M. Casolino

M. Casolino
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High Energy Astrophysical Phenomena (23)
 
Astrophysics (12)
 
High Energy Physics - Experiment (8)
 
Physics - Space Physics (8)
 
Instrumentation and Methods for Astrophysics (7)
 
Earth and Planetary Astrophysics (6)
 
Solar and Stellar Astrophysics (5)
 
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Publications Authored By M. Casolino

2017Jan
Affiliations: 1National Research Nuclear University MEPhI, 2INFN, Sezione di Florence and Physics Department of University of Florence, 3INFN, Sezione di Naples and Physics Department of University of Naples Federico II, 4Lebedev Physical Institute, 5INFN, Sezione di Bari Physics and Department of University of Bari, 6INFN, Sezione di Trieste, 7Ioffe Physical Technical Institute, 8INFN, Sezione di Florence and Physics Department of University of Florence, 9INFN, Sezione di Trieste, 10INFN, Sezione di Florence and Physics Department of University of Florence, 11INFN, Sezione di Bari Physics and Department of University of Bari, 12INFN, Sezione di Bari Physics and Department of University of Bari, 13INFN, Sezione di Naples and Physics Department of University of Naples Federico II, 14KTH, Department of Physics, and The Oskar Klein Centre for Cosmoparticle Physics, 15INFN, Sezione di Rome "Tor Vergata", 16INFN, IFAC, 17INFN, Sezione di Rome "Tor Vergata", 18INFN, Sezione di Rome "Tor Vergata", 19INFN, Sezione di Rome "Tor Vergata", 20INFN, Sezione di Rome "Tor Vergata", 21National Research Nuclear University MEPhI, 22National Research Nuclear University MEPhI, 23National Research Nuclear University MEPhI, 24National Research Nuclear University MEPhI, 25Ioffe Physical Technical Institute, 26Lebedev Physical Institute, 27National Research Nuclear University MEPhI, 28National Research Nuclear University MEPhI, 29National Research Nuclear University MEPhI, 30INFN, Sezione di Rome "Tor Vergata", 31INFN, Sezione di Rome "Tor Vergata", 32National Research Nuclear University MEPhI, 33Universität Siegen, Department of Physics, 34INFN, Sezione di Rome "Tor Vergata", 35INFN, Sezione di Trieste, 36INFN, Sezione di Bari Physics and Department of University of Bari, 37INFN, IFAC, 38INFN, Sezione di Trieste, 39INFN, Sezione di Naples and Physics Department of University of Naples Federico II, 40INFN, Sezione di Florence and Physics Department of University of Florence, 41INFN, Sezione di Rome "Tor Vergata", 42INFN, Sezione di Naples and Physics Department of University of Naples Federico II, 43KTH, Department of Physics, and The Oskar Klein Centre for Cosmoparticle Physics, 44INFN, Sezione di Rome "Tor Vergata", 45INFN, Laboratori Nazionali di Frascati, 46INFN, Sezione di Florence and Physics Department of University of Florence, 47National Research Nuclear University MEPhI, 48Universität Siegen, Department of Physics, 49INFN, Sezione di Rome "Tor Vergata", 50National Research Nuclear University MEPhI, 51Lebedev Physical Institute, 52INFN, Sezione di Trieste, 53INFN, Sezione di Florence and Physics Department of University of Florence, 54Ioffe Physical Technical Institute, 55National Research Nuclear University MEPhI, 56National Research Nuclear University MEPhI, 57INFN, Sezione di Trieste, 58INFN, Sezione di Trieste

We present a measurements of electron and positron fluxes below the geomagnetic cutoff rigidity in wide energy range from 50 MeV to several GeV by the PAMELA magnetic spectrometer. The instrument was launched on June 15th 2006 on-board the Resurs-DK satellite on low orbit with 70 degrees inclination and altitude between 350 and 600 km. The procedure of trajectories calculations in the geomagnetic field separates stably trapped and albedo components produced in interactions of cosmic ray protons with the residual atmosphere from galactic cosmic rays. Read More

2016Oct
Authors: D. de Florian1, C. Grojean2, F. Maltoni3, C. Mariotti4, A. Nikitenko5, M. Pieri6, P. Savard7, M. Schumacher8, R. Tanaka9, R. Aggleton10, M. Ahmad11, B. Allanach12, C. Anastasiou13, W. Astill14, S. Badger15, M. Badziak16, J. Baglio17, E. Bagnaschi18, A. Ballestrero19, A. Banfi20, D. Barducci21, M. Beckingham22, C. Becot23, G. Bélanger24, J. Bellm25, N. Belyaev26, F. U. Bernlochner27, C. Beskidt28, A. Biekötter29, F. Bishara30, W. Bizon31, N. E. Bomark32, M. Bonvini33, S. Borowka34, V. Bortolotto35, S. Boselli36, F. J. Botella37, R. Boughezal38, G. C. Branco39, J. Brehmer40, L. Brenner41, S. Bressler42, I. Brivio43, A. Broggio44, H. Brun45, G. Buchalla46, C. D. Burgard47, A. Calandri48, L. Caminada49, R. Caminal Armadans50, F. Campanario51, J. Campbell52, F. Caola53, C. M. Carloni Calame54, S. Carrazza55, A. Carvalho56, M. Casolino57, O. Cata58, A. Celis59, F. Cerutti60, N. Chanon61, M. Chen62, X. Chen63, B. Chokoufé Nejad64, N. Christensen65, M. Ciuchini66, R. Contino67, T. Corbett68, D. Curtin69, M. Dall'Osso70, A. David71, S. Dawson72, J. de Blas73, W. de Boer74, P. de Castro Manzano75, C. Degrande76, R. L. Delgado77, F. Demartin78, A. Denner79, B. Di Micco80, R. Di Nardo81, S. Dittmaier82, A. Dobado83, T. Dorigo84, F. A. Dreyer85, M. Dührssen86, C. Duhr87, F. Dulat88, K. Ecker89, K. Ellis90, U. Ellwanger91, C. Englert92, D. Espriu93, A. Falkowski94, L. Fayard95, R. Feger96, G. Ferrera97, A. Ferroglia98, N. Fidanza99, T. Figy100, M. Flechl101, D. Fontes102, S. Forte103, P. Francavilla104, E. Franco105, R. Frederix106, A. Freitas107, F. F. Freitas108, F. Frensch109, S. Frixione110, B. Fuks111, E. Furlan112, S. Gadatsch113, J. Gao114, Y. Gao115, M. V. Garzelli116, T. Gehrmann117, R. Gerosa118, M. Ghezzi119, D. Ghosh120, S. Gieseke121, D. Gillberg122, G. F. Giudice123, E. W. N. Glover124, F. Goertz125, D. Gonçalves126, J. Gonzalez-Fraile127, M. Gorbahn128, S. Gori129, C. A. Gottardo130, M. Gouzevitch131, P. Govoni132, D. Gray133, M. Grazzini134, N. Greiner135, A. Greljo136, J. Grigo137, A. V. Gritsan138, R. Gröber139, S. Guindon140, H. E. Haber141, C. Han142, T. Han143, R. Harlander144, M. A. Harrendorf145, H. B. Hartanto146, C. Hays147, S. Heinemeyer148, G. Heinrich149, M. Herrero150, F. Herzog151, B. Hespel152, V. Hirschi153, S. Hoeche154, S. Honeywell155, S. J. Huber156, C. Hugonie157, J. Huston158, A. Ilnicka159, G. Isidori160, B. Jäger161, M. Jaquier162, S. P. Jones163, A. Juste164, S. Kallweit165, A. Kaluza166, A. Kardos167, A. Karlberg168, Z. Kassabov169, N. Kauer170, D. I. Kazakov171, M. Kerner172, W. Kilian173, F. Kling174, K. Köneke175, R. Kogler176, R. Konoplich177, S. Kortner178, S. Kraml179, C. Krause180, F. Krauss181, M. Krawczyk182, A. Kulesza183, S. Kuttimalai184, R. Lane185, A. Lazopoulos186, G. Lee187, P. Lenzi188, I. M. Lewis189, Y. Li190, S. Liebler191, J. Lindert192, X. Liu193, Z. Liu194, F. J. Llanes-Estrada195, H. E. Logan196, D. Lopez-Val197, I. Low198, G. Luisoni199, P. Maierhöfer200, E. Maina201, B. Mansoulié202, H. Mantler203, M. Mantoani204, A. C. Marini205, V. I. Martinez Outschoorn206, S. Marzani207, D. Marzocca208, A. Massironi209, K. Mawatari210, J. Mazzitelli211, A. McCarn212, B. Mellado213, K. Melnikov214, S. B. Menari215, L. Merlo216, C. Meyer217, P. Milenovic218, K. Mimasu219, S. Mishima220, B. Mistlberger221, S. -O. Moch222, A. Mohammadi223, P. F. Monni224, G. Montagna225, M. Moreno Llácer226, N. Moretti227, S. Moretti228, L. Motyka229, A. Mück230, M. Mühlleitner231, S. Munir232, P. Musella233, P. Nadolsky234, D. Napoletano235, M. Nebot236, C. Neu237, M. Neubert238, R. Nevzorov239, O. Nicrosini240, J. Nielsen241, K. Nikolopoulos242, J. M. No243, C. O'Brien244, T. Ohl245, C. Oleari246, T. Orimoto247, D. Pagani248, C. E. Pandini249, A. Papaefstathiou250, A. S. Papanastasiou251, G. Passarino252, B. D. Pecjak253, M. Pelliccioni254, G. Perez255, L. Perrozzi256, F. Petriello257, G. Petrucciani258, E. Pianori259, F. Piccinini260, M. Pierini261, A. Pilkington262, S. Plätzer263, T. Plehn264, R. Podskubka265, C. T. Potter266, S. Pozzorini267, K. Prokofiev268, A. Pukhov269, I. Puljak270, M. Queitsch-Maitland271, J. Quevillon272, D. Rathlev273, M. Rauch274, E. Re275, M. N. Rebelo276, D. Rebuzzi277, L. Reina278, C. Reuschle279, J. Reuter280, M. Riembau281, F. Riva282, A. Rizzi283, T. Robens284, R. Röntsch285, J. Rojo286, J. C. Romão287, N. Rompotis288, J. Roskes289, R. Roth290, G. P. Salam291, R. Salerno292, R. Santos293, V. Sanz294, J. J. Sanz-Cillero295, H. Sargsyan296, U. Sarica297, P. Schichtel298, J. Schlenk299, T. Schmidt300, C. Schmitt301, M. Schönherr302, U. Schubert303, M. Schulze304, S. Sekula305, M. Sekulla306, E. Shabalina307, H. S. Shao308, J. Shelton309, C. H. Shepherd-Themistocleous310, S. Y. Shim311, F. Siegert312, A. Signer313, J. P. Silva314, L. Silvestrini315, M. Sjodahl316, P. Slavich317, M. Slawinska318, L. Soffi319, M. Spannowsky320, C. Speckner321, D. M. Sperka322, M. Spira323, O. Stål324, F. Staub325, T. Stebel326, T. Stefaniak327, M. Steinhauser328, I. W. Stewart329, M. J. Strassler330, J. Streicher331, D. M. Strom332, S. Su333, X. Sun334, F. J. Tackmann335, K. Tackmann336, A. M. Teixeira337, R. Teixeira de Lima338, V. Theeuwes339, R. Thorne340, D. Tommasini341, P. Torrielli342, M. Tosi343, F. Tramontano344, Z. Trócsányi345, M. Trott346, I. Tsinikos347, M. Ubiali348, P. Vanlaer349, W. Verkerke350, A. Vicini351, L. Viliani352, E. Vryonidou353, D. Wackeroth354, C. E. M. Wagner355, J. Wang356, S. Wayand357, G. Weiglein358, C. Weiss359, M. Wiesemann360, C. Williams361, J. Winter362, D. Winterbottom363, R. Wolf364, M. Xiao365, L. L. Yang366, R. Yohay367, S. P. Y. Yuen368, G. Zanderighi369, M. Zaro370, D. Zeppenfeld371, R. Ziegler372, T. Zirke373, J. Zupan374
Affiliations: 1eds., 2eds., 3eds., 4eds., 5eds., 6eds., 7eds., 8eds., 9eds., 10The LHC Higgs Cross Section Working Group, 11The LHC Higgs Cross Section Working Group, 12The LHC Higgs Cross Section Working Group, 13The LHC Higgs Cross Section Working Group, 14The LHC Higgs Cross Section Working Group, 15The LHC Higgs Cross Section Working Group, 16The LHC Higgs Cross Section Working Group, 17The LHC Higgs Cross Section Working Group, 18The LHC Higgs Cross Section Working Group, 19The LHC Higgs Cross Section Working Group, 20The LHC Higgs Cross Section Working Group, 21The LHC Higgs Cross Section Working Group, 22The LHC Higgs Cross Section Working Group, 23The LHC Higgs Cross Section Working Group, 24The LHC Higgs Cross Section Working Group, 25The LHC Higgs Cross Section Working Group, 26The LHC Higgs Cross Section Working Group, 27The LHC Higgs Cross Section Working Group, 28The LHC Higgs Cross Section Working Group, 29The LHC Higgs Cross Section Working Group, 30The LHC Higgs Cross 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This Report summarizes the results of the activities of the LHC Higgs Cross Section Working Group in the period 2014-2016. The main goal of the working group was to present the state-of-the-art of Higgs physics at the LHC, integrating all new results that have appeared in the last few years. The first part compiles the most up-to-date predictions of Higgs boson production cross sections and decay branching ratios, parton distribution functions, and off-shell Higgs boson production and interference effects. Read More

The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetically trapped and albedo particles. Its observations comprise the solar energetic particle events between solar cycles 23 and 24, and the geomagnetic cutoff variations during magnetospheric storms. Read More

Cosmic-ray electrons and positrons are a unique probe of the propagation of cosmic rays as well as of the nature and distribution of particle sources in our Galaxy. Recent measurements of these particles are challenging our basic understanding of the mechanisms of production, acceleration and propagation of cosmic rays. Particularly striking are the differences between the low energy results collected by the space-borne PAMELA and AMS-02 experiments and older measurements pointing to sign-charge dependence of the solar modulation of cosmic-ray spectra. Read More

Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy (>80 MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (94 min). Estimated cutoff values were compared with those obtained by means of a trajectory tracing approach based on a dynamical empirical modeling of the Earth's magnetosphere. Read More

The cosmic-ray hydrogen and helium ($^1$H, $^2$H, $^3$He, $^4$He) isotopic composition has been measured with the satellite-borne experiment PAMELA, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. The rare isotopes $^2$H and $^3$He in cosmic rays are believed to originate mainly from the interaction of high energy protons and helium with the galactic interstellar medium. The isotopic composition was measured between 100 and 1100 MeV/n for hydrogen and between 100 and 1400 MeV/n for helium isotopes using two different detector systems over the 23rd solar minimum from July 2006 to December 2007. Read More

Precision measurements of the electron component in the cosmic radiation provide important information about the origin and propagation of cosmic rays in the Galaxy not accessible from the study of the cosmic-ray nuclear components due to their differing diffusion and energy-loss processes. However, when measured near Earth, the effects of propagation and modulation of galactic cosmic rays in the heliosphere, particularly significant for energies up to at least 30 GeV, must be properly taken into account. In this paper the electron (e^-) spectra measured by PAMELA down to 70 MeV from July 2006 to December 2009 over six-months time intervals are presented. Read More

The PAMELA satellite experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth space, bridging the low energy data by other space-based instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies. This work reports the analysis methods developed to estimate the SEP energy spectra as a function of the particle pitch-angle with respect to the Interplanetary Magnetic Field (IMF) direction. Read More

Data from the PAMELA satellite experiment were used to measure the geomagnetic cutoff for high-energy ($\gtrsim$ 80 MeV) protons during the solar particle events on 2006 December 13 and 14. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to single spacecraft orbits (about 94 minutes). Estimated cutoff values were cross-checked with those obtained by means of a trajectory tracing approach based on dynamical empirical modeling of the Earth's magnetosphere. Read More

Data from the PAMELA satellite experiment were used to perform a detailed measurement of under-cutoff protons at low Earth orbits. On the basis of a trajectory tracing approach using a realistic description of the magnetosphere, protons were classified into geomagnetically trapped and re-entrant albedo. The former include stably-trapped protons in the South Atlantic Anomaly, which were analyzed in the framework of the adiabatic theory, investigating energy spectra, spatial and angular distributions; results were compared with the predictions of the AP8 and the PSB97 empirical trapped models. Read More

CP-odd scalars are an integral part of many extensions of the Standard Model. Recently, electroweak-scale pseudoscalars have received increased attention in explaining the diffuse gamma-ray excess from the Galactic Centre. Elusive due to absence of direct couplings to gauge bosons, these particles receive only weak constraints from direct searches at LEP or searches performed during the first LHC runs. Read More

We present a precise measurement of downward-going albedo proton fluxes for kinetic energy above $\sim$ 70 MeV performed by the PAMELA experiment at an altitude between 350 and 610 km. On the basis of a trajectory tracing simulation, the analyzed protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped spreading over all latitudes, including both short-lived (precipitating) and long-lived (pseudo-trapped) components. In addition, features of the penumbra region around the geomagnetic cutoff were investigated in detail. Read More

We present a concept for large-area, low-cost detection of ultra-high energy cosmic rays (UHECRs) with a Fluorescence detector Array of Single-pixel Telescopes (FAST), addressing the requirements for the next generation of UHECR experiments. In the FAST design, a large field of view is covered by a few pixels at the focal plane of a mirror or Fresnel lens. We report first results of a FAST prototype installed at the Telescope Array site, consisting of a single 200 mm photomultiplier tube at the focal plane of a 1 m$^2$ Fresnel lens system taken from the prototype of the JEM-EUSO experiment. Read More

The nature of particle acceleration at the Sun, whether through flare reconnection processes or through shocks driven by coronal mass ejections (CMEs), is still under scrutiny despite decades of research. The measured properties of solar energetic particles (SEPs) have long been modeled in different particle-acceleration scenarios. The challenge has been to disentangle to the effects of transport from those of acceleration. Read More

Two types of orbital detectors of extreme energy cosmic rays are being developed nowadays: (i) TUS and KLYPVE with reflecting optical systems (mirrors) and (ii) JEM-EUSO with high-transmittance Fresnel lenses. They will cover much larger areas than existing ground-based arrays and almost uniformly monitor the celestial sphere. The TUS detector is the pioneering mission developed in SINP MSU in cooperation with several Russian and foreign institutions. Read More

Reliability assessment in concerned with the analysis of devices and systems whose individual components are prone to fail. This reliability analysis documents the process and results of reliability determination of the JEM-EUSO photomultiplier tube component using the methods 217 Plus. Quantum efficiency degradation and radiation hardness assurance. Read More

The PAMELA satellite-borne experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from $\sim$80 MeV to several GeV in near-Earth space. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies related to SEP events. This paper focuses on the analysis methods developed to estimate SEP energy spectra as a function of the particle pitch angle with respect to the Interplanetary Magnetic Field (IMF). Read More

We report an accurate measurement of the geomagnetically trapped proton fluxes for kinetic energy above > 70 MeV performed by the PAMELA mission at low Earth orbits (350-610 km). Data were analyzed in the frame of the adiabatic theory of charged particle motion in the geomagnetic field. Flux properties were investigated in detail, providing a full characterization of the particle radiation in the South Atlantic Anomaly region, including locations, energy spectra and pitch angle distributions. Read More

Precision measurements of the positron component in the cosmic radiation provide important information about the propagation of cosmic rays and the nature of particle sources in our Galaxy. The satellite-borne experiment PAMELA has been used to make a new measurement of the cosmic-ray positron flux and fraction that extends previously published measurements up to 300 GeV in kinetic energy. The combined measurements of the cosmic-ray positron energy spectrum and fraction provide a unique tool to constrain interpretation models. Read More

2013May
Authors: J. H. Adams, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, M. Ave, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, L. del Peral, A. Dell'Oro, M. P. De Pascale, M. Di Martino, G. Distratis, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, I. Fernandez-Gomez, S. Ferrarese, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgrio, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, K. Mannheim, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rios, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, T. Nakamura, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reina, M. Reyes, M. Ricci, I. Rodriguez, M. D. Rodriguez Frias, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieb, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, Y. Takahashi, H. Takami, M. Takeda, Y. Takizawa, C. Tenzer, O. Tibolla, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi

We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. Read More

The satellite-borne experiment PAMELA has been used to make new measurements of cosmic ray H and He isotopes. The isotopic composition was measured between 100 and 600 MeV/n for hydrogen and between 100 and 900 MeV/n for helium isotopes over the 23rd solar minimum from July 2006 to December 2007. The energy spectrum of these components carries fundamental information regarding the propagation of cosmic rays in the galaxy which are competitive with those obtained from other secondary to primary measurements such as B/C. Read More

2012Apr
Authors: The JEM-EUSO Collaboration, :, J. H. Adams Jr, S. Ahmad, J. -N. Albert, D. Allard, M. Ambrosio, L. Anchordoqui, A. Anzalone, Y. Arai, C. Aramo, K. Asano, P. Barrillon, T. Batsch, J. Bayer, T. Belenguer, R. Bellotti, A. A. Berlind, M. Bertaina, P. L. Biermann, S. Biktemerova, C. Blaksley, J. Blecki, S. Blin-Bondil, J. Bluemer, P. Bobik, M. Bogomilov, M. Bonamente, M. S. Briggs, S. Briz, A. Bruno, F. Cafagna, D. Campana, J-N. Capdevielle, R. Caruso, M. Casolino, C. Cassardo, G. Castellini, O. Catalano, A. Cellino, M. Chikawa, M. J. Christl, V. Connaughton, J. F. Cortes, H. J. Crawford, R. Cremonini, S. Csorna, J. C. D'Olivo, S. Dagoret-Campagne, A. J. de Castro, C. De Donato, C. de la Taille, M. P. De Pascale, L. del Peral, A. Dell'Oro, M. Di Martino, G. Distrati, M. Dupieux, A. Ebersoldt, T. Ebisuzaki, R. Engel, S. Falk, K. Fang, F. Fenu, S. Ferrarese, I. Fernandez-Gomez, A. Franceschi, J. Fujimoto, P. Galeotti, G. Garipov, J. Geary, U. G. Giaccari, G. Giraudo, M. Gonchar, C. Gonzalez Alvarado, P. Gorodetzky, F. Guarino, A. Guzman, Y. Hachisu, B. Harlov, A. Haungs, J. Hernandez Carretero, K. Higashide, T. Iguchi, H. Ikeda, N. Inoue, S. Inoue, A. Insolia, F. Isgro, Y. Itow, E. Joven, E. G. Judd, A. Jung, F. Kajino, T. Kajino, I. Kaneko, Y. Karadzhov, J. Karczmarczyk, K. Katahira, K. Kawai, Y. Kawasaki, B. Keilhauer, B. A. Khrenov, Jeong-Sook Kim, Soon-Wook Kim, Sug-Whan Kim, M. Kleifges, P. A. Klimov, S. H. Ko, D. Kolev, I. Kreykenbohm, K. Kudela, Y. Kurihara, E. Kuznetsov, G. La Rosa, J. Lee, J. Licandro, H. Lim, F. Lopez, M. C. Maccarone, L. Marcelli, A. Marini, G. Martin-Chassard, O. Martinez, G. Masciantonio, K. Mase, R. Matev, A. Maurissen, G. Medina-Tanco, T. Mernik, H. Miyamoto, Y. Miyazaki, Y. Mizumoto, G. Modestino, D. Monnier-Ragaigne, J. A. Morales de los Rıos, B. Mot, T. Murakami, M. Nagano, M. Nagata, S. Nagataki, J. W. Nam, S. Nam, K. Nam, T. Napolitano, D. Naumov, A. Neronov, K. Nomoto, T. Ogawa, H. Ohmori, A. V. Olinto, P. Orleanski, G. Osteria, N. Pacheco, M. I. Panasyuk, E. Parizot, I. H. Park, B. Pastircak, T. Patzak, T. Paul, C. Pennypacker, T. Peter, P. Picozza, A. Pollini, H. Prieto, P. Reardon, M. Reina, M. Reyes, M. Ricci, I. Rodrıguez, M. D. Rodrıguez Frıas, F. Ronga, H. Rothkaehl, G. Roudil, I. Rusinov, M. Rybczynski, M. D. Sabau, G. Saez Cano, A. Saito, N. Sakaki, M. Sakata, H. Salazar, S. Sanchez, A. Santangelo, L. Santiago Cruz, M. Sanz Palomino, O. Saprykin, F. Sarazin, H. Sato, M. Sato, T. Schanz, H. Schieler, V. Scotti, M. Scuderi, A. Segreto, S. Selmane, D. Semikoz, M. Serra, S. Sharakin, T. Shibata, H. M. Shimizu, K. Shinozaki, T. Shirahama, G. Siemieniec-Ozieblo, H. H. Silva Lopez, J. Sledd, K. Slominska, A. Sobey, T. Sugiyama, D. Supanitsky, M. Suzuki, B. Szabelska, J. Szabelski, F. Tajima, N. Tajima, T. Tajima, H. Takami, T. Nakamura, M. Takeda, Y. Takahashi, Y. Takizawa, C. Tenzer, L. Tkachev, T. Tomida, N. Tone, F. Trillaud, R. Tsenov, K. Tsuno, T. Tymieniecka, Y. Uchihori, O. Vaduvescu, J. F. Valdes-Galicia, P. Vallania, L. Valore, G. Vankova, C. Vigorito, L. Villasenor, P. von Ballmoos, S. Wada, J. Watanabe, S. Watanabe, J. Watts Jr, M. Weber, T. J. Weiler, T. Wibig, L. Wiencke, M. Wille, J. Wilms, Z. Wlodarczyk, T. Yamamoto, Y. Yamamoto, J. Yang, H. Yano, I. V. Yashin, D. Yonetoku, K. Yoshida, S. Yoshida, R. Young, A. Zamora, A. Zuccaro Marchi

Contributions of the JEM-EUSO Collaboration to the 32nd International Cosmic Ray Conference, Beijing, August, 2011. Read More

The existence of a significant flux of antiprotons confined to Earth's magnetosphere has been considered in several theoretical works. These antiparticles are produced in nuclear interactions of energetic cosmic rays with the terrestrial atmosphere and accumulate in the geomagnetic field at altitudes of several hundred kilometers. A contribution from the decay of albedo antineutrons has been hypothesized in analogy to proton production by neutron decay, which constitutes the main source of trapped protons at energies above some tens of MeV. Read More

We present the space spectrometer PAMELA observations of proton and helium fluxes during the December 13 and 14, 2006 solar particle events. This is the first direct measurement of the solar energetic particles in space with a single instrument in the energy range from $\sim$ 80 MeV/n up to $\sim$ 3 GeV/n. In the event of December 13 measured energy spectra of solar protons and helium were compared with results obtained by neutron monitors and other detectors. Read More

The 15th of June 2006, the PAMELA satellite-borne experiment was launched from the Baikonur cosmodrome and it has been collecting data since July 2006. The apparatus comprises a time-of-flight system, a silicon-microstrip magnetic spectrometer, a silicon-tungsten electromagnetic calorimeter, an anticoincidence system, a shower tail counter scintillator and a neutron detector. The combination of these devices allows precision studies of the charged cosmic radiation to be conducted over a wide energy range (100 MeV -- 100's GeV) with high statistics. Read More

PAMELA is a satellite borne experiment designed to study with great accuracy cosmic rays of galactic, solar, and trapped nature in a wide energy range (protons: 80 MeV-700 GeV, electrons 50 MeV-400 GeV). Main objective is the study of the antimatter component: antiprotons (80 MeV-190 GeV), positrons (50 MeV-270 GeV) and search for antimatter with a precision of the order of $10^{-8}$). The experiment, housed on board the Russian Resurs-DK1 satellite, was launched on June, 15 2006 in a $350\times 600 km$ orbit with an inclination of 70 degrees. Read More

Positrons are known to be produced in interactions between cosmic-ray nuclei and interstellar matter ("secondary production"). Positrons may, however, also be created by dark matter particle annihilations in the galactic halo or in the magnetospheres of near-by pulsars. The nature of dark matter is one of the most prominent open questions in science today. Read More

PAMELA is a satellite borne experiment designed to study with great accuracy cosmic rays of galactic, solar, and trapped nature in a wide energy range (protons: 80 MeV-700 GeV, electrons 50 MeV-400 GeV). Main objective is the study of the antimatter component: antiprotons (80 MeV-190 GeV), positrons (50 MeV-270 GeV) and search for antinuclei with a precision of the order of $10^{-8}$). The experiment, housed on board the Russian Resurs-DK1 satellite, was launched on June, $15^{th}$ 2006 in a $350\times 600 km$ orbit with an inclination of 70 degrees. Read More

On the 15th of June 2006, the PAMELA satellite-borne experiment was launched from the Baikonur cosmodrome and it has been collecting data since July 2006. The apparatus comprises a time-of-flight system, a silicon-microstrip magnetic spectrometer, a silicon-tungsten electromagnetic calorimeter, an anticoincidence system, a shower tail counter scintillator and a neutron detector. The combination of these devices allows precision studies of the charged cosmic radiation to be conducted over a wide energy range (100 MeV - 100's GeV) with high statistics. Read More

The PAMELA experiment is devoted to the study of cosmic rays in Low Earth Orbit with an apparatus optimized to perform a precise determination of the galactic antimatter component of c.r. It is constituted by a number of detectors built around a permanent magnet spectrometer. Read More

The Altcriss project aims to perform a long term survey of the radiation environment on board the International Space Station. Measurements are being performed with active and passive devices in different locations and orientations of the Russian segment of the station. The goal is to perform a detailed evaluation of the differences in particle fluence and nuclear composition due to different shielding material and attitude of the station. Read More

PAMELA is a satellite borne experiment designed to study with great accuracy cosmic rays of galactic, solar, and trapped nature in a wide energy range protons: 80 MeV-700 GeV, electrons 50 MeV-400 GeV). Main objective is the study of the antimatter component: antiprotons (80 MeV-190 GeV), positrons (50 MeV-270 GeV) and search for antimatter with a precision of the order of 10^-8). The experiment, housed on board the Russian Resurs-DK1 satellite, was launched on June, 15, 2006 in a 350*600 km orbit with an inclination of 70 degrees. Read More

The PAMELA experiment is a satellite-borne apparatus designed to study charged particles in the cosmic radiation with a particular focus on antiparticles. PAMELA is mounted on the Resurs DK1 satellite that was launched from the Baikonur cosmodrome on June 15th 2006. The PAMELA apparatus comprises a time-of-flight system, a magnetic spectrometer, a silicon-tungsten electromagnetic calorimeter, an anticoincidence system, a shower tail catcher scintillator and a neutron detector. Read More

A new measurement of the primary cosmic-ray proton and helium fluxes from 3 to 350 GeV was carried out by the balloon-borne CAPRICE experiment in 1998. This experimental setup combines different detector techniques and has excellent particle discrimination capabilities allowing clear particle identification. Our experiment has the capability to determine accurately detector selection efficiencies and systematic errors associated with them. Read More

Cosmic ray measurements performed with the instrument SilEye-2 on Mir space station are presented. SilEye-2 is a silicon detector telescope for the study of the causes of Light Flashes perception by astronauts. As a stand-alone device, it monitors in the short and long term the radiation composition inside Mir. Read More

This article reports nine Solar Energetic Particle events detected by the instrument NINA between October 1998 and April 1999. NINA is a silicon-based particle detector mounted on-board the Russian satellite Resurs-01-N4, which has flown at an altitude of about 800 km in polar inclination since July 1998. For every solar event the power-law He4 spectrum across the energy interval 10--50 MeV/n was reconstructed, and spectral indexes, gamma, from 1. Read More