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  • 1. Adriani, O.
    et al.
    Barbarino, G. C.
    Bazilevskaya, G. A.
    Boezio, M.
    Bogomolov, E. A.
    Bonechi, L.
    Bongi, M.
    Bonvicini, V.
    Borisov, S. V.
    Bottai, S.
    Bruno, A.
    Cafagna, F.
    Campana, D.
    Carbone, R.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Casolino, M.
    Castellini, G.
    De Pascale, M. P.
    De Santis, C.
    De Simone, N.
    Di Felice, V.
    Galper, A. M.
    Gillard, William
    KTH, School of Engineering Sciences (SCI), Physics.
    Grishantseva, L. A.
    Jerse, G.
    Karelin, A. V.
    Krutkov, S. Y.
    Kvashnin, A. N.
    Leonov, A. A.
    Malakhov, V. V.
    Marcelli, L.
    Mayorov, A. G.
    Koldashov, S. V.
    Mikhailov, V. V.
    Mocchiutti, E.
    Monaco, A.
    Mori, N.
    Osteria, G.
    Palma, F.
    Papini, P.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Picozza, P.
    Pizzolotto, C.
    Ricciarini, S.
    Rossetto, Laura
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Sarkar, R.
    Simon, M.
    Sparvoli, R.
    Spillantini, P.
    Stozhkov, Y. I.
    Vacchi, A.
    Vannuccini, E.
    Vasilyev, G. I.
    Voronov, S. A.
    Yurkin, Y. T.
    Wu, Juan
    KTH, School of Engineering Sciences (SCI), Physics.
    Zampa, G.
    Zampa, N.
    Zverev, V. G.
    Measurements of cosmic-ray proton and helium spectra with the PAMELA calorimeter2013In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 51, no 2, p. 219-226Article in journal (Refereed)
    Abstract [en]

    We present a new measurement of the cosmic ray proton and helium spectra by the PAMELA experiment performed using the "thin" (in terms of nuclei interactions) sampling electromagnetic calorimeter. The described method, optimized by using Monte Carlo simulation, beam test and experimental data, allows the spectra to be measured up to 10 TeV, thus extending the PAMELA observational range based on the magnetic spectrometer measurement.

  • 2.
    Amati, L.
    et al.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    O'Brien, P.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Gotz, D.
    Univ Paris Saclay, IRFU, CEA, Dept Astrophys, F-91191 Gif Sur Yvette, France..
    Bozzo, E.
    Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland..
    Tenzer, C.
    Eberhard Karls Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Abt Hochenergieastrophys, Sand 1, D-72076 Tubingen, Germany..
    Frontera, F.
    Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy.;INAF IASF, Via Gobetti 101, I-40129 Bologna, Italy..
    Ghirlanda, G.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Labanti, C.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Osborne, J. P.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Stratta, G.
    Univ Urbino Carlo Bo, I-61029 Urbino, Italy..
    Tanvir, N.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.;Univ Leicester, Leicester Inst Space & Earth Observat, Univ Rd, Leicester LE1 7RH, Leics, England..
    Willingale, R.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Attina, P.
    GP Adv Projects, Gussago, Italy..
    Campana, R.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Castro-Tirado, A. J.
    CSIC, IAA, POB 03004, E-18080 Granada, Spain..
    Contini, C.
    OHB Italia, Via Gallarate 150, I-20151 Milan, Italy..
    Fuschino, F.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Gomboc, A.
    Univ Nova Gorica, Ctr Astrophys & Cosmol, Vipayska 11c, Ajdov V Sv cina 5270, Slovenia..
    Hudec, R.
    Czech Tech Univ, Fac Elect Engn, Prague 16627, Czech Republic.;Kazan Fed Univ, Kazan 420008, Russia..
    Orleanski, P.
    Polish Acad Sci, Space Res Ctr, Warsaw, Poland..
    Renotte, E.
    Ctr Spatial Liege, Parc Sci Sart Tilman Ave Pre Aily, B-4031 Angleur Liege, Belgium..
    Rodic, T.
    Slovenian Ctr Excellence Space Sci & Technol, SPACE SI, Ljubljana, Slovenia..
    Bagoly, Z.
    Eotv Os Univ, Budapest, Hungary..
    Blain, A.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Callanan, P.
    Univ Coll Cork, Dept Phys, Cork, Ireland..
    Covino, S.
    Brera Astron Observ, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy..
    Ferrara, A.
    Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy.;Univ Tokyo, Kavli IPMU, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan..
    Le Floch, E.
    Univ Paris Saclay, IRFU, CEA, Dept Astrophys, F-91191 Gif Sur Yvette, France..
    Marisaldi, M.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Mereghetti, S.
    IASF Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Rosati, P.
    Univ Ferrara, Via Saragat 1, Ferrara, Italy..
    Vacchi, A.
    INFN Trieste, Via Valerio 2, Trieste, Italy..
    D'Avanzo, P.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Giommi, P.
    Italian Space Agcy, ASI, Via Politecn Snc, I-00133 Rome, Italy..
    Piranomonte, S.
    Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy..
    Piro, L.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Reglero, V
    Univ Valencia, Image Proc Lab, C Catedrat Jose Beltran 2, Valencia 46980, Spain..
    Rossi, A.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Santangelo, A.
    Eberhard Karls Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Abt Hochenergieastrophys, Sand 1, D-72076 Tubingen, Germany..
    Salvaterra, R.
    Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Tagliaferri, G.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Vergani, S.
    PSL Res Univ, Observ Paris, CNRS, GEPI, Pl Jules Janssen, F-92190 Meudon, France.;Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy..
    Vinciguerra, S.
    Univ Birmingham, Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England.;Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England..
    Briggs, M.
    Univ Alabama, Ctr Space Plasma & Aeron Res, 320 Sparkman Dr, Huntsville, AL 35805 USA..
    Campolongo, E.
    OHB Italia, Via Gallarate 150, I-20151 Milan, Italy..
    Ciolfi, R.
    Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy.;Trento Inst Fundamental Phys & Applicat, INFN TIFPA, Via Sommarive 14, I-38123 Trento, Italy..
    Connaughton, V
    Univ Space Res Assoc, NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA..
    Cordier, B.
    Univ Paris Saclay, IRFU, CEA, Dept Astrophys, F-91191 Gif Sur Yvette, France..
    Morelli, B.
    OHB Italia, Via Gallarate 150, I-20151 Milan, Italy..
    Orlandini, M.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Adami, C.
    Aix Marseille Univ, LAM, CNRS, F-13388 Marseille, France..
    Argan, A.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Atteia, J-L
    Univ Toulouse, UPS, CNRS, CNES,IRAP, Toulouse, France..
    Auricchio, N.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Balazs, L.
    MTA CSFK Konkoly Observ, Konkoly Thege Mut 13-17, H-1121 Budapest, Hungary..
    Baldazzi, G.
    INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.;Univ Bologna, Dept Phys, Viale Berti Pichat 6-2, I-40127 Bologna, Italy..
    Basa, S.
    Aix Marseille Univ, LAM, CNRS, F-13388 Marseille, France..
    Basak, Rupal
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
    Bellutti, P.
    FBK, Via Sommarive 18, I-38123 Povo, Trento, Italy..
    Bernardini, M. G.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Bertuccio, G.
    Politecn Milan, Via Anzani 42, I-22100 Como, Italy.;INFN Milano, Via Celoria 16, I-20133 Milan, Italy..
    Braga, J.
    INPE, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil..
    Branchesi, M.
    Univ Urbino Carlo Bo, Via A Saffi 2, I-61029 Urbino, Italy.;INFN, Sez Firenze, Via G Sansone 1, I-50019 Sesto Fiorentino, Italy..
    Brandt, S.
    DTU Space Natl Space Inst Elektrovej, Bldg 327, DK-2800 Lyngby, Denmark..
    Brocato, E.
    INAF Astron Teramo, I-64100 Teramo, Italy..
    Budtz-Jorgensen, C.
    DTU Space Natl Space Inst Elektrovej, Bldg 327, DK-2800 Lyngby, Denmark..
    Bulgarelli, A.
    IASF Bologna, INAF, Via Gobetti 101, I-40129 Bologna, Italy..
    Burderi, L.
    Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu Km 0-7, I-09042 Monserrato, Italy..
    Camp, J.
    Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA..
    Capozziello, S.
    Univ Napoli Federico II, Dipartimento Fis, Via Cinthia, I-80126 Naples, Italy..
    Caruana, J.
    Univ Malta, Dept Phys, Msida 2080, Msd, Malta.;Univ Malta, Inst Space Sci & Astron, Msida 2080, Msd, Malta..
    Casella, P.
    Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy..
    Cenko, B.
    NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.;Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA..
    Chardonnet, P.
    Univ Savoie, CNRS, LAPTh, BP 110, F-74941 Annecy Le Vieux, France.;Natl Res Nucl Univ MEPhI, 31 Kashirskoe Sh, Moscow 115409, Russia..
    Ciardi, B.
    Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany..
    Colafrancesco, S.
    Univ Witwatersrand, Sch Phys, Private Bag 3, ZA-2050 Johannesburg, South Africa..
    Dainotti, M. G.
    Stanford Univ, Dept Phys & Astron, Via Pueblo Mall 382, Stanford, CA 94305 USA.;INAF OAS Bologna, Via P Gobetti 93-3, Bologna, Italy.;Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-31501 Krakow, Poland..
    D'Elia, V
    Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.;Agenzia Spaziale Italiana, SSDC, Via Politecn Snc, I-00133 Rome, Italy..
    De Martino, D.
    Capodimonte Astron Observ Naples, INAF, Via Moiariello 16, I-80131 Naples, Italy..
    De Pasquale, M.
    Istanbul Univ, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey..
    Del Monte, E.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Della Valle, M.
    Osserv Astron Capodimonte, INAF, Salita Moiariello 16, I-80131 Naples, Italy.;Int Ctr Relativist Astrophys, Piazzale Repubbl 2, I-65122 Pescara, Italy..
    Drago, A.
    INFN, Via Enrico Fermi 40, Frascati, Italy..
    Evangelista, Y.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Feroci, M.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Finelli, F.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Fiorini, M.
    Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Fynbo, J.
    Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark..
    Gal-Yam, A.
    Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel..
    Gendre, B.
    Univ Virgin Isl, 2 John Brewers Bay, St Thomas, VI 00802 USA.;Etelman Observ, Bonne Resolut, St Thomas, VI USA..
    Ghisellini, G.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Grado, A.
    Capodimonte Astron Observ Naples, INAF, Via Moiariello 16, I-80131 Naples, Italy..
    Guidorzi, C.
    Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy..
    Hafizi, M.
    Univ Tirana, Dept Phys, Tirana, Albania..
    Hanlon, L.
    Univ Coll Dublin, Sch Phys, Space Sci Grp, Dublin 4, Ireland..
    Hjorth, J.
    Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark..
    Izzo, L.
    CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain..
    Kiss, L.
    Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklosut 15-17, H-1121 Budapest, Hungary..
    Kumar, P.
    Univ Texas Austin, Dept Astron, Austin, TX 78712 USA..
    Kuvvetli, I
    DTU Space Natl Space Inst Elektrovej, Bldg 327, DK-2800 Lyngby, Denmark..
    Lavagna, M.
    Politecn Milan, Via La Masa 1, I-20156 Milan, Italy..
    Li, T.
    Tsinghua Univ, Dept Engn Phys, Beijing, Peoples R China.;Tsinghua Univ, Ctr Astrophys, Beijing, Peoples R China..
    Longo, F.
    INFN Trieste, Via Valerio 2, Trieste, Italy.;Univ Trieste, Dept Phys, Via Valerio 2, Trieste, Italy..
    Lyutikov, M.
    Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA.;McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.;McGill Univ, McGill Space Inst, 3600 Univ St, Montreal, PQ H3A 2T8, Canada..
    Maio, U.
    Leibniz Inst Astrophys, Sternwarte 16, D-14482 Potsdam, Germany.;Osserv Astron Trieste, INAF, Via G Tiepolo 11, I-34131 Trieste, Italy..
    Maiorano, E.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Malcovati, P.
    Univ Pavia, Dept Elect Comp & Biomed Engn, Pavia, Italy..
    Malesani, D.
    Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark..
    Margutti, R.
    Northwestern Univ, CIERA, Evanston, IL 60208 USA.;Northwestern Univ, Dept Phys & Astrophys, Evanston, IL 60208 USA..
    Martin-Carrillo, A.
    Univ Coll Dublin, Sch Phys, Space Sci Grp, Dublin 4, Ireland..
    Masetti, N.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy.;Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile..
    McBreen, S.
    Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland..
    Mignani, R.
    Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy.;Univ Zielona Gora, Janusz Gil Inst Astron, Lubuska 2, PL-65265 Zielona Gora, Poland..
    Morgante, G.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Mundell, C.
    Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England..
    Nargaard-Nielsen, H. U.
    DTU Space Natl Space Inst Elektrovej, Bldg 327, DK-2800 Lyngby, Denmark..
    Nicastro, L.
    Inst Astrofis Spaziale & Fis Cosm, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Palazzi, E.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Paltani, S.
    Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland..
    Panessa, F.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Pareschi, G.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Pe'er, A.
    Univ Coll Cork, Dept Phys, Cork, Ireland..
    Penacchioni, A. , V
    Pian, E.
    Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy..
    Piedipalumbo, E.
    Univ Napoli Federico II, Dipartimento Fis, Compl Univ Monte S Angelo, I-80126 Naples, Italy.;INFN, Sez Napoli, Univ Monte S Angelo,Edificio 6,Via Cinthia, I-80126 Naples, Italy..
    Piran, T.
    Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel..
    Rauw, G.
    Univ Liege, Quartier Agora, Allee 6 Aout 19c, B-4000 Liege, Belgium..
    Razzano, M.
    Univ Pisa, Dept Phys, I-56127 Pisa, Italy.;INFN Pisa, I-56127 Pisa, Italy..
    Read, A.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Rezzolla, L.
    Goethe Univ Frankfurt, Inst Theoret Phys, Max von Laue Str 1, D-60438 Frankfurt, Germany.;Frankfurt Inst Adv Studies, Ruth Moufang Str 1, D-60438 Frankfurt, Germany..
    Romano, P.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy..
    Ruffini, R.
    ICRANet, Pzza Repubbl 10, I-65122 Pescara, Italy.;Sapienza Univ Roma, ICRA, Ple Aldo Moro 5, I-00185 Rome, Italy.;Sapienza Univ Roma, Dipartimento Fis, Ple Aldo Moro 5, I-00185 Rome, Italy..
    Savaglio, S.
    Univ Calabria, Phys Dept, Via P Bucci, I-87036 Arcavacata Di Rende, Italy..
    Sguera, V
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Schady, P.
    Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany..
    Skidmore, W.
    Thirty Meter Telescope Int Observ, 100 W Walnut St,Suite 300, Pasadena, CA 91124 USA..
    Song, L.
    Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China..
    Stanway, E.
    Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England..
    Starling, R.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England.;Univ Leicester, Leicester Inst Space & Earth Observat, Univ Rd, Leicester LE1 7RH, Leics, England..
    Topinka, M.
    Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin 2, Ireland..
    Troja, E.
    Univ Maryland, Dept Astron, College Pk, MD 20742 USA.;NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA..
    van Putten, M.
    Sejong Univ, 98 Gunja Dong, Seoul 143747, South Korea..
    Vanzella, E.
    Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy..
    Vercellone, S.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy..
    Wilson-Hodge, C.
    NASA, Marshall Space Flight Ctr, Huntsville, AL USA..
    Yonetoku, D.
    Kanazawa Univ, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan..
    Zampa, G.
    INFN Trieste, Via Valerio 2, Trieste, Italy..
    Zampa, N.
    INFN Trieste, Via Valerio 2, Trieste, Italy..
    Zhang, B.
    Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA..
    Zhang, B. B.
    CSIC, IAA, POB 03004, E-18080 Granada, Spain..
    Zhang, S.
    Inst High Energy Phys, Beijing 100049, Peoples R China..
    Zhang, S-N
    Inst High Energy Phys, Beijing 100049, Peoples R China..
    Antonelli, A.
    ASDC, Via Politecn Snc, I-00133 Rome, Italy..
    Bianco, F.
    NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA..
    Boci, S.
    Univ Tirana, Dept Phys, Tirana, Albania..
    Boer, M.
    Univ Cote dAzur, Observ Cote dAzur, ARTEMIS, CNRS UMR 5270,CS 34229, Blvd Observ, F-06304 Nice 04, France..
    Botticella, M. T.
    Capodimonte Astron Observ Naples, INAF, Via Moiariello 16, I-80131 Naples, Italy..
    Boulade, O.
    Univ Paris Saclay, IRFU, CEA, Dept Astrophys, F-91191 Gif Sur Yvette, France..
    Butler, C.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    Campana, S.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Capitanio, F.
    IAPS Roma, INAF, Via Fosso Cavaliere 100, I-00133 Rome, Italy..
    Celotti, A.
    Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy.;SISSA, Via Bonomea 265, I-34136 Trieste, Italy.;INFN, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy..
    Chen, Y.
    Inst High Energy Phys, Beijing 100049, Peoples R China..
    Colpi, M.
    Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy.;INFN, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy..
    Comastri, A.
    Osservatorio Astron Bologna, INAF, Via Piero Gobetti 93-3, I-40129 Bologna, Italy..
    Cuby, J-G
    LAM, F-13388 Marseille, France..
    Dadina, M.
    IASF Bologna, INAF, via P Gobetti 101, I-40129 Bologna, Italy..
    De Luca, A.
    Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Dong, Y-W
    Inst High Energy Phys, Beijing 100049, Peoples R China..
    Ettori, S.
    INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.;Osservatorio Astron Bologna, INAF, Via Piero Gobetti 93-3, I-40129 Bologna, Italy..
    Gandhi, P.
    Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England..
    Geza, E.
    Hungarian Acad Sci, Wigner Res Ctr Phys, POB 49, H-1525 Budapest, Hungary..
    Greiner, J.
    Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany..
    Guiriec, S.
    Univ Maryland, Dept Astron, College Pk, MD 20742 USA.;George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.;NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.;CRESST, Greenbelt, MD 20771 USA..
    Harms, J.
    Univ Urbino Carlo Bo, I-61029 Urbino, Italy..
    Hernanz, M.
    CSIC, Inst Space Sci IEEC, Carrer Can Magrans S-N, E-08193 Barcelona, Spain..
    Hornstrup, A.
    DTU Space Natl Space Inst Elektrovej, Bldg 327, DK-2800 Lyngby, Denmark..
    Hutchinson, I
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Israel, G.
    Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy..
    Jonker, P.
    SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.;Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands..
    Kaneko, Y.
    Sabanc Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey..
    Kawai, N.
    Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan..
    Wiersema, K.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Korpela, S.
    Univ Helsinki, Dept Phys, POB 48, FIN-00014 Helsinki, Finland..
    Lebrun, V
    LAM, F-13388 Marseille, France..
    Lu, F.
    Inst High Energy Phys, Beijing 100049, Peoples R China..
    MacFadyen, A.
    NYU, Ctr Cosmol & Particle Phys, New York, NY USA..
    Malaguti, G.
    IASF Bologna, INAF, Via Piero Gobetti 101, I-40129 Bologna, Italy..
    Maraschi, L.
    Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy..
    Melandri, A.
    Osserv Astron Brera, INAF, Via E Bianchi 36, I-23807 Merate, LC, Italy..
    Modjaz, M.
    NYU, Ctr Cosmol & Particle Phys, Dept Phys, 726 Broadway Off 1044, New York, NY 10003 USA..
    Morris, D.
    Etelman Observ, St Thomas, VI 00802 USA.;Univ Virgin Isl, Coll Sci & Math, St Thomas, VI 00802 USA..
    Omodei, N.
    Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.;Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA..
    Paizis, A.
    IASF Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Pata, P.
    Czech Tech Univ, Fac Elect Engn, Dept Radioelect, Tech 2, Prague 16627 6, Czech Republic..
    Petrosian, V
    Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.;Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA..
    Rachevski, A.
    INFN, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy..
    Rhoads, J.
    Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.;Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA..
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
    Sabau-Graziati, L.
    INTA, Div Ciencias Espacio, Madrid, Spain..
    Shigehiro, N.
    RIKEN, ABBL, Wako, Saitama 3510198, Japan..
    Sims, M.
    Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England..
    Soomin, J.
    CSIC, IAA, Glorieta Astron S-N, E-18008 Granada, Spain..
    Szecsi, D.
    Univ Birmingham, Inst Gravitat Wave Astron, Birmingham B15 2TT, W Midlands, England.;Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.;Czech Acad Sci, Astron Inst, Frivcova 298, Ondvrejov 25165, Czech Republic..
    Urata, Y.
    Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan..
    Uslenghi, M.
    IASF Bologna, INAF, Via E Bassini 15, I-20133 Milan, Italy..
    Valenziano, L.
    IASF Bologna, INAF, Via Gobetti 101, Bologna, Italy..
    Vianello, G.
    Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA..
    Vojtech, S.
    Acad Sci Czech Republ, Astron Inst, Fricova 1, CZ-25165 Ondrejov, Czech Republic..
    Watson, D.
    Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark..
    Zicha, J.
    Czech Tech Univ, Fac Mech Engn, Dept Instrumentat & Control Engn, Tech 4, Prague 16607 6, Czech Republic..
    The THESEUS space mission concept: science case, design and expected performances2018In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 62, no 1, p. 191-244Article in journal (Refereed)
    Abstract [en]

    THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1 sr) with 0.5-1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift similar to 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s/early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).

  • 3.
    Bagherbandi, Mohammad
    et al.
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geoinformatik och Geodesi.
    Eshagh, Mehdi
    Recovery of Moho's undulations based on the Vening Meinesz-Moritz theory from satellite gravity gradiometry data: A simulation study2012In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 49, no 6, p. 1097-1111Article in journal (Refereed)
    Abstract [en]

    In the gravimetric approach to determine the Moho depth an isostatic hypothesis can be used. The Vening Meinesz-Moritz isostatic hypothesis is the recent theory for such a purpose. Here, this theory is further developed so that the satellite gravity gradiometry (SGG) data are used for recovering the Moho depth through a nonlinear integral inversion procedure. The kernels of its forward and inverse problems show that the inversion should be done in a larger area by 5 than the desired one to reduce the effect of the spatial truncation error of the integral formula. Our numerical study shows that the effect of this error on the recovered Moho depths can reach 6 km in Persia and it is very significant. The iterative Tikhonov regularization in a combination with either generalized cross validation or quasi-optimal criterion of estimating the regularization parameter seems to be suitable and the solution is semi-convergent up to the third iteration. Also the Moho depth recovered from the simulated SGG data will be more or less the same as that obtained from the terrestrial gravimetric data with a root mean square error of 2 km and they are statistically consistent.

  • 4.
    Blomberg, Lars G.
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Cumnock, Judy A.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Kasaba, Y.
    Matsumoto, H.
    Kojima, H.
    Omura, Y.
    Moncuquet, M.
    Wahlund, J. -E
    Electric fields in the Hermean environment2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 4, p. 627-631Article in journal (Refereed)
    Abstract [en]

    Returning to Mercury with the BepiColombo mission will provide a unique opportunity to obtain in situ information on the electric field in Mercury's magnetosphere. The electric field plays a crucial role for plasma transport in the magnetosphere, for transfer of energy between different parts of the system, and for propagation of information. Measuring the electric field, we will be able to better understand plasma motion and wave propagation in Mercury's magnetosphere. Together with knowledge of the magnetic field a better understanding will be derived of the magnetospheric current systems and their closure at or near the planetary surface. Further, insight into possible substorms at Mercury will be gained. We here focus on the expected amplitudes and frequencies of the electric fields concerned and the requirements for instrument capability that they pose.

  • 5.
    Blomberg, Lars G.
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Matsumoto, H.
    Bougeret, J. -L
    Kojima, H.
    Yagitani, S.
    Cumnock, Judy A.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Eriksson, A. I.
    Marklund, Göran T.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Wahlund, J. -E
    Bylander, Lars
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Åhlen, L.
    Holtet, J. A.
    Ishisaka, K.
    Kallio, E.
    Kasaba, Y.
    Matsuoka, A.
    Moncuquet, M.
    Mursula, K.
    Omura, Y.
    Trotignon, J. G.
    MEFISTO - An electric field instrument for BepiColombo/MMO2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 4, p. 672-679Article in journal (Refereed)
    Abstract [en]

    MEFISTO, together with the companion instrument WPT, are planning the first-ever in situ measurements of the electric field in the magnetosphere of planet Mercury. The instruments have been selected by JAXA for inclusion in the BepiColombo/MMO payload, as part of the Plasma Wave Investigation coordinated by Kyoto University. The magnetosphere of Mercury was discovered by Mariner 10 in 1974 and will be studied further by Messenger starting in 2011. However, neither spacecraft did or will measure the electric field. Electric fields are crucial in the dynamics of a magnetosphere and for the energy and plasma transport between different regions within the magnetosphere as well as between the magnetosphere and the surrounding regions. The MEFISTO instrument will be capable of measuring electric fields from DC to 3 MHz, and will thus also allow diagnostics of waves at all frequencies of relevance to the Hermean magnetosphere. MEFISTO is a double-probe electric field instrument. The double-probe technique has strong heritage and is well proven on missions such as Viking, Polar, and Cluster. For BepiColombo, a newly developed deployment mechanism is planned which reduces the mass by a factor of about 5 compared to conventional mechanisms for 15 in long booms. We describe the basic characteristics of the instrument and briefly discuss the new developments made to tailor the instrument to flight in Mercury orbit.

  • 6. Bruno, A.
    et al.
    Adriani, O.
    Barbarino, G. C.
    Bazilevskaya, G. A.
    Bellotti, R.
    Boezio, M.
    Bogomolov, E. A.
    Bongi, M.
    Bonvicini, V.
    Bottai, S.
    Cafagna, F.
    Campana, D.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Casolino, M.
    Castellini, G.
    Christian, E. C.
    De Donato, C.
    de Nolfo, G. A.
    De Santis, C.
    De Simone, N.
    Di Felice, V.
    Galper, A. M.
    Karelin, A. V.
    Koldashov, S. V.
    Koldobskiy, S.
    Krutkov, S. Y.
    Kvashnin, A. N.
    Leonov, A.
    Malakhov, V.
    Marcelli, L.
    Martucci, M.
    Mayorov, A. G.
    Menn, W.
    Merge, M.
    Mikhailov, V. V.
    Mocchiutti, E.
    Monaco, A.
    Mori, N.
    Munini, R.
    Osteria, G.
    Palma, F.
    Panico, B.
    Papini, P.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Picozza, P.
    Ricci, M.
    Ricciarini, S. B.
    Ryan, J. M.
    Sarkar, R.
    Scotti, V.
    Simon, M.
    Sparvoli, R.
    Spillantini, P.
    Stochaj, S.
    Stozhkov, Y. I.
    Vacchi, A.
    Vannuccini, E.
    Vasilyev, G. I.
    Voronov, S. A.
    Yurkin, Y. T.
    Zampa, G.
    Zampa, N.
    Geomagnetically trapped, albedo and solar energetic particles: Trajectory analysis and flux reconstruction with PAMELA2017In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 60, no 4, p. 788-795Article in journal (Refereed)
    Abstract [en]

    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. PAMELA's measurements are supported by an accurate analysis of particle trajectories in the Earth's magnetosphere based on a realistic geomagnetic field modeling, which allows the classification of particle populations of different origin and the investigation of the asymptotic directions of arrival.

  • 7.
    Capel, Francesca
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. The Oskar Klein Centre for Cosmoparticle Physics, Stockholm.
    Belov, A.
    Casolino, M.
    Klimov, P.
    Mini-EUSO: A high resolution detector for the study of terrestrial and cosmic UV emission from the International Space Station2017In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948Article in journal (Refereed)
    Abstract [en]

    The Mini-EUSO instrument is a UV telescope to be placed inside the International Space Station (ISS), looking down on the Earth from a nadir-facing window in the Russian Zvezda module. Mini-EUSO will map the earth in the UV range (300-400. nm) with a spatial resolution of 6.11. km and a temporal resolution of 2.5. μs, offering the opportunity to study a variety of atmospheric events such as transient luminous events (TLEs) and meteors, as well as searching for strange quark matter and bioluminescence. Furthermore, Mini-EUSO will be used to detect space debris to verify the possibility of using a EUSO-class telescope in combination with a high energy laser for space debris remediation. The high-resolution mapping of the UV emissions from Earth orbit allows Mini-EUSO to serve as a pathfinder for the study of Extreme Energy Cosmic Rays (EECRs) from space by the JEM-EUSO collaboration. 

  • 8. Casolino, M.
    et al.
    Bidoll, V.
    Minori, M.
    Narici, L.
    De Pascale, M. P.
    Picozza, P.
    Reall, E.
    Zaconte, V.
    Fuglesang, Christer
    Vittori, R.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Galper, A.
    Korotkov, M.
    Popov, A.
    Vavilov, N.
    Avdeev, S.
    Berighin, V.
    Petrov, V. P.
    Salnitskii, V. P.
    Shevchenko, O. I.
    Trukhanov, K. A.
    Shurshakov, K. A.
    Boezio, M.
    Bonvicini, W.
    Vacchi, A.
    Zampa, G.
    Zarnpa, N.
    Mazzenga, G.
    Ricci, M.
    Spillantini, P.
    Relative nuclear abundances inside ISS with Sileye-3/Alteino experiment2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 37, no 9, p. 1685-1690Article in journal (Refereed)
    Abstract [en]

    The experiment Sileye-3/Alteino was first operational on board the international Space Station between 27/4 and 1/5/2002. It is constituted of a cosmic ray silicon detector and an electroencephalograph and is used to monitor radiation environment and study the light flash phenomenon in space. As a stand-alone device, Sileye-3/Alteino can monitor in real time cosmic ray nuclei. In this work, we report on relative nuclear abundance measurements in different regions of the orbit for nuclei from B to Fe in the energy range above similar or equal to 60 Mev/n. Abundances of nuclei such as 0 and Ne relative to C are found to be increased in respect to particle composition outside of the station, whereas the Fe group is reduced. This effect could be ascribed to nuclear interactions with the hull of the station.

  • 9. Casolino, M.
    et al.
    Picozza, P.
    Altamura, F.
    Basili, A.
    De Simone, N.
    Di Felice, V.
    De Pascale, M. P.
    Marcelli, L.
    Minori, M.
    Nagni, M.
    Sparvoli, R.
    Galper, A. M.
    Mikhailov, V. V.
    Runtso, M. F.
    Voronov, S. A.
    Yurkin, Y. T.
    Zverev, V. G.
    Castellini, G.
    Adriani, O.
    Bonechi, L.
    Bongi, M.
    Taddei, E.
    Vannuccini, E.
    Fedele, D.
    Papini, P.
    Ricciarini, S. B.
    Spillantini, P.
    Ambriola, M.
    Cafagna, F.
    De Marzo, C.
    Barbarino, G. C.
    Campana, D.
    De Rosa, G.
    Osteria, G.
    Russo, S.
    Bazilevskaja, G. A.
    Kvashnin, A. N.
    Maksumov, O.
    Misin, S.
    Stozhkov, Yu. I.
    Bogomolov, E. A.
    Krutkov, S. Yu.
    Nikonov, N. N.
    Bonvicini, V.
    Boezio, M.
    Lundquist, J.
    Mocchiutti, E.
    Vacchi, A.
    Zampa, G.
    Zampa, N.
    Bongiorno, L.
    Ricci, M.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Hofverberg, Petter
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Lund, Jens
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Orsi, Silvio
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Menn, W.
    Simon, M.
    Launch of the space experiment PAMELA2008In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 42, no 3, p. 455-466Article in journal (Refereed)
    Abstract [en]

    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-DK I satellite, was launched on June 15th, 2006 in a 350 x 600 km orbit with all inclination of 70'. The detector is composed of a series of scintillator counters arranged at the extremities of a permanent magnet spectrometer to provide charge, time-of-flight, and rigidity information. Lepton/hadron identification is performed by a silicon-tungsten calorimeter and a neutron detector placed at the bottom of the device. An anticounter system is used offline to reject false triggers coming from the satellite. In self-trigger mode the calorimeter, the neutron detector, and a shower tail catcher are capable of an independent measure of the lepton component up to 2 TeV. In this work we describe the experiment, its scientific objectives, and the performance in the first months after launch.

  • 10.
    Cumnock, Judy A.
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics. KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics. KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
    Alexeev, I. I.
    Belenkaya, E. S.
    Bobrovnikov, S. Yu.
    Kalegaev, V. V.
    Simultaneous polar aurorae and modelled convection patterns in both hemispheres2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 8, p. 1685-1693Article in journal (Refereed)
    Abstract [en]

    We present an event study illustrating the relationships between plasma convection and polar auroral emissions, as well as illustrating the influence of the interplanetary magnetic field's y-component on theta aurora development in both hemispheres. Transpolar arcs (TPAs) are often observed during northward IMF with duskside (dawnside) formation of the TPA and dawnward (duskward) motion occurring when B-y changes from positive to negative in the northern (southern) hemisphere. POLAR UVI provides images in the northern hemisphere while DMSP provides ionospheric plasma flow and precipitating particle data in both hemispheres. Concurrent solar wind plasma and interplanetary magnetic field measurements are provided by the ACE satellite. Utilizing the satellite data as inputs, the Royal Institute of Technology (KTH) numerical model provides the high-latitude ionospheric electrostatic potential patterns in both hemispheres calculated at different times during the evolution of the theta aurora resulting from a variety of field-aligned current configurations associated with the changing global aurora. These model patterns are compared to the convection predicted by mapping the magnetopause electric field to the ionosphere using the Moscow State University's (MSU) paraboloid model of the magnetosphere. The model predicts that parallel electric fields are set up along the magnetic field lines projecting to the transpolar aurora. Their possible role in the acceleration of the auroral electrons is discussed.

  • 11.
    Ekbom, Lars B
    et al.
    KTH, Superseded Departments, Materials Science and Engineering.
    Eliasson, Anders
    KTH, Superseded Departments, Materials Science and Engineering.
    Liquid Phase Sintering of Tungsten Composites in Space: Results of Tests Performed in Texus1988In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 8, no 12, p. 315-319Article in journal (Refereed)
  • 12.
    Eriksson, Tommy
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Blomberg, Lars
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Glassmeier, K.-H.
    Institute for Geophysics and Extraterrestrial Physics, Technical University of Braunschweig, Tyskland.
    Cluster satellite observations of mHz pulsations in the dayside magnetosphere2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 8, p. 1730-1737Article in journal (Refereed)
    Abstract [en]

    On 17 August 2002 the Cluster spacecraft moved through the dayside magnetosphere. Between 16:00 and 18:30 LIT clear monochromatic oscillations are seen in both electric field and magnetometer data. The frequency is 4.2 mHz in the spacecraft frame of reference. The oscillations have a clear spatial localisation. The magnetic field oscillations are radially polarised in the plane perpendicular to the background magnetic field, indicating that the wave is in the poloidal mode. From the difference in phase between the satellites we estimate the azimuthal wave number, in, to be about 130, consistent with the magnetic field polarisation. The frequency is stable for different L-values as well as over time. From the value of in, the Doppler shift due to satellite motion is estimated to 0.5 mHz. By looking at the phase of the electric and the magnetic field close to the equator we conclude that the oscillations are in a mode with an odd number of half wavelengths between the two ionospheres.

  • 13.
    Eriksson, Tommy
    et al.
    KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
    Walker, A. D. M.
    School of Pure and Applied Physics, University of KwaZulu-Natal, Durban, South Africa.
    Stephenson, J. A. E.
    School of Pure and Applied Physics, University of KwaZulu-Natal, Durban, South Africa.
    A statistical correlation of Pc5 pulsations and solar wind pressure oscillations2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 8, p. 1763-1771Article in journal (Refereed)
    Abstract [en]

    The SHARE high frequency (HF) radar in Antarctica is used to compare ionospheric plasma flow oscillations in the Pc5 frequency range with low-frequency oscillations in the solar wind pressure measured by the ACE spacecraft. Ten different days in 2000 and 2001 are analysed with respect to different frequencies and geomagnetic latitudes. Both data sets are bandpass filtered and a complex demodulation technique is used to calculate the correlation in each band. On a number of occasions the wave packet structure of the Pc5 pulsations is in good or excellent agreement with the wave packet structure of the solar wind pressure oscillations. This strongly suggests that the oscillations were directly driven by the solar wind. Particularly good correlation is found in the frequency band 0.8-1.2 mHz. Pulsations in this frequency range are hard to reconcile with the magnetospheric cavity mode model. We conclude that, at least on some occasions, Pc5 pulsations may be directly driven and the magnetosphere cavity/waveguide then assumes a more passive role.

  • 14.
    Eshagh, Mehdi
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geoinformatik och Geodesi.
    Inversion of satellite gradiometry data using statistically modified integral formulas for local gravity field recovery2011In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 47, no 1, p. 74-85Article in journal (Refereed)
    Abstract [en]

    The satellite gravity gradiometric data can be used directly to recover the gravity anomaly at sea level using inversion of integral formulas. This approach suffers by the spatial truncation errors of the integrals, but these errors can be reduced by modifying the formulas. It allows us to consider smaller coverage of the satellite data over the region of recovery. In this study, we consider the second-order radial derivative (SORD) of disturbing potential (T-rr) and determine the gravity anomaly with a resolution of 1 degrees x 1 degrees at sea level by inverting the statistically modified version of SORD of extended Stokes' formula. Also we investigate the effect of the spatial truncation error on the quality of inversion considering noise of T-rr. The numerical investigations show satisfactory results when the area of T-rr coverage is the same with that of the gravity anomaly and the integral formula is modified by the biased least-squares modification. The error of recovery will be about 6 mGal after removing the regularization bias in the presence of 1 mE noise in T-rr measured on the orbit. (c) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.

  • 15.
    Eshagh, Mehdi
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geoinformatik och Geodesi.
    Semi-stochastic modification of second-order radial derivative of Abel-Poisson's formula for validating satellite gravity gradiometry data2011In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 47, no 4, p. 757-767Article in journal (Refereed)
    Abstract [en]

    The geoid can be used to validate the satellite gravity gradiometry data. Validation of such data is important prior to their downward continuation because of amplification of the data errors through this process. In this paper, the second-order radial derivative of Abel-Poisson's formula is modified stochastically to reduce the effect of the far-zone geoid and generate the second-order radial derivative of geopotential at 250 km level. The numerical studies over Fennoscandia show that this method yields the gradients with an error of 10 mE and when the long wavelength of geoid is removed from the estimator and restored after the computations (remove compute restore) the error will be in 1 mE level. We name this method semi-stochastic modification. The best case scenario is found when the degree of modification of the integral formula is 200 and the long wavelength geoid to degree 100 is removed and restored. In this case the geoid should have a resolution of 15' x 15' and the integration should be performed over a cap size of 3 degrees.

  • 16.
    Eshagh, Mehdi
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geoinformatik och Geodesi.
    The effect of spatial truncation error on integral inversion of satellite gravity gradiometry data2011In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 47, no 7, p. 1238-1247Article in journal (Refereed)
    Abstract [en]

    The satellite gravity gradiometry (SGG) data can be used for local modelling of the Earth's gravity field. In this study, the SGG data in the local north-oriented and orbital frames are inverted to the gravity anomaly at sea level using the second-order partial derivatives of the extended Stokes formula. The emphasis is on the spatial truncation error and the kernel behaviour of the integral formulas in the aforementioned frames. The paper will show that only the diagonal elements of gravitational tensor at satellite level are suitable for recovering the gravity anomaly at sea level. Numerical studies show that the gravity anomaly can be recovered in Fennoscandia with an accuracy of about 6 mGal directly from on-orbit SGG data.

  • 17.
    Eshagh, Mehdi
    et al.
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geodesy and Geoinformatics.
    Ghorbannia, Morteza
    The use of Gaussian equations of motions of a satellite for local gravity anomaly recovery2013In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 52, no 1, p. 30-38Article in journal (Refereed)
    Abstract [en]

    The orbital elements of a low Earth orbiting satellite and their velocities can be used for local determination of gravity anomaly. The important issue is to find direct relations among the anomalies and these parameters. Here, a primary theoretical study is presented for this purpose. The Gaussian equations of motion of a satellite are used to develop integral formulas for recovering the gravity anomalies. The behaviour of kernels of the integrals are investigated for a two-month simulated orbit similar to that of the Gravity field and steady-state ocean circulation explorer (GOCE) mission over Fennoscandia. Numerical investigations show that the integral formulas have neither isotropic nor well-behaved kernels. In such a case, gravity anomaly recovery is not successful due to large spatial truncation error of the integral formulas. Reformulation of the problem by combining the orbital elements and their velocities leads to an integral with a well-behaved kernel which is suitable for our purpose. Also based on these combinations some general relations among the orbital elements and their velocities are obtained which can be used for validation of orbital parameters and their velocities. (C) 2013 COSPAR.

  • 18.
    Eshagh, Mehdi
    et al.
    KTH, School of Architecture and the Built Environment (ABE), Urban Planning and Environment, Geoinformatik och Geodesi.
    Romeshkani, Mohsen
    Department of Geodesy, KNToosi Uni. Tech..
    Generation of vertical–horizontal and horizontal–horizontal gravity gradients using stochastically modified integral estimators2011In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 48, no 8, p. 1341-1358Article in journal (Refereed)
    Abstract [en]

    The Earth’s gravity field modelling is an ill-posed problem having a sensitive solution to the error of data. Satellite gravity gradiometry (SGG) is a space technique to measure the second-order derivatives of geopotential for modelling this field, but the measurements should be validated prior to use. The existing terrestrial gravity anomalies and Earth gravity models can be used for this purpose. In this paper, the second-order vertical–horizontal (VH) and horizontal–horizontal (HH) derivatives of the extended Stokes formula in the local north-oriented frame are modified using biased, unbiased and optimum types of least-squares modification. These modified integral estimators are used to generate the VH and HH gradients at 250 km level for validation purpose of the SGG data. It is shown that, unlike the integral estimator for generating the second-order radial derivative of geopotential, the system of equations from which the modification parameters are obtained is unstable for all types of modification, with large cap size and high degree, and regularization is strongly required for solving the system. Numerical studies in Fennoscandia show that the SGG data can be estimated with an accuracy of 1 mE using an integral estimator modified by a biased type least-squares modification. In this case an integration cap size of 2.5° and a degree of modification of 100 for integrating 30′ × 30′ gravity anomalies are required.

  • 19.
    Ivchenko, Nickolay V.
    et al.
    KTH, Superseded Departments, Alfvén Laboratory.
    Marklund, Göran T.
    KTH, Superseded Departments, Alfvén Laboratory.
    Current singularities observed on Astrid-22002In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 30, no 7, p. 1779-1782Article in journal (Refereed)
    Abstract [en]

    Swedish microsatellite Astrid-2 carried out,electric and magnetic field measurements at 1000 km altitude during its operation in January-July, 1999. At a number of occasions sharp gradients in the magnetic field were observed by the satellite. If interpreted as spatial gradients they imply current densities of hundreds muA/m(2). Occurrence of such 11 current singularities is studied. The nature of the events is discussed.

  • 20. Leonov, A. A.
    et al.
    Larsson, Josefin
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zverev, V. G.
    et al.,
    Separation of electrons and protons in the GAMMA-400 gamma-ray telescope2015In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 56, no 7, p. 1538-1545Article in journal (Refereed)
    Abstract [en]

    The GAMMA-400 telescope will measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. These measurements will allow it to achieve the following scientific objectives: search for signatures of dark matter, investigation of gamma-ray point-like and extended sources, study of the energy spectrum of the Galactic and extragalactic diffuse emission, study of gamma-ray bursts and gamma-ray emission from the active Sun, together with high-precision measurements of the high-energy electrons and positrons spectra, protons and nuclei up to the knee. The bulk of cosmic rays are protons and helium nuclei, whereas the lepton component in the total flux is similar to 10(-3) at high energy. In the present paper, the simulated capability of the GAMMA-400 telescope to distinguish electrons and positrons from protons in cosmic rays is addressed. The individual contribution to the proton rejection from each detector system of GAMMA-400 is studied separately. The use of the combined information from all detectors allows us to reach a proton rejection of the order of similar to 4 x 10(5) for vertical incident particles and similar to 3 x 10(5) for particles with initial inclination of 30 degrees in the electron energy range from 50 GeV to 1 TeV. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.

  • 21.
    Marklund, Göran T.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    On high-altitude electric fields in the auroral downward current region and their coupling to ionospheric electric fields2010In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 46, no 4, p. 440-448Article in journal (Refereed)
    Abstract [en]

    The downward field-aligned current region plays an active role in magnetosphere ionosphere coupling processes associated with aurora. A quasi-static electric field structure with a downward parallel electric field forms at altitudes between 800 km and 5000 km, accelerating ionospheric electrons upward, away from the auroral ionosphere. Other phenomena including energetic ion conics, electron solitary waves, low-frequency wave activity, and plasma density cavities occur in this region, which also acts as a source region for VLF saucers. Results are presented from high-altitude Cluster observations with particular emphasis on the characteristics and dynamics of quasi-static electric field structures. These, extending up to altitudes of at least 4-5 Earth radii, appear commonly as monopolar or bipolar electric fields. The former occur at sharp boundaries, such as the polar cap boundary whereas the bipolar fields occur at softer boundaries within the plasma sheet. The temporal evolution of quasi-static electric field structures, as captured by the pearls-on-a-string configuration of the Cluster spacecraft, indicates that the formation of electric field structures and of ionospheric plasma density cavities are closely coupled processes. A related feature of the downward current is a broadening of the current sheet with time, possibly related to the depletion process. Preliminary studies of the coupling of electric fields in the downward current region, show that small-scale structures are typically decoupled from the ionosphere, similar to what has been found for the upward current region. However, exceptions are also found where small-scale electric fields couple perfectly between the ionosphere and Cluster altitudes. Recent FAST results indicate that the degree of coupling differs between sheet-like and curved structures, and that it is typically partial. The electric field coupling further depends on the current-voltage relationship, which is highly non-linear in the downward current region, and still unrevealed, as to its specific form. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved.

  • 22. Menn, W.
    et al.
    Adriani, O.
    Barbarino, G. C.
    Bazilevskaya, G. A.
    Bellotti, R.
    Boezio, M.
    Bogomolov, E. A.
    Bonechi, L.
    Bongi, M.
    Bonvicini, V.
    Borisov, S.
    Bottai, S.
    Bruno, A.
    Cafagna, F.
    Campana, D.
    Carbone, R.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Casolino, M.
    Castellini, G.
    Consiglio, L.
    De Pascale, M. P.
    De Santis, C.
    De Simone, N.
    Di Felice, V.
    Galper, A. M.
    Gillard, William
    KTH, School of Engineering Sciences (SCI), Physics.
    Grishantseva, L.
    Jerse, G.
    Karelin, A. V.
    Koldashov, S. V.
    Krutkov, S. Y.
    Kvashnin, A. N.
    Leonov, A.
    Malakhov, V.
    Malvezzi, V.
    Marcelli, L.
    Mayorov, A. G.
    Mikhailov, V. V.
    Mocchiutti, E.
    Monaco, A.
    Mori, N.
    Nikonov, N.
    Osteria, G.
    Palma, F.
    Papini, P.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Picozza, P.
    Pizzolotto, C.
    Ricci, M.
    Ricciarini, S. B.
    Sarkar, R.
    Rossetto, Laura
    KTH, School of Engineering Sciences (SCI), Physics.
    Simon, M.
    Sparvoli, R.
    Spillantini, P.
    Stochaj, S. J.
    Stockton, J. C.
    Stozhkov, Y. I.
    Vacchi, A.
    Vannuccini, E.
    Vasilyev, G.
    Voronov, S. A.
    Wu, Juan
    KTH, School of Engineering Sciences (SCI), Physics.
    Yurkin, Y. T.
    Zampa, G.
    Zampa, N.
    Zverev, V. G.
    The PAMELA space experiment2013In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 51, no 2, p. 209-218Article in journal (Refereed)
    Abstract [en]

    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 is comprised of 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 to 100's GeV) with high statistics. The primary scientific goal is the measurement of the antiproton and positron energy spectra in order to search for exotic sources, such as dark matter particle annihilations. PAMELA is also searching for primordial antinuclei (anti-helium), and testing cosmic-ray propagation models through precise measurements of the antiparticle energy spectrum and precision studies of light nuclei and their isotopes. Moreover, PAMELA is investigating phenomena connected with solar and earth physics. After 4 years of operation in flight, PAMELA is now delivering coherent results about spectra and chemical composition of the charged cosmic radiation, allowing scenarios of production and propagation of cosmic rays to be fully established and understood.

  • 23. Moncuquet, M.
    et al.
    Matsumoto, H.
    Bougeret, J-L
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics. KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
    Issautier, K.
    Kasaba, Y.
    Kojima, H.
    Maksimovic, M.
    Meyer-Vernet, N.
    Zarka, P.
    The radio waves and thermal electrostatic noise spectroscopy (SORBET) experiment on BEPICOLOMBO/MMO/PWI: Scientific objectives and performance2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 4, p. 680-685Article in journal (Refereed)
    Abstract [en]

    SORBET (Spectroscopie des Ondes Radio and du Bruit Electrostatique Thermique) is a radio HF spectrometer designed for the radio and Plasma Waves Instrument onboard BepiColombo/Mercury Magnetospheric Orbiter (MMO), which performs remote and in situ measurements of waves (electromagnetic and electrostatic). Technically, SORBET includes a plasma wave spectrometer, with two E-field inputs from the two perpendicular electric antennas and one B-field input from a search coil, in the range 2.5-640 kHz. This frequency band includes the local gyrofrequency and plasma frequency expected on most part of the MMO orbits. SORBET also includes a higher frequency radio receiver for remote sensing in the range 500 kHz-10.2 MHz. Owing to its capabilities, SORBET will be able to address the following scientific objectives: High resolution mapping(similar to 30 km) of electron density and temperature in the solar wind and in the Hermean magnetosphere and exo-ionosphere, via the technique of Quasi-Thermal Noise (QTN) spectroscopy. These QTN measurements will be determinant for the dynamic modeling of the magnetosphere and will provide a fundamental input for the chemistry of cold ionized species (Na, K, O, . . .) in Mercury's environment. Detection and study of Hermean radio emissions, including possible cyclotron emissions (up to similar to 10-20 kHz) from mildly energetic electrons in most highly magnetized (polar?) regions, and possible synchrotron radiation (up to a few MHz?) from more energetic electrons. Monitoring of solar radio emissions up to similar to 10 MHz in order to create a solar activity index from the view point of Mercury, allowing to correlate it with the Hermean magnetospheric response. We especially discuss the capabilities of SORBET for performing the QTN spectroscopy in Mercury's magnetosphere, using the two electric dipole antennas equipping MMO, called MEFISTO and WPT.

  • 24.
    Orsi, Silvio
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Lund, Jens
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Lundquist, Johan
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    The anticoincidence shield of the PAMELA space experiment2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 37, no 10, p. 1853-1856Article in journal (Refereed)
    Abstract [en]

    The PAMELA space experiment will be launched in 2005 onboard a Russian Resurs DK1 satellite, orbiting Earth at an altitude varying between 300 and 600 km. The main scientific goal is a study of the antimatter component of the cosmic radiation. The semi-polar orbit (71 degrees) allows PAMELA to investigate a wide range of energies for antiprotons (80 MeV-190 GeV) and positrons (50 MeV-270 GeV). Three years of data taking will provide unprecedented statistics in this energy range and will set the upper limit for the ratio He-/He below 10(-7). PAMELA is built around a permanent magnet silicon spectrometer, surrounded by a plastic scintillator anticoincidence shield. The anticounter scintillators are used to aid in the rejection of background from particles which do not cleanly enter the acceptance of the experiment but which are responsible for coincidental energy deposits in the trigger scintillators ('false triggers'). Information from the anticounter system can be included as a veto in a second level trigger, to exclude the acquisition of events generated by such false triggers. The construction of the anticounter system is described, along with its functionality and performance. The read-out electronics and the LED-based monitoring system are also described. Test-beam and simulation studies of the system are reviewed.

  • 25. Trotignon, J. G.
    et al.
    Beghin, C.
    Lagoutte, D.
    Michau, J. L.
    Matsumoto, H.
    Kojima, H.
    Hashimoto, K.
    Kasaba, Y.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Lebreton, J. P.
    Masson, A.
    Hamelin, M.
    Pottelette, R.
    Active measurement of the thermal electron density and temperature on the Mercury Magnetospheric Orbiter of the BepiColombo mission2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 38, no 4, p. 686-692Article in journal (Refereed)
    Abstract [en]

    The thermal component of Mercury's electron population has never been measured. One scientific objective of the Plasma Wave Investigation consortium, PWI, is to determine the influence of the thermal plasma upon the formation and dynamics of the planetary magnetosphere, as a function of solar activity. The Active Measurement of Mercury's Plasma experiment, AM(2)p, has been proposed as part of PWI, to monitor the density and temperature of the thermal electron population, during the whole mission of the Mercury Magnetospheric Orbiter of BepiColombo. These two physical parameters will be deduced from the measurements of the self- and mutual-impedances of the MEFISTO (Mercury Electric Field In Situ Tool) double-sphere antenna, in a frequency range comprising the expected plasma frequency. The in situ measurement of the antenna impedance is also essential for calibrating the electric antenna which measures the natural waves; it will allow, in particular, the effective length of the antenna to be calculated as a function of frequency and plasma conditions. The purpose of this paper is to define the scientific objectives of AM(2)p, to explain the principle of the measurement, to describe the electronic device, and to show the ability of AM 2p to make reliable and accurate measurements of the thermal plasma density and temperature in the Hermean magnetosphere, as well as in the solar wind at heliocentric distances of 0.31-0.47 AU. The potential performance of this instrument has been evaluated using both an analytical approach and numerical simulations.

  • 26. Ubertini, Pietro
    et al.
    Corsi, A.
    Foley, S.
    McGlynn, Sinead
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    De Cesare, G.
    Bazzano, A.
    The INTEGRAL view of Gamma-Ray Bursts2011In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 47, no 8, p. 1374-1386Article in journal (Refereed)
    Abstract [en]

    After more than six and half years in orbit, the ESA space observatory INTEGRAL has provided new, exciting results in the soft gamma-ray energy range (from a few keV to a few MeV). With the discovery of about 700 hard X-Ray sources, it has changed our previous view of a sky composed of peculiar and "monster" sources. The new high energy sky is in fact full of a large variety of normal, very energetic emitters, characterized by new accretion and acceleration processes (see also IBIS cat4 (Bird et al., 2010). At the same time, about one GRB/month is detected and imaged by the two main gamma-ray instruments on board: IBIS and SPI. In this paper, we review the major achievements of the INTEGRAL observatory in the field of Gamma-Ray Bursts. We summarize the global properties of Gamma-Ray Bursts detected by INTEGRAL, with respect to their duration, spectral index, and peak flux distributions. We recall INTEGRAL results on the spectral lag analysis, showing how long-lag GRBs appear to form a separate population at low peak fluxes. We review the outcome of polarisation studies performed by using INTEGRAL data. Finally, concerning single GRB studies, we highlight the properties of particularly interesting Gamma-Ray Bursts in the INTEGRAL sample. 

  • 27. Usoskin, I. G.
    et al.
    Kovaltsov, G. A.
    Adriani, O.
    Barbarino, G. C.
    Bazilevskaya, G. A.
    Bellotti, R.
    Boezio, M.
    Bogomolov, E. A.
    Bongi, M.
    Bonvicini, V.
    Bottai, S.
    Bruno, A.
    Cafagna, F.
    Campana, D.
    Carbone, R.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Casolino, M.
    Castellini, G.
    De Donato, C.
    De Santis, C.
    De Simone, N.
    Di Felice, V.
    Format, V.
    Galper, A. M.
    Karelin, A. V.
    Koldashov, S. V.
    Koldobskiy, S.
    Krutkov, S. Y.
    Kvashnin, A. N.
    Leonov, A.
    Malakhov, V.
    Marcelli, L.
    Martucci, M.
    Mayorov, A. G.
    Menn, W.
    Merge, M.
    Mikhailov, V. V.
    Mocchiutti, E.
    Monaco, A.
    Mori, N.
    Munini, R.
    Osteria, G.
    Palma, F.
    Panico, B.
    Papini, P.
    Pearce, Mark
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Picozza, P.
    Pizzolotto, C.
    Ricci, M.
    Ricciarini, S. B.
    Rossetto, Laura
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Sarkar, R.
    Scotti, V.
    Simon, M.
    Sparvoli, R.
    Spillantini, P.
    Stozhkov, Y. I.
    Vacchi, A.
    Vannuccini, E.
    Vasilye, G. I.
    Voronov, S. A.
    Yurkin, Y. T.
    Zampa, G.
    Zampa, N.
    Zverev, V. G.
    Force-field parameterization of the galactic cosmic ray spectrum: Validation for Forbush decreases2015In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 55, no 12, p. 2940-2945Article in journal (Refereed)
    Abstract [en]

    A useful parametrization of the energy spectrum of galactic cosmic rays (GCR) near Earth is offered by the so-called force-field model which describes the shape of the entire spectrum with a single parameter, the modulation potential. While the usefulness of the force-field approximation has been confirmed for regular periods of solar modulation, it was not tested explicitly for disturbed periods, when GCR are locally modulated by strong interplanetary transients. Here we use direct measurements of protons and alpha-particles performed by the PAMELA space-borne instrument during December 2006, including a major Forbush decrease, in order to directly test the validity of the force-field parameterization. We conclude that (1) The force-field parametrization works very well in describing the energy spectra of protons and alpha-particles directly measured by PAMELA outside the Earths atmosphere; (2) The energy spectrum of GCR can be well parameterized by the force-field model also during a strong Forbush decrease; (3) The estimate of the GCR modulation parameter, obtained using data from the world-wide neutron monitor network, is in good agreement with the spectra directly measured by PAMELA during the studied interval. This result is obtained on the basis of a single event analysis, more events need to be analyzed.

  • 28. Vaivads, A.
    et al.
    Eriksson, A. I.
    Andre, M.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Wahlund, J. -E
    Bale, S. D.
    Low-frequency electric field and density fluctuation measurements on Solar Orbiter2007In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 39, no 9, p. 1502-1509Article in journal (Refereed)
    Abstract [en]

    Solar Orbiter will orbit the Sun down to a distance of 0.22 AU allowing detailed in situ studies of important but unexplored regions of the solar wind in combination with coordinated remote sensing of the Sun. In-situ measurements require high quality measurements of particle distributions and electric and magnetic fields. We show that such important scientific topics as the identification of coronal heating remnants, solar wind turbulence, magnetic reconnection and shock formation within coronal mass ejections all require electric field and plasma density measurements in the frequency range from DC up to about 100 Hz. We discuss how such measurements can be achieved using the double-probe technique. We sketch a few possible antenna design solutions.

  • 29. Zaconte, V.
    et al.
    Fuglesang, Christer
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Schardt, D.
    et al.,
    ALTEA: flight model calibration at GSI2006In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 37, no 9, p. 1704-1709Article in journal (Refereed)
    Abstract [en]

    The ALTEA project, an international and multi-disciplinary collaboration scheduled to fly in the International Space Station (ISS) after July 2006, is aimed at studying particle radiation in space environment and its effects on astronauts, in particular the anomalous perception of 'light flashes'. In this paper, we present experimental results obtained by testing the Flight Model of the ALTEA particle detector in two measurement sessions performed at the heavy ion accelerator of GSI laboratory in Darmstadt, Germany. Instrument response was compared with Monte-carlo simulations to study its linearity and calculate amplification.

1 - 29 of 29
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