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1. Atmospheric transport and chemistry of trace gases in LMDz5B: evaluation and implications for inverse modelling

Author

Anne Cozic, Philippe Bousquet, S. van der Laan, C. Schlosser, Alex Vermeulen, John Moncrieff, Fleur Couvreux, Robin Locatelli, Ute Karstens, Alastair G. Williams, Frédéric Hourdin, Peter Bergamaschi, Martina Schmidt, M. P. Lefebvre, Michel Ramonet, J. Y. Grandpeix, V. Kazan, Scott D. Chambers, H. A. Scheeren, Harro A. J. Meijer, Marielle Saunois, Catherine Rio, STMicroelectronics, ESIM - Déterminants Sociaux de la Santé et du Recours aux Soins ( DS3 ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] ( LSCE ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Groupe d'étude de l'atmosphère météorologique ( CNRM-GAME ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Météo France-Centre National de la Recherche Scientifique ( CNRS ), ONERA - The French Aerospace Lab ( Chatillon ), ONERA, JRC Institute for Environment and Sustainability ( IES ), European Commission - Joint Research Centre [Ispra] ( JRC ), Max-Planck-Institut für Biogeochemie ( MPI-BGC ), Centre National de la Recherche Scientifique ( CNRS ), Institut de génétique humaine ( IGH ), Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), School of Geosciences [Edinburgh], University of Edinburgh, Leibniz Institut für Meereswissenschaften, IFM-GEOMAR, Kiel, Germany ( IfM-GEOMAR ), Leibniz-Institut für Meereswissenschaften ( IFM-GEOMAR ), Service des Photons, Atomes et Molécules ( SPAM ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Cranfield University, Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Modélisation INVerse pour les mesures atmosphériques et SATellitaires (SATINV), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Calcul Scientifique (CALCULS), Centre national de recherches météorologiques (CNRM), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), JRC Institute for Environment and Sustainability (IES), European Commission - Joint Research Centre [Ispra] (JRC), Max-Planck-Institut für Biogeochemie (MPI-BGC), ICOS-RAMCES (ICOS-RAMCES), Institut de génétique humaine (IGH), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Bundesamt für Strahlenschutz - Federal Office for Radiation Protection (BfS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Groupe d'étude de l'atmosphère météorologique (CNRM-GAME), Institut national des sciences de l'Univers (INSU - CNRS)-Météo France-Centre National de la Recherche Scientifique (CNRS), Federal Office for Radiation Protection (BfS), and Isotope Research

Subjects
[ SDU.OCEAN ] Sciences of the Universe [physics]/Ocean, Atmosphere, Meteorology, 010504 meteorology & atmospheric sciences, Planetary boundary layer, Mesoscale meteorology, SURFACE MEASUREMENTS, Atmospheric sciences, 010502 geochemistry & geophysics, Convective Boundary Layer, 01 natural sciences, 7. Clean energy, CUMULUS CONVECTION, Troposphere, CARBON-DIOXIDE, Diurnal cycle, LARGE-SCALE MODELS, METHANE EMISSIONS, [ SDU.ENVI ] Sciences of the Universe [physics]/Continental interfaces, environment, GENERAL-CIRCULATION MODEL, CABAUW TALL TOWER, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, Stratosphere, Physics::Atmospheric and Oceanic Physics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, LARGE-EDDY SIMULATION, Chemistry, VERTICAL PROFILES, lcsh:QE1-996.5, Trace gas, lcsh:Geology, CONVECTIVE BOUNDARY-LAYER, 13. Climate action, Greenhouse gas
Abstract

Representation of atmospheric transport is a major source of error in the estimation of greenhouse gas sources and sinks by inverse modelling. Here we assess the impact on trace gas mole fractions of the new physical parameterizations recently implemented in the atmospheric global climate model LMDz to improve vertical diffusion, mesoscale mixing by thermal plumes in the planetary boundary layer (PBL), and deep convection in the troposphere. At the same time, the horizontal and vertical resolution of the model used in the inverse system has been increased. The aim of this paper is to evaluate the impact of these developments on the representation of trace gas transport and chemistry, and to anticipate the implications for inversions of greenhouse gas emissions using such an updated model. Comparison of a one-dimensional version of LMDz with large eddy simulations shows that the thermal scheme simulates shallow convective tracer transport in the PBL over land very efficiently, and much better than previous versions of the model. This result is confirmed in three-dimensional simulations, by a much improved reproduction of the radon-222 diurnal cycle. However, the enhanced dynamics of tracer concentrations induces a stronger sensitivity of the new LMDz configuration to external meteorological forcings. At larger scales, the inter-hemispheric exchange is slightly slower when using the new version of the model, bringing them closer to observations. The increase in the vertical resolution (from 19 to 39 layers) significantly improves the representation of stratosphere/troposphere exchange. Furthermore, changes in atmospheric thermodynamic variables, such as temperature, due to changes in the PBL mixing modify chemical reaction rates, which perturb chemical equilibriums of reactive trace gases. One implication of LMDz model developments for future inversions of greenhouse gas emissions is the ability of the updated system to assimilate a larger amount of highfrequency data sampled at high-variability stations. Others implications are discussed at the end of the paper., JRC.H.2-Air and Climate

Published
2015
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2. Update of GALLEX solar neutrino results and implications

Author

P. Anselmann, W. Hampel, G. Heusser, J. Kiko, T. Kirsten, M. Laubenstein, E. Pernicka, S. Pezzoni, U. Rönn, M. Sann, C. Schlosser, R. Wink, M. Wójcik, R. von Ammon, K.H. Ebert, T. Fritsch, K. Hellriegel, E. Henrich, L. Stieglitz, F. Weirich, M. Balata, N. Ferrari, H. Lalla, E. Bellotti, C. Cattadori, O. Cremonesi, E. Fiorini, L. Zanotti, M. Altmann, F. von Feilitzsch, R. Möβbauer, U. Schanda, G. Berthomieu, E. Schatzman, I. Carmi, I. Dostrovsky, C. Bacci, P. Belli, R. Bernabei, S. d'Angelo, L. Paoluzi, A. Bevilacqua, S. Charbit, M. Cribier, L. Gosset, J. Rich, M. Spiro, T. Stolarczyk, C. Tao, D. Vignaud, R.L. Hahn, F.X. Hartmann, J.K. Rowley, R.W. Stoenner, J. Weneser, Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Solar neutrino, Settore FIS/01 - Fisica Sperimentale, Solar luminosity, Solar physics, 01 natural sciences, 7. Clean energy, Atomic and Molecular Physics, and Optics, Settore FIS/04 - Fisica Nucleare e Subnucleare, Nuclear physics, Deuterium, solar neutrinos, 0103 physical sciences, Nuclear fusion, Neutrino, GALLEX, 010306 general physics, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, Energy (signal processing), ComputingMilieux_MISCELLANEOUS
Abstract

The galliumchloride detector operated by the GALLEX-collaboration in the Gran Sasso Underground Laboratory responds primarily to pp-neutrinos. They are produced in the primary fusion reaction of hydrogen into deuterium and directly coupled to the solar luminosity. Standard Solar Models predict ca. 58% of the total signal expected in GALLEX (123-132 SNU) to be due to pp-neutrinos. The relative pp-neutrino dominance becomes even larger if the deficit of higher energy neutrinos (as observed in the Homestake- and Kamiokande experiments) is considered. During the first data taking period, 15 solar runs had been performed within the exposure period 14.5.1991 - 29.4.1992. The result, 81 {+-} 17 {+-} 9 SNU provided the first experimental evidence for pp-neutrinos from the Sun. At the same time, it confirmed the depression of higher energy neutrino fluxes relative to the model predictions. Here the authors report the results of 15 more solar neutrino runs, covering the period 19.8.92 - 13.10.93. They obtain 78 {+-} 13 {+-} 5 SNU. Evaluated together, the result for all 30 runs is 79 {+-} 10 {+-} 6 SNU. While the SNU rate of GALLEX I is well reproduced the statistical error has been reduced so substantially that a value of signal +2{sigma}more » is required to accommodate not only pp-and pep- but also the {sup 7}Be-neutrino induced {sup 71}Ge-production. Contrary, the fate of {sup 8}B-neutrinos has only little discernible effect on the GALLEX data. In conclusion, with the present errors GALLEX constitutes a 2.5 {sigma} problem for {sup 7}Be neutrinos within the frame of {open_quotes}astrophysical{close_quotes} solutions. Alternatively, the particle physics solution (MSW-effect) can consistently explain all available solar neutrino results, leading to a most probable mass scale with the muon-neutrino at approximately 3 meV (milli-eV). However, since the GALLEX result allows the presence of pp and pep neutrinos at full strength. the latter explanation of the data is not forced.« less

Published
1995
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3. GALLEX solar neutrino observations. The results from GALLEX I and early results from GALLEX II

Author

L. Paoluzi, Charling Tao, Matthias Laubenstein, R. Möβbauer, M. Sann, Ettore Fiorini, Ernst Pernicka, U. Rönn, F.v. Feilitzsch, M. Wojcik, M. Cribier, Michel Spiro, C. Bacci, T. Fritsch, S. Pezzoni, C. Cattadori, F. Weyrich, C. Schlosser, N. Ferrari, Oliviero Cremonesi, M. Balata, R. Plaga, I. Dostrovsky, H. Lalla, P. Anselmann, J. Weneser, J. Rich, T. Kirsten, P. Belli, R.W. Stoenner, L. Stieglitz, I. Carmi, R. Wink, K.H. Ebert, K. Hellriegel, L. Gosset, D. Vignaud, R.L. Hahn, J.K. Rowley, U. Schanda, E. Schatzman, L. Zanotti, M. Altmann, S. d'Angelo, J. Kiko, R. Bernabei, E. Henrich, E. Bellotti, R.v. Ammon, W. Hampel, G. Heusser, G. Berthomieu, T. Stolarczyk, F.X. Hartmann, S. Charbit, G. Dupont, Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Nuclear and High Energy Physics, 010308 nuclear & particles physics, Solar neutrino, Settore FIS/01 - Fisica Sperimentale, 01 natural sciences, Settore FIS/04 - Fisica Nucleare e Subnucleare, Nuclear physics, Early results, 0103 physical sciences, GALLEX, Neutrino, 010306 general physics, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS
Abstract

The first period (GALLEX I) of data taking in the GALLEX solar neutrino experiment has been completed. From 14 May 1991 to 29 April 1992, the experiment observed the solar neutrino flux using neutrino capture by 71 Ga to form 71 Ge. Counting ended on 2 November 1992. The final result from the 15 runs of this periodpis (81±17 [ stat .]±9 [ syst .]) SNU (1 σ ). The first 6 runs of GALLEX II recorded the neutrino signal from 19 August 1992 to 3 February 1993. The preliminary result for this period is (97±23 [ stat .]±7 [ syst .]) SNU (1 σ ). With counting data considered until 29 April 1993, the joint result for all 21 runs is (87±14 [ stat .]±7 [ syst .]) SNU (1 σ ). The present neutrino recording period GALLEX II is continuing with one solar exposure every four weeks.

Published
1993
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4. Solar neutrinos observed by GALLEX at Gran Sasso

Author

R. Mößbauer, R. Plaga, L. Paoluzi, F. Weyrich, C. Cattadori, C. Bacci, G. Heusser, Ettore Fiorini, G. Berthomieu, U. Schanda, J. Rich, W. Hampel, S. d'Angelo, N. Ferrari, M. Balata, K. Hellriegel, P. Belli, Charling Tao, E. Bellotti, E. Henrich, D. Vignaud, R. Wink, R. Bernabei, Michel Spiro, Till Kirsten, T. Fritsch, L. Zanotti, L. Gosset, F.X. Hartmann, M. Sann, U. Rönn, H. Lalla, S. Charbit, Ernst Pernicka, I. Carmi, I. Dostrovsky, S. Pezzoni, J. Kiko, J. Weneser, T. Stolarczyk, G. Dupont, M. Cribier, J.K. Rowley, P. Anselmann, Marcin Wójcik, C. Schlosser, Oliviero Cremonesi, F. von Feilitzsch, R.W. Stoenner, K.H. Ebert, L. Stieglitz, R. von Ammon, R.L. Hahn, E. Schatzman, Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Kernforschungs Zentrum Karlsruhe, Laboratori Nazionali del Gran Sasso (LNGS), Istituto Nazionale di Fisica Nucleare (INFN), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departement d'Astrophysique Stellaire et Galactique (DASGAL), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Weizmann Institute of Science [Rehovot, Israël], Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tor Vergata (INFN, Sezione di Roma Tor Vergata), Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), and GALLEX Collaboration

Subjects
Particle physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Solar neutrino, Gallium chloride, 7. Clean energy, 01 natural sciences, Settore FIS/04 - Fisica Nucleare e Subnucleare, Nuclear physics, 0103 physical sciences, OSCILLATIONS, solar neutrinos, gallex, 010306 general physics, Neutrino oscillation, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS, Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Standard solar model, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Settore FIS/01 - Fisica Sperimentale, Solar neutrino problem, Atomic and Molecular Physics, and Optics, Neutrino detector, 13. Climate action, MATTER, Measurements of neutrino speed, High Energy Physics::Experiment, GALLEX, Neutrino
Abstract

International audience; We have measured the rate of production of $^{71}$Ge from $^{71}$Ga by solar neutrinos. The target consists of 30.3 t of gallium in the form of 8.13 M aqueous gallium chloride solution (101 t), shielded by $\approx$ 3300 m water equivalent of standard rock in the Gran Sasso Underground Laboratory (Italy). In nearly one year of operation, 14 measurements of the production rate of $^{71}$Ge were carried out to give, after corrections for side reactions and other backgrounds, an average value of 83$\pm$19 (stat.)$\pm$8 (syst.) SNU (l$\sigma$) due to solar neutrinos. This conclusion constitutes the first observation of solar pp neutrinos. Our result is consistent with the presence of the full pp neutrino flux expected according to the "standard solar model" together with a reduced flux of $^8$B+$^7$Be neutrinos as observed in the Homestake and Kamiokande experiments. Astrophysical reasons remain as a possible explanation of the solar neutrino problem. On the other hand, if the result is to be interpreted in terms of the MSW effect, it would fix neutrino masses and mixing angles within a very restricted range.

Published
1993
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5. Status report on theGALLEX experiment

Author

E. Henrich, I. Carmi, P. Anselmann, J. Weneser, U. Schanda, L. Paoluzi, S. d'Angelo, Oliviero Cremonesi, F.X. Hartmann, N. Ferrari, M. Balata, L. Gosset, J. Rich, M. Cribier, F. von Feilitzsch, E. Bellotti, R. Bernabei, R. Plaga, L. Zanotti, J. Kiko, W. Hampel, M. Sann, C. Cattadori, P. Belli, G. Berthomieu, J.K. Rowley, K.H. Ebert, R.W. Stoenner, U. Rönn, H. Lalla, S. Charbit, R. Wink, Ernst Pernicka, Till Kirsten, T. Fritsch, C. Schlosser, R. von Ammon, G. Du Pont, T. Stolarczyk, S. Pezzoni, Marcin Wójcik, Charling Tao, I. Dostrovsky, C. Bacci, E. Schatzman, R. Möβbauer, L. Stieglitz, F. Weyrich, K. Hellriegel, D. Vignaud, Ettore Fiorini, Michel Spiro, R.L. Hahn, G. Heusser, Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, 010308 nuclear & particles physics, Solar neutrino, Settore FIS/01 - Fisica Sperimentale, Status report, 7. Clean energy, 01 natural sciences, Settore FIS/04 - Fisica Nucleare e Subnucleare, Nuclear physics, 0103 physical sciences, Underground laboratory, GALLEX, Neutrino, 010306 general physics, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS
Abstract

The GALLEX collaboration is performing an experiment for the detection of neutrinos coming principally from the p-p fusion reaction in the Sun, via the reaction ve +71Ga →71Ge + e-. The experiment is running in the Gran Sasso Underground Laboratory of INFN, using as a target 30.3 tons of gallium in the form of 8.13 molar aqueous GaCl3 solution. A report is given of the status of GALLEX after the end of the operations devoted to the removal from the solution of the cosmogenically formed Ge isotopes, completed in the middle of 1991. The experiment is now collecting data on solar neutrinos and the data analysis is in progress. Preliminary results concerning the first year of measurement are presented.

Published
1992
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6. Implications of the GALLEX determination of the solar neutrino flux

Author

R. von Ammon, I. Dostrovsky, E. Schatzman, E. Henrich, Marcin Wójcik, J.K. Rowley, P. Anselmann, U. Rönn, L. Gosset, J. Weneser, U. Schanda, K.H. Ebert, S. d'Angelo, Ettore Fiorini, I. Carmi, L. Zanotti, Charling Tao, M. Sann, Michel Spiro, P. Belli, R. Plaga, R. Bernabei, Till Kirsten, C. Cattadori, C. Bacci, J. Rich, G. Heusser, W. Hampel, R. Wink, Oliviero Cremonesi, F. von Feilitzsch, F.X. Hartmann, M. Cribier, S. Charbit, T. Stolarczyk, R.L. Hahn, G. Dupont, R.W. Stoenner, Ernst Pernicka, C. Schlosser, L. Paoluzi, S. Pezzoni, J. Kiko, G. Berthomieu, H. Lalla, D. Vignaud, E. Bellotti, R. Mößbauer, N. Ferrari, M. Balata, Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Nuclear and High Energy Physics, Particle physics, Solar neutrino, Flux, 7. Clean energy, 01 natural sciences, Settore FIS/04 - Fisica Nucleare e Subnucleare, Nuclear physics, REGENERATION, Resonance oscillation, 0103 physical sciences, OSCILLATIONS, EARTH, 010306 general physics, Neutrino oscillation, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, ComputingMilieux_MISCELLANEOUS, Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, 010308 nuclear & particles physics, Settore FIS/01 - Fisica Sperimentale, SUN, MATTER, MODEL, Massless particle, Neutrino, GALLEX
Abstract

The GALLEX result 83 ± 19 (stat.) ± 8 (syst.) SNU is two standard deviations below the predictions of stellar model calculations (124–132 SNU). To fit this result together with those of the chlorine and Kamiokande experiments requires severe stretching of solar models but does not rule out such a procedure, leaving the possibility of massless neutrinos. It clearly implies that the pp neutrinos have been detected. The Mikheyev-Smirnov-Wolfenstein (MSW) mechanism provides a good fit, and the GALLEX result fixes the Δm 2 and sin 2 2 θ parameters in two very confined ranges (around Δm 2 = 6 × 10 −6 eV 2 and sin 2 2 θ = 7 × 10 −3 and around Δm 2 = 8 × 10 −6 eV 2 and sin 2 2 θ = 0.6). Explanations of the solar neutrino problems based on the decay or magnetic interactions of neutrinos are disfavoured.

Published
1992
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