jr. A Biographical Memoir by Kenneth Lande
Raymond Davis Jr. 1914 2006 A Biographical Memoir by Kenneth Lande 2018 National Academy of Sciences. Any opinions expressed in this memoir are those of the author and do not necessarily reflect the views
David Reyna Belkis Cabrera-Palmer AAP2010, Japan
David Reyna Belkis Cabrera-Palmer AAP2010, Japan Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy s National Nuclear
ICARUS T600 experiment: latest results and perspectives
ICARUS T600 experiment: latest results and perspectives Marta Torti University of Pavia, INFN Pavia NBIA Ph.D School: Neutrinos underground & in the heavens ICARUS T600 at LNGS The ICARUS T600 detector
192 days of Borexino. Neutrino 2008 Christchurch, New Zeland May 26, Cristiano Galbiati on behalf of Borexino Collaboration
192 days of Borexino Neutrino 2008 Christchurch, New Zeland May 26, 2008 Cristiano Galbiati on behalf of Borexino Collaboration 2 Solar Neutrinos Spectrum 3 Solar Neutrinos Spectrum SNO, SuperK 3 Solar
Status of Cuore experiment and last results from Cuoricino
Status of Cuore experiment and last results from Cuoricino on behalf of the Cuore collaboration Istituto Nazionale di Fisica Nucleare, Genova E-mail: elena.guardincerri@ge.infn.it CUORE is a cryogenic-bolometer
Rn/ 226 Ra as a Background Source in the Solar Neutrino Experiments GALLEX and BOREXINO
Rn/ 226 Ra as a Background Source in the Solar Neutrino Experiments GALLEX and BOREXINO M. Wójcik, G. Zuzel Institute of Physics, Jagiellonian University 7 th of June 2017, MPI Heidelberg From Cosmochemistry
GERDA experiment A search for neutrinoless double beta decay. Roberto Santorelli (Physik-Institut der Universität Zürich)
GERDA experiment A search for neutrinoless double beta decay Roberto Santorelli (Physik-Institut der Universität Zürich) on behalf of the GERDA collaboration ÖPG/SPS/ÖGAA meeting 04/09/09 Neutrinos mixing
Solar Neutrinos and the Borexino experiment
Journal of Physics: Conference Series OPEN ACCESS Solar Neutrinos and the Borexino experiment To cite this article: D Vignaud 2015 J. Phys.: Conf. Ser. 593 012007 View the article online for updates and
Neutrino nucleus coherent scattering - Prospects of future reactor experiments with germanium detectors
Neutrino nucleus coherent scattering - Prospects of future reactor experiments with germanium detectors Marco Salathe 1, Thomas Rink 2 8 December 2015 Applied Antineutrino Physics - Virginia Tech 1 marco.salathe@mpi-hd.mpg.de,
DIANA A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY
DIANA D. Leitner for the DIANA collaboration Michigan State University PAC 2011 New York, April 2011 A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY Outline of the Talk Why underground? Brief science
Double Beta Present Activities in Europe
APPEAL Workshop 19-21 February 2007, Japan Double Beta Present Activities in Europe Xavier Sarazin Laboratoire de l Accélérateur Linéaire Orsay France Germanium detector Bolometers CdZnTe semiconductors
arxiv: v1 [physics.ins-det] 22 Dec 2016
![arxiv: v1 [physics.ins-det] 22 Dec 2016](/thumbs/83/87421236.jpg "arxiv: v1 [physics.ins-det] 22 Dec 2016")
Results from the DM-Ice17 Dark Matter Experiment at the South Pole arxiv:161.0746v1 [physics.ins-det] Dec 016, on behalf of the DM-Ice Collaboration Department of Physics and Wright Laboratory, Yale University
A HALF-CENTURY WITH SOLAR NEUTRINOS
A HALF-CENTURY WITH SOLAR NEUTRINOS Nobel Lecture, December 8, 2002 by RAYMOND DAVIS, JR. Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 and Chemistry Department,
SOLAR NEUTRINO EXPERIMENTS: NEW PHYSICS? JOHN N. BAHCALL ABSTRACT. 1. New Physics is Required if Solar Neutrino Experiments are Correct.
SOLAR NEUTRINO EXPERIMENTS: NEW PHYSICS? JOHN N. BAHCALL Institute for Advanced Study, Princeton, New Jersey 08540, USA ABSTRACT Physics beyond the simplest version of the standard electroweak model is
Neutrino Oscillations
1. Introduction 2. Status and Prospects A. Solar Neutrinos B. Atmospheric Neutrinos C. LSND Experiment D. High-Mass Neutrinos 3. Conclusions Plenary talk given at DPF 99 UCLA, January 9, 1999 Introduction
Interactions/Weak Force/Leptons
Interactions/Weak Force/Leptons Quantum Picture of Interactions Yukawa Theory Boson Propagator Feynman Diagrams Electromagnetic Interactions Renormalization and Gauge Invariance Weak and Electroweak Interactions
Neutrino Sources in the Universe
Crab Nebula Neutrino Sources in the Universe Georg G. Raffelt Max-Planck-Institut für Physik, München Where do Neutrinos Appear in Nature? Nuclear Reactors Sun Particle Accelerators Supernovae (Stellar
KamLAND Data and the Solution to the Solar Neutrino Problem
1416 Brazilian Journal of Physics, vol. 34, no. 4A, December, 004 KamLAND Data and the Solution to the Solar Neutrino Problem P. C. de Holanda 1 and A. Yu. Smirnov,3 1 Instituto de Física Gleb Wataghin
UNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos
UNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos Stefania Ricciardi HEP PostGraduate Lectures 2016 University of London 1 Neutrino Sources Artificial: nuclear reactors
Search for 0νββ-decay with GERDA Phase II
Search for 0νββ-decay with GERDA Phase II (MPI für Physik) for the collaboration GERDA OUTLINE: Phase I background results Phase II data taking Phase II background \wo cuts LAr veto and PSD cuts 0νββ result
Neutrino Experiments with Reactors
Neutrino Experiments with Reactors 1 Ed Blucher, Chicago Lecture 2 Reactors as antineutrino sources Antineutrino detection Reines-Cowan experiment Oscillation Experiments Solar Δm 2 (KAMLAND) Atmospheric
Results from 730 kg days of the CRESST-II Dark Matter Search
Results from 730 kg days of the CRESST-II Dark Matter Search Federica Petricca on behalf of the CRESST collaboration: Max-Planck-Institut für Physik, München TU München University of Oxford Universität
Analysis of Neutrino Oscillation experiments
Analysis of Neutrino Oscillation experiments Mario Andrés Acero Ortega Università degli Studi di Torino, LAPTH - Université de Savoie Second Year - Seminar Torino, Italy January 15th, 2008 Tutor: Carlo
SOLAR NEUTRINO PROBLEM SOLVED
Fakulteta za matematiko in fiziko Oddelek za fiziko Jadranska 19 1000 Ljubljana UROŠ BOROVŠAK SOLAR NEUTRINO PROBLEM SOLVED ADVISOR dr. TOMAŽ PODOBNIK Ljubljana, April 2, 2003 Abstract Since the end of
hep-ph/ Oct 1994
A Model Independent Analysis of Solar Neutrino Data DFTT 32/94 S.M. Bilenky Joint Institute of Nuclear Research, Dubna, Russia INFN Torino, Via P. Giuria 1, 10125 Torino, Italy Dipartimento di Fisica Teorica,
Deep underground Neutron Flux Measurement with Large BF3 Counters (*).
IL NUOVO CIMENTO VOL. 101 A, N. 6 Giugno 1989 Deep underground Neutron Flux Measurement with Large BF3 Counters (*). P. BELLI, R. BERNABEI, S. D'ANGELO, M. P. DE PASCALE L. PAOLUZI and R. SANTONICO Dipartimento
LARGE UNDERGROUND XENON
LARGE UNDERGROUND XENON Cláudio Silva (LIP Coimbra) On behalf of the LUX Collaboration IDPASC Dark Matter Workshop 17 December 2011 1 THE LUX COLLABORATION Collaboration was formed in 2007 and fully funded
arxiv: v1 [nucl-ex] 20 Dec 2008
![arxiv: v1 [nucl-ex] 20 Dec 2008](/thumbs/90/102022457.jpg "arxiv: v1 [nucl-ex] 20 Dec 2008")
Operation of a GERDA Phase I prototype detector in liquid argon and nitrogen M. Barnabé Heider a, A. Bakalyarov b, L. Bezrukov c, C. Cattadori d, O. Chkvorets a, K. Gusev b,e, M. Hult f, I. Kirpichnikov
Search for sterile neutrino mixing in the muon neutrino to tau neutrino appearance channel with the OPERA detector
Search for sterile neutrino mixing in the muon neutrino to tau neutrino appearance channel with the OPERA detector INFN - Sezione di Bologna, I-4017 Bologna, Italy E-mail: matteo.tenti@bo.infn.it The OPERA
GERDA: The GERmanium Detector Array for the search for neutrinoless decays of 76 Ge. Allen Caldwell Max-Planck-Institut für Physik
GERDA: The GERmanium Detector Array for the search for neutrinoless decays of 76 Ge Allen Caldwell Max-Planck-Institut für Physik What we know Mass Scale NORMAL INVERTED m 12 2 known m 13 2 known Mixing
The next generation dark matter hunter: XENON1T status and perspective
The next generation dark matter hunter: XENON1T status and perspective A. Rizzo a on behalf of the XENON Collaboration Department of Astrophysics, Columbia University in the City of New York, USA Abstract.
Neutrino Oscillation Measurements, Past and Present. Art McDonald Queen s University And SNOLAB
Neutrino Oscillation Measurements, Past and Present Art McDonald Queen s University And SNOLAB Early Neutrino Oscillation History -1940 s to 1960 s: - Neutrino oscillations were proposed by Pontecorvo
SOLAR NEUTRINO EXPERIMENTS: STATUS AND PROSPECTS M. C. Chen
ˆ ˆŠ Œ ˆ ˆ Œ ƒ Ÿ 2011.. 42.. 4 SOLAR NEUTRINO EXPERIMENTS: STATUS AND PROSPECTS M. C. Chen Department of Physics, Queen's University, Kingston, Ontario, Canada NEUTRINOS FROM THE SUN 1087 CHLORINE EXPERIMENT
arxiv:hep-ph/ v2 8 Sep 2000
July 2000 Revised September 2000 Is the ν µ ν s oscillation solution to the atmospheric neutrino anomaly excluded by the superkamiokande data? arxiv:hep-ph/0007065v2 8 Sep 2000 R. Foot School of Physics
Astrophysical Nucleosynthesis
R. D. Gehrz ASTRO 2001, Fall Semester 2018 1 RDG The Chemical Evolution of the Universe 2RDG 1 The Stellar Evolution Cycle 3 RDG a v a v X X V = v a + v X 4 RDG reaction rate r n n s cm ax a X r r ( E)