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Neutrinos and Dark Matter in Nuclear Physics 2015

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Neutrinos and Dark Matter in Nuclear Physics 2015 Neutrinos and Dark Matter in Nuclear Physics 2015 June 1–5, 2015, Jyväskylä, Finland Organizers Jouni Suhonen (Chair) Dieter Frekers (Münster) (Co-chair) Jukka Maalampi Wladyslaw Trzaska Markus Kortelainen Jenni Kotila Kai Loo International advisary committee Frank Avignone (South Carolina) Baha Balantekin (Wisconsin) Alexander Barabash (ITEP, Moscow) Rita Bernabei (INFN, Rome) Osvaldo Civitarese (La Plata) Hiro Ejiri (Osaka) Ettore Fiorini (Milano-Bicocca) Aksel Hallin (Alberta) Wick Haxton (Seattle) Toshitaka Kajino (Tokyo) Sun Kee Kim (Seoul) Karlhainz Langanke (GSI, Darmstadt) Manfred Lindner (MPI, Heidelberg) Yuri N. Novikov (St.Petersburg) Serguey Petcov (SISSA) Andre Rubbia (ETH, Zürich) Yoichiro Suzuki (Tokyo) John D. Vergados (Ioannina) Petr Vogel (Caltech) Alexei Yu. Smirnov (ICTP, Trieste) 1 Program layout Time Sun May 31 Mon June 1 Tue June 2 Wed June 3 Thu June 4 Fri June 5 OPENING 8 : 30 − 11 : 00 NEMF NNA DBD DM SSO Photo CLOSING 11 : 00 − 11 : 30 B R E AK (20 min) LUNCH SSO NEMF DM NEMF 11 : 30 − 13 : 00 DM DBD SSO DBD 13 : 00 − 14 : 30 L U N CH DBD DBD DBD 14 : 30 − 16 : 00 NNA DM NNA SSO 15:30 16 : 00 − 16 : 30 BREAK SSO BREAK DM NNA Boat cruise 16 : 30 − 19 : 00 NEMF DBD and Banquet Welcome Informal Reception Informal at 19 : 00− Reception Nanosauna at the Nanosauna Savutuvan 19:00 - 22:00 Seminar City Hall Seminar Apaja Hotel Alba Session 18:00 - 21:00 Session 16:15 - 23:00 NNA = Neutrinos in Nucleosynthesis and Astrophysics DM = Dark Matter DBD = Double Beta Decay SSO = Supernova and Solar neutrinos, neutrino Oscillations NEMF = Neutrino Experiments, Methods and Facilities 2 Talks 3 STATUS OF THE RED EXPERIMENT D.Yu. Akimova,b, V.A. Belova,b, A.I. Bolozdynyab, A.A. Burenkova,b, Yu.V. Efre- menkoc,b, Yu.V. Gusakovd,b, A.V. Etenkoe,b, V.A. Kaplinb, A.V. Khromovb, A.M. Kono- valova,b, A.G. Kovalenkoa,b, A.V. Kumpanb, T.D. Krakhmalovab, Yu.A. Melikyanb, P.P. Naumovb, D.G. Rudika,b, R.R. Shafigullinb, A.V. Shakirovb, G.E. Simakova,b, V.V. Sos- novtsevb, V.N. Stekhanova,b A.A. Tobolkinb, I.A. Tolstukhinb a SSC RF ITEP of NRC “Kurchatov Institute”, Moscow, Russian Federation b NRNU MEPhI (Moscow Engineering Physics Institute), Moscow, Russian Federation c University of Tennessee, Knoxville, USA d JINR, Dubna, Russian Federation e NRC “Kurchatov Institute”, Moscow, Russian Federation e-mail: [email protected] The RED-100 (Russian Emission Detector) is being constructed for the experiment on the first observation of neutrino elastic coherent scattering off atomic nuclei [1]. This fundamental process was predicted several decades ago by the Standard Model of elec- troweak interactions but has not been discovered yet. The RED-100 is an emission two-phase xenon detector containing ~200 kg of the liquid Xe (~ 100 kg in a fiducial volume). One of the possible sites to carry out the experiment is SNS (Spallation Neutron Source) facility of Oak Ridge National Laboratory, USA. The energy spectrum of neutrinos produced at the SNS source extends up to ~ 50 MeV that gives kinetic energies of Xe recoils of up to a few tens of keV. For these energies of Xe recoils the response of the LXe is well known from neutron calibrations of dark mat- ter detectors. Possible detector locations at the SNS are under consideration now. One of them is in a basement under the experimental hall at a distance of ~30 meters from the SNS target. The expected signal and background (neutron and gamma) are estimated for this specific location of the detector. The detector details and the current status are given. [1] D.Yu. Akimov, I.S. Alexandrov, V.I. Aleshin et al., JINST 8 (2013) P10023, arXiv:1212.1938[physics.ins-det]. 4 Heavy element nucleosynthesis in core-collapse supernovae and neutron star mergers A. Arcones TU Darmstadt and GSI email: [email protected] Core-collapse supernovae and neutrino-driven winds can produce elements up to silver. Because the synthesis of these elements occurs closer to stability, in the near future, the nuclear physics uncertainties will be reduced by experiments. This will uniquely allow us to combine observations and nucleosynthesis calculations to constrain the astrophys- ical conditions in neutrino-driven winds [1] and thus gain new insights about core- collapse supernovae. In addition, all r-process elements are synthesized in neutron star mergers. Different ways of ejecting matter lead to variations of the nucleosynthesis: the early dynamic ejecta is very neutron rich and produce the heaviest elements, while in the post-merger neutrino-driven wind elements below the second r-process peak are synthesized [2]. The radioactive decay of neutron-rich nuclei triggers an electromagnet- ic signal in mergers known as kilonova or macronova. This was potentially observed after a short gamma ray burst, associated with a neutron star merger. The composition and distribution of the different ejecta is critical to understand such kilonova light curve. [1] C. Hansen, F. Montes, and A. Arcones, ApJ 797, 123 (2014). [2] D. Martin et al., in prep. 5 NEUTRINO PROPERTIES, COLLECTIVE NEUTRINO OSCILLATIONS, AND R-PROCESS NUCLEOSYNTHESIS A. B. Balantekin Department of Physics, University of Wisconsin-Madison, Madison, Wisconsin 53706 USA email: [email protected] For a long time very little experimental information was available about neutrino prop- erties, even though even a small neutrino mass has intriguing cosmological and astro- physical implications. This situation has changed in the recent years. In this talk recent experimental and theoretical developments in solar, atmospheric, and reactor neutrino physics will be briefly reviewed. Implications of those experiments for astronomy and astrophysics will be discussed. The role of neutrinos in the dynamics of core-collapse supernovae will be elucidated. In addition, neutrinos form the intellectual bridge between many astrophysical phenom- ena and laboratory nuclear physics, investigating stable as well as unstable, exotic, and rare elements. Exploiting this connection in an intellectually beneficial way necessitates a multitude of experimental and theoretical efforts. One topic where the connection be- tween rare isotope physics and neutrino physics is manifest is the nucleosynthesis of various elements. In this talk the connection between neutrinos and the various nucle- oynthesis scenarios will be explored. In particular, neutrino collective oscillations, their symmetries, and their impact on possible supernova r-process nucleosynthesis will be discussed. 6 REVIEW OF MODERN DOUBLE BETA DECAY EXPERIMENTS A.S Barabash Institute of Theoretical and Experimental Physics, Russia email: [email protected] The review of modern experiments on search and studying of double beta decay pro- cesses is done. Results of the most sensitive current experiments are discussed. The main attention is paid to EXO-200, KamLAND-Zen, GERDA-I and CUORE0 experi- ments. Modern values of T1/2(2ν) and best present limits on neutrinoless double beta de- cay and double beta decay with Majoron emission are presented. Conservative limits on effective mass of a Majorana neutrino (<mν> < 0.34 eV) and a coupling constant of Ma- -5 joron to neutrino (<gee> < 10 ) are obtained. In the second part of the review prospects of search for neutrinoless double beta decay in new experiments with sensitivity to <mν> at the level of ~ 0.01-0.1 eV are discussed. The main attention is paid to experiments of CUORE, GERDA, MAJORANA, EXO, KamLAND-Zen-2, SuperNEMO and SNO+. Possibilities of low-temperature scintillat- ing bolometers on the basis of inorganic crystals (ZnSe, ZnMoO4, Li2MoO4, CdWO4, CaMoO4) are considered too. 7 DOUBLE BETA DECAY MATRIX ELEMENTS IN THE IBM-2 WITH ISOSPIN RESTORATION J. Barea1, J. Kotila2,3 and F. Iachello2 1Departamento de Física, Universidad de Concepción, Casilla 160-C, Concepción 4070386, Chile. 2Center for Theoretical Physics, Sloane Physics Laboratory, Yale University, New Haven, Connecticut 06520-8120, USA. 3University of Jyvaskyla, Department of Physics, B.O. Box 35, FI-40014, University of Jyvaskyla, Finland. The halflives for double beta decays can be written as a product of several terms where one is the socalled nuclear matrix element, which takes into account the nuclear structure of the states involved in the decay. So far these quantities have been calculated in the microscopic Interacting Boson Model (IBM-2) using a transition operator which violates the isospin selection rule of the Fermi matrix element for the two neutrinos double beta decay. Very recently we published a work [1] where we introduce a method to solve this issue. We will discuss this method and show the new values for the matrix elements obtained by using it. In general, the new values reduced and the Fermi matrix elements for the two neutrinos double beta decay decay become zero. [1] J. Barea, J. Kotila and F. Iachello Phys. Rev. C 91, 034304 (2015). 8 RESULTS AND STRATEGIES FOR DARK MATTER INVESTIGATIONS P. Belli Dip. di Fisica, Università di Roma “Tor Vergata”, I-00133 Rome, Italy and I.N.F.N., sez. Roma “Tor Vergata”, I-00133 Rome, Italy An overview of the latest results of Dark Matter direct detection will be discussed, with particular care to the DAMA/LIBRA-phase1 results and the 9.3 σ C.L. evidence obtained by exploiting the model-independent Dark Matter annual modulation signature for the presence of Dark Matter particles in the galactic halo. Comparisons, implications and experimental perspectives will be addressed. 9 CUORE-0 experiment: first physics results. M. Biassoni for the CUORE Collaboration University of Milano-Bicocca and INFN - Sezione di Milano-Bicocca email: [email protected] CUORE (Cryogenic Underground Observatory for Rare Events) is a ton-scale experiment for the search for neutrinoless double beta decay in 130Te with tellurium oxide bolome- ters. It’s projected sensitivity touches the inverted mass hierarchy region, and it is cur- rently at final stage of construction at the Gran Sasso National Laboratory (LNGS, Italy).
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