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  • 1. Abdellaoui, G.
    et al.
    Abe, S.
    Acheli, A.
    Adams, J. H. J. H.
    Ahmad, S.
    Ahriche, A.
    Albert, J. -N
    Allard, D.
    Alonso, G.
    Anchordoqui, L.
    Andreev, V.
    Anzalone, A.
    Aouimeure, W.
    Arai, Y.
    Arsene, N.
    Asano, K.
    Attallah, R.
    Attoui, H.
    Pemas, M. Ave
    Bacholle, S.
    Bakiri, M.
    Baragatti, P.
    Barrillon, P.
    Bartocci, S.
    Batsch, T.
    Bayer, J.
    Bechini, R.
    Belenguer, T.
    Bellotti, R.
    Belov, A.
    Belov, K.
    Benadda, B.
    Benmessai, K.
    Berlind, A. A.
    Bertaina, M.
    Biermann, P. L.
    Biktemerova, S.
    Bisconti, F.
    Blanc, N.
    Blecki, J.
    Blin-Bondil, S.
    Bobik, P.
    Bogomilov, M.
    Bonamente, M.
    Boudaoud, R.
    Bozzo, E.
    Briggs, M. S.
    Bruno, A.
    Caballero, K. S.
    Cafagna, F.
    Campana, D.
    Capdevielle, J. -N
    Capel, Francesca
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Caramete, A.
    Caramete, L.
    Carlson, Per
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Caruso, R.
    Casolino, M.
    Cassardo, C.
    Castellina, A.
    Castellini, G.
    Catalano, C.
    Catalano, O.
    Cellino, A.
    Chikawa, M.
    Chiritoi, G.
    Christl, M. J.
    Connaughton, V.
    Conti, L.
    Cordero, G.
    Crawford, H. J.
    Cremonini, R.
    Csorna, S.
    Dagoret-Campagne, S.
    De Donato, C.
    de la Taille, C.
    De Santis, C.
    del Peral, L.
    Di Martino, M.
    Djemil, T.
    Djenas, S. A.
    Dulucq, F.
    Dupieux, M.
    Dutan, I.
    Ebersoldt, A.
    Ebisuzaki, T.
    Engel, R.
    Eser, J.
    Fang, K.
    Fenu, F.
    Fernandez-Gonzalez, S.
    Fernandez-Soriano, J.
    Ferrarese, S.
    Finco, D.
    Flamini, M.
    Fornaro, C.
    Fouka, M.
    Franceschi, A.
    Franchini, S.
    Fuglesang, Christer
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Fujimoto, J.
    Fukushima, M.
    Galeotti, P.
    Garcia-Ortega, E.
    Garipov, G.
    Gascon, E.
    Geary, J.
    Gelmini, G.
    Genci, J.
    Giraudo, G.
    Gonchar, M.
    Alvarado, C. Gonzalez
    Gorodetzky, P.
    Guarino, F.
    Guehaz, R.
    Guzman, A.
    Hachisu, Y.
    Haiduc, M.
    Harlov, B.
    Haungs, A.
    Carretero, J. Hernandez
    Hidber, W.
    Higashide, K.
    Ikeda, D.
    Ikeda, H.
    Inoue, N.
    Inoue, S.
    Isgro, F.
    Itow, Y.
    Jammer, T.
    Joven, E.
    Judd, E. G.
    Jung, A.
    Jochum, J.
    Kajino, F.
    Kajino, T.
    Kalli, S.
    Kaneko, I.
    Kang, D.
    Kanouni, F.
    Karadzhov, Y.
    Karczmarczyk, J.
    Karus, M.
    Katahira, K.
    Kawai, K.
    Kawasaki, Y.
    Kedadra, A.
    Khales, H.
    Khrenov, B. A.
    Kim, Jeong-Sook
    Kim, Soon-Wook
    Kim, Sug-Whan
    Kleifges, M.
    Klimov, P. A.
    Kolev, D.
    Kreykenbohm, I.
    Kudela, K.
    Kurihara, Y.
    Kusenko, A.
    Kuznetsov, E.
    Lacombe, M.
    Lachaud, C.
    Lahmar, H.
    Lakhdari, F.
    Larsson, Oscar
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Lee, J.
    Licandro, J.
    Lim, H.
    Campano, L. Lopez
    Maccarone, M. C.
    Mackovjak, S.
    Mandi, M.
    Maravilla, D.
    Marcelli, L.
    Marcos, J. L.
    Marini, A.
    Martens, K.
    Martin, Y.
    Martinez, O.
    Masciantonio, G.
    Mase, K.
    Matev, R.
    Matthews, J. N.
    Mebarki, N.
    Medina-Tanco, G.
    Mehrad, L.
    Mendoza, M. A.
    Merino, A.
    Memik, T.
    Meseguer, J.
    Messaoud, S.
    Micu, O.
    Mimouni, J.
    Miyamoto, H.
    Miyazaki, Y.
    Mizumoto, Y.
    Modestino, G.
    Monaco, A.
    Monnier-Ragaigne, D.
    de los Rios, J. A. Morales
    Moretto, C.
    Morozenko, V. S.
    Mot, B.
    Murakami, T.
    Nadji, B.
    Nagano, M.
    Nagata, M.
    Nagataki, S.
    Nakamura, T.
    Napolitano, T.
    Nardellis, A.
    Naumov, D.
    Nava, R.
    Neronov, A.
    Nomoto, K.
    Nonaka, T.
    Ogawa, T.
    Ogio, S.
    Ohmori, H.
    Olinto, A. V.
    Orleariski, P.
    Osteria, G.
    Painter, W.
    Panasyuk, M. I.
    Panico, B.
    Parizot, E.
    Park, I. H.
    Park, H. W.
    Pastircak, B.
    Patzak, T.
    Paul, T.
    Pennypacker, C.
    Perdichizzi, M.
    Perez-Grande, I.
    Perfetto, F.
    Peter, T.
    Picozza, P.
    Pierog, T.
    Pindado, S.
    Piotrowski, L. W.
    Pirainou, S.
    Placidis, L.
    Plebaniak, Z.
    Pliego, S.
    Pollini, A.
    Popescu, E. M.
    Prat, P.
    Prevot, G.
    Prieto, H.
    Putis, M.
    Rabanal, J.
    Radu, A. A.
    Rahmani, M.
    Reardon, P.
    Reyes, M.
    Rezazadeh, M.
    Ricci, M.
    Frias, M. D. Rodriguez
    Ronga, F.
    Roth, M.
    Rothkaehl, H.
    Roudil, G.
    Rusinov, I.
    Rybczynski, M.
    Sabau, M. D.
    Cano, G. Saez
    Sagawa, H.
    Sahnoune, Z.
    Saito, A.
    Sakaki, N.
    Sakata, M.
    Salazar, H.
    Sanchez, J. C.
    Sanchez, J. L.
    Santangelo, A.
    Cruz, L. Santiago
    Sanz-Andres, A.
    Palomino, M. Sanz
    Saprykin, O.
    Sarazin, F.
    Sato, H.
    Sato, M.
    Schanz, T.
    Schieler, H.
    Scotti, V.
    Segreto, A.
    Selmane, S.
    Semikoz, D.
    Serra, M.
    Sharakin, S.
    Shibata, T.
    Shimizu, H. M.
    Shinozaki, K.
    Shirahama, T.
    Siemieniec-Ozieblo, G.
    Sledd, J.
    Slomiriska, K.
    Sobey, A.
    Stan, I.
    Sugiyama, T.
    Supanitsky, D.
    Suzuki, M.
    Szabelska, B.
    Szabelski, J.
    Tahi, H.
    Tajima, F.
    Tajima, N.
    Tajima, T.
    Takahashi, Y.
    Takami, H.
    Takeda, M.
    Takizawa, Y.
    Talai, M. C.
    Tenzer, C.
    Tibolla, O.
    Tkachev, L.
    Tokuno, H.
    Tomida, T.
    Tone, N.
    Toscano, S.
    Traiche, M.
    Tsenov, R.
    Tsunesada, Y.
    Tsuno, K.
    Tymieniecka, T.
    Uchihori, Y.
    Unger, M.
    Vaduvescu, O.
    Valdes-Galicia, J. F.
    Vallania, P.
    Vankova, G.
    Vigorito, C.
    Villasenor, L.
    Vicek, B.
    von Ballmoos, P.
    Vrabel, M.
    Wada, S.
    Watanabe, J.
    Watanabe, S.
    Watts, J., Jr.
    Weber, M.
    Munoz, R. Weigand
    Weindl, A.
    Weiler, T. J.
    Wibig, T.
    Wiencke, L.
    Wille, M.
    Wilms, J.
    Wlodarczyk, Z.
    Yamamoto, T.
    Yamamoto, Y.
    Yang, J.
    Yano, H.
    Yashin, I. V.
    Yonetoku, D.
    Yoshida, S.
    Young, R.
    Zgura, I. S.
    Zotov, M. Yu.
    Marchi, A. Zuccaro
    Meteor studies in the framework of the JEM-EUSO program2017In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 143, p. 245-255Article in journal (Refereed)
    Abstract [en]

    We summarize the state of the art of a program of UV observations from space of meteor phenomena, a secondary objective of the JEM-EUSO international collaboration. Our preliminary analysis indicates that JEM-EUSO, taking advantage of its large FOV and good sensitivity, should be able to detect meteors down to absolute magnitude close to 7. This means that JEM-EUSO should be able to record a statistically significant flux of meteors, including both sporadic ones, and events produced by different meteor streams. Being unaffected by adverse weather conditions, JEM-EUSO can also be a very important facility for the detection of bright meteors and fireballs, as these events can be detected even in conditions of very high sky background. In the case of bright events, moreover, exhibiting some persistence of the meteor train, preliminary simulations show that it should be possible to exploit the motion of the ISS itself and derive at least a rough 3D reconstruction of the meteor trajectory. Moreover, the observing strategy developed to detect meteors may also be applied to the detection of nuclearites, exotic particles whose existence has been suggested by some theoretical investigations. Nuclearites are expected to move at higher velocities than meteoroids, and to exhibit a wider range of possible trajectories, including particles moving upward after crossing the Earth. Some pilot studies, including the approved Mini-EUSO mission, a precursor of JEM-EUSO, are currently operational or in preparation. We are doing simulations to assess the performance of Mini-EUSO for meteor studies, while a few meteor events have been already detected using the ground-based facility EUSO-TA.

  • 2.
    Alday, Juan
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Roth, Lorenz
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Ivchenko, Nickolay
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Retherford, Kurt D.
    Becker, Tracy M.
    Molyneux, Philippa
    Saur, Joachim
    New constraints on Ganymede's hydrogen corona: Analysis of Lyman-alpha emissions observed by HST/STIS between 1998 and 20142017In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 148, p. 35-44Article in journal (Refereed)
    Abstract [en]

    Far-ultraviolet observations of Ganymede's atmospheric emissions were obtained with the Space Telescope Imaging Spectrograph (STIS) onboard of the Hubble Space Telescope (HST) on several occasions between 1998 and 2014. We analyze the Lyman-alpha emission from four HST campaigns in order to constrain the abundance and variation of atomic hydrogen in Ganymede's atmosphere. We apply a forward model that estimates surface reflection and resonant scattering in an escaping corona of the solar Lyman-alpha flux, taking into account the effects of the hydrogen in the interplanetary medium. The atmospheric emissions around Ganymede's disk derived for the observations taken between 1998 and 2011 are consistent with a hydrogen corona in the density range of (5-8) x 10(3) cm(-3) at the surface. The hydrogen density appears to be generally stable in that period. In 2014, Ganymede's corona brightness is approximately 3 times lower during two observations of Ganymede's trailing hemisphere and hardly detectable at all during two observations of the leading hemisphere. We also investigate extinction of Ganymede's coronal emissions in the Earth's upper atmosphere or geocorona. For small Doppler shifts, resonant scattering in the geocorona of the moon corona emissions can effectively reduce the brightness observed by HST. In the case of the 2014 leading hemisphere observations, an estimated extinction of 80% might explain the non-detection of Ganymede's hydrogen corona. Geocoronal extinction might also explain a previously detected hemispheric difference from Callisto's hydrogen corona.

  • 3.
    Amador, Elena S.
    et al.
    Univ Washington, Astrobiol Program, Seattle, WA 98195 USA..
    Cable, Morgan L.
    CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA..
    Chaudry, Nosheen
    Cranfield Univ, Sch Engn, Cranfield MK43 0AL, Beds, England..
    Cullen, Thomas
    Cranfield Univ, Sch Engn, Cranfield MK43 0AL, Beds, England..
    Gentry, Diana
    Stanford Univ, Stanford, CA 94305 USA..
    Jacobsen, Malene B.
    Murukesan, Gayathri
    Univ Turku, Dept Biochem Biochem, Turun 20014, Finland..
    Schwieterman, Edward W.
    Univ Washington, Astrobiol Program, Seattle, WA 98195 USA..
    Stevens, Adam H.
    Open Univ, Dept Phys Sci, Milton Keynes MK15 0BT, Bucks, England..
    Stockton, Amanda
    Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA..
    Yin, Chang
    KTH, School of Biotechnology (BIO), Centres, Albanova VinnExcellence Center for Protein Technology, ProNova. Royal Inst Technol, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden.;Stockholm Univ, Astrobiol Ctr, SE-10691 Stockholm, Sweden..
    Cullen, David C.
    Cranfield Univ, Sch Engn, Cranfield MK43 0AL, Beds, England..
    Geppert, Wolf
    Stockholm university, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden.;Stockholm Univ, Astrobiol Ctr, SE-10691 Stockholm, Sweden..
    Synchronous in-field application of life-detection techniques in planetary analog missions2015In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 106, p. 1-10Article in journal (Refereed)
    Abstract [en]

    Field expeditions that simulate the operations of robotic planetary exploration missions at analog sites on Earth can help establish best practices and are therefore a positive contribution to the planetary exploration community. There are many sites in Iceland that possess heritage as planetary exploration analog locations and whose environmental extremes make them suitable for simulating scientific sampling and robotic operations. We conducted a planetary exploration analog mission at two recent lava fields in Iceland, Fimmvorouhals (2010) and Eldfell (1973), using a specially developed field laboratory. We tested the utility of in-field site sampling down selection and tiered analysis operational capabilities with three life detection and characterization techniques: fluorescence microscopy (FM), adenine-triphosphate (ATP) bioluminescence assay, and quantitative polymerase chain reaction (qPCR) assay. The study made use of multiple cycles of sample collection at multiple distance scales and field laboratory analysis using the synchronous fife-detection techniques to heuristically develop the continuing sampling and analysis strategy during the expedition. Here we report the operational lessons learned and provide brief summaries of scientific data. The full scientific data report will follow separately. We found that rapid in-field analysis to determine subsequent sampling decisions is operationally feasible, and that the chosen life detection and characterization techniques are suitable for a terrestrial life-detection field mission. In-field analysis enables the rapid obtainment of scientific data and thus facilitates the collection of the most scientifically relevant samples within a single field expedition, without the need for sample relocation to external laboratories. The operational lessons learned in this study could be applied to future terrestrial field expeditions employing other analytical techniques and to future robotic planetary exploration missions.

  • 4.
    Blomberg, Lars
    KTH, Superseded Departments, Alfvén Laboratory. KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Mercury's magnetosphere, exosphere and surface: Low-frequency field and wave measurements as a diagnostic tool1997In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 45, no 1, p. 143-148Article in journal (Refereed)
    Abstract [en]

    Diagnostics that can be made with combined electric and magnetic field measurements at Mercury are reviewed. Fundamental electrodynamic questions which can be answered by means of a Mercury Orbiter are discussed. These include, solar wind-magnetosphere coupling, coupling to low altitude, exospheric or planetary surface conductivity, auroral particle acceleration, and magnetospheric substorms. It is concluded that a comprehensive instrumentation package for low-frequency fields and waves on a future Mercury Orbiter mission may yield significant new information of interest to magnetospheric as well as to planetary physics in general. (C) 1997 Elsevier Science Ltd.

  • 5.
    Futaana, Yoshifumi
    et al.
    Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden..
    Barabash, Stas
    Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden..
    Wieser, Martin
    Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden..
    Wurz, Peter
    Univ Bern, Bern, Switzerland..
    Hurley, Dana
    Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA..
    Horanyi, Mihaly
    Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA..
    Mall, Urs
    Max Planck Inst Solar Syst Res, Gottingen, Germany..
    Andre, Nicolas
    Univ Toulouse, CNRS, IRAP, Toulouse, France..
    Ivchenko, Nickolay
    KTH, School of Electrical Engineering and Computer Science (EECS), Space and Plasma Physics.
    Oberst, Juergen
    German Aerosp Ctr, Berlin, Germany..
    Retherford, Kurt
    Southwest Res Inst, San Antonio, TX USA..
    Coates, Andrew
    UCL, Mullard Space Sci Lab, London, England..
    Masters, Adam
    Imperial Coll London, London, England..
    Wahlund, Jan-Erik
    Swedish Inst Space Phys, Uppsala, Sweden..
    Kallio, Esa
    Aalto Univ, Helsinki, Finland..
    SELMA mission: How do airless bodies interact with space environment? The Moon as an accessible laboratory2018In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 156, p. 23-40Article in journal (Refereed)
    Abstract [en]

    The Moon is an archetypal atmosphere-less celestial body in the Solar System. For such bodies, the environments are characterized by complex interaction among the space plasma, tenuous neutral gas, dust and the outermost layer of the surface. Here we propose the SELMA mission (Surface, Environment, and Lunar Magnetic Anomalies) to study how airless bodies interact with space environment. SELMA uses a unique combination of remote sensing via ultraviolet and infrared wavelengths, and energetic neutral atom imaging, as well as in situ measurements of exospheric gas, plasma, and dust at the Moon. After observations in a lunar orbit for one year, SELMA will conduct an impact experiment to investigate volatile content in the soil of the permanently shadowed area of the Shackleton crater. SELMA also carries an impact probe to sound the Reiner-Gamma mini-magnetosphere and its interaction with the lunar regolith from the SELMA orbit down to the surface. SELMA was proposed to the European Space Agency as a medium-class mission (M5) in October 2016. Research on the SELMA scientific themes is of importance for fundamental planetary sciences and for our general understanding of how the Solar System works. In addition, SELMA outcomes will contribute to future lunar explorations through qualitative characterization of the lunar environment and, in particular, investigation of the presence of water in the lunar soil, as a valuable resource to harvest from the lunar regolith.

  • 6. Heikkila, W.J.
    et al.
    Pellinen, R.J.
    Fälthammar, Carl-Gunne
    KTH, Superseded Departments, Alfvén Laboratory. KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Block, Lars P
    KTH, Superseded Departments, Alfvén Laboratory. KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Potential and inductive electric fields in the magnetosphere during auroras1979In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 27, p. 1383-1389Article in journal (Refereed)
  • 7.
    Karlsson, Tomas
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Liljeblad, Elisabet
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Kullen, Anita
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Raines, Jim M.
    Slavin, James A.
    Sundberg, Torbjorn
    Isolated magnetic field structures in Mercury's magnetosheath as possible analogues for terrestrial magnetosheath plasmoids and jets2016In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 129, p. 61-73Article in journal (Refereed)
    Abstract [en]

    We have investigated MESSENGER magnetic field data from the Mercury magnetosheath and near solar wind, to identify isolated magnetic field structures (defined as clear, isolated changes in the field magnitude). Their properties are studied in order to determine if they may be considered as analogues to plasmoids and jets known to exist in Earth's magnetosheath. Both isolated decreases of the magnetic field absolute value ('negative magnetic field structures') and increases ('positive structures') are found in the magnetosheath, whereas only negative structures are found in the solar wind. The similar properties of the solar wind and magnetosheath negative magnetic field structures suggests that they are analogous to diamagnetic plasmoids found in Earth's magnetosheath and near solar wind. The latter have earlier been identified with solar wind magnetic holes. Positive magnetic field structures are only found in the magnetosheath, concentrated to a region relatively close to the magnetopause. Their proximity to the magnetopause, their scale sizes, and the association of a majority of the structures with bipolar magnetic field signatures identify them as flux transfer events (which generally are associated with a decrease of plasma density in the magnetosheath). The positive magnetic field structures are therefore not likely to be analogous to terrestrial paramagnetic plasmoids but possibly to a sub-population of magnetosheath jets. At Earth, a majority of magnetosheath jets are associated with the quasi-parallel bow shock. We discuss some consequences of the findings of the present investigation pertaining to the different nature of the quasi-parallel bow shock at Mercury and Earth.

  • 8. Kasaba, Y.
    et al.
    Bougeret, J. L.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Kojima, H.
    Yagitani, S.
    Moncuquet, M.
    Trotignon, J. G.
    Chanteur, G.
    Kumamoto, A.
    Kasahara, Y.
    Lichtenberger, J.
    Omura, Y.
    Ishisaka, K.
    Matsumoto, H.
    MatsumotoJ, H.
    The Plasma Wave Investigation (PWI) onboard the BepiColombo/MMO: First measurement of electric fields, electromagnetic waves, and radio waves around Mercury2010In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 58, no 1-2, p. 238-278Article in journal (Refereed)
    Abstract [en]

    The BepiColombo Mercury Magnetospheric Orbiter (MMO) spacecraft includes the plasma and radio wave observation system called Plasma Wave Investigation (PWI). Since the receivers for electric field, plasma waves, and radio waves are not installed in any of the preceding spacecraft to Mercury, the PWI will provide the first opportunity for conducting in-situ and remote-sensing observations of electric fields, plasma waves, and radio waves in the Hermean magnetosphere and exosphere. These observations are valuable in studying structure, dynamics, and energy exchange processes in the unique magnetosphere of Mercury. They are characterized by the key words of the non-MHD environment and the peculiar interaction between the relatively large planet without ionosphere and the solar wind with high dynamic pressure. The PWI consists of three sets of receivers (EWO, SORBET, and AM(2)P), connected to two sets of electric field sensors (MEFISTO and WPT) and two kinds of magnetic field sensors (LF-SC and DB-SC). The PWI will observe both waveforms and frequency spectra in the frequency range from DC to 10 MHz for the electric field and from 0.3 Hz to 640kHz for the magnetic field. From 2008, we will start the development of the engineering model, which is conceptually consistent with the flight model design. The present paper discusses the significance and objectives of plasma/radio wave observations in the Hermean magnetosphere, and describes the PWI sensors, receivers and their performance as well as the onboard data processing.

  • 9.
    Marklund, Göran
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Block, Lars
    Lindqvist, Per-Arne
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Rocket measurements of electric fields, electron density and temperature during different phases of auroral substorms1981In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 29, no 2, p. 249-259Article in journal (Refereed)
    Abstract [en]

    On 27 January 1979, three rocket payloads were launched from Kiruna, Sweden into different phases of two successive auroral substorrns. Among other experiments, the payloads carried the RIT double probe electric field experiments providing electric field, electron density and temperature data which are presented here. These data supported by rocket particle observations are discussed mainly in association with ground-based observations (magnetometer, TV) and very briefly with GEOS electric field data. The motions of the auroral forms as obtained from auroral pictures are compared with E × B/B2 drifts and the currents calculated from the rocket electric field and density measurements with the equivalent current system deduced from ground-based magnetometer data (Scandinavian Magnetometer Array).

  • 10.
    Mattsson, Lars
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Modelling dust processing and the evolution of grain sizes in the ISM using the method of moments2016In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088Article in journal (Refereed)
    Abstract [en]

    Interstellar dust grains do not have a single well-defined origin. Stars are demonstrably dust producers, but also efficient destroyers of cosmic dust. Dust destruction in the ISM is believed to be the result of SN shocks hitting the ambient ISM gas (and dust) and lead to an increased rate of ion sputtering, which reduces the dust mass. Grains located in cold molecular clouds can on the other hand grow by condensation, thus providing a replenishment mechanism or even a dominant channel of dust formation. In dense environments grains may coagulate and form large composite grains and aggregates and if grains collide with large enough energies they may be shattered, forming a range of smaller debris grains. The present paper presents a statistical modelling approach using the method of moments, which is computationally very inexpensive and may therefore be an attractive option when combining dust processing with, e.g., detailed simulations of interstellar gas dynamics. A solar-neighbourhood-like toy model of interstellar dust evolution is presented as an example. © 2016.

  • 11. SANDAHL, I
    et al.
    Lindqvist, Per-Arne
    KTH.
    Electron populations above the nightside auroral oval during magnetic quiet times1990In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 38, no 8, p. 1031-1049Article in journal (Refereed)
    Abstract [en]

    In several studies of particle morphology above the nightside auroral oval, the electrons have been divided into two separate spatial regions, often called the BPS (from "boundary plasma sheet") and the CPS (from "central plasma sheet") (Winningham et al., 1975, J. geophys. Res. 80, 3148). The names were derived from the source regions suggested by Winningham et al. In many cases this classification has worked well, but there are also many cases in which it has not. In this paper an alternative classification is proposed and explored by investigating the spatial distribution of electrons at altitudes between 2000 and 13,500 km, using particle spectrograms from the Viking satellite. A major difference between the newly proposed and the earlier classification is that spatial regions of populations may overlap in this new scheme. Electrons above the auroral oval could be divided into two populations. The first one is spatially unstructured and has a characteristic energy of a few kiloelectron volts. It is usually trapped in its equatorward part, while it is isotropic in its poleward part. The second one is spatially structured and normally has a characteristic energy of 100 eV or less. It is always present when there are signs of electron acceleration along magnetic field lines. The global distributions of both the structured and the unstructured electrons are ring-shaped. The two regions partially overlap, and the average latitude of the structured electrons is higher than the average latitude of the unstructured electrons. The majority of bright auroras appear in the region of overlap. The average poleward edge of the overlap region seems to coincide with the average poleward edge of region 1 field-aligned currents. We suggest that this boundary maps to the boundary between the central plasma sheet and the plasma sheet boundary layer. We also suggest that the sources for the region where only structured electrons are present are the low-latitude boundary layer and plasma sheet boundary layer. The conclusions concerning source regions are supported by mapping of the particle population regions into the equatorial plane of the magnetosphere using the Tsyganenko (1987, Planet. Space Sci. 35, 1347) magnetic field model. The average boundary between region 1 and region 2 field-aligned currents in the afternoon and evening is approximately at the average equatorward boundary of unstructured electrons. Through the midnight, morning and prenoon sectors it is at the average equatorward boundary of structured electrons.

  • 12.
    Sundberg, Torbjörn
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Boardsen, S. A.
    Slavin, J. A.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Korth, H.
    The Kelvin-Helmholtz instability at Mercury: An assessment2010In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 58, no 11, p. 1434-1441Article in journal (Refereed)
    Abstract [en]

    The Kelvin-Helmholtz instability is believed to be an important means for the transfer of energy, plasma, and momentum from the solar wind into planetary magnetospheres, with in situ measurements reported from Earth, Saturn, and Venus. During the first MESSENGER flyby of Mercury, three periodic rotations were observed in the magnetic field data possibly related to a Kelvin-Helmholtz wave on the dusk side magnetopause. We present an analysis of the event, along with comparisons to previous Kelvin-Helmholtz observations and an investigation of what influence finite ion gyro radius effects, believed to be of importance in the Hermean magnetosphere, may have on the instability. The wave signature does not correspond to that of typical Kelvin-Helmholtz events, and the magnetopause direction does not show any signs of major deviation from the unperturbed case. There is thus no indication of any high amplitude surface waves. On the other hand, the wave period corresponds to that expected for a Kelvin-Helmholtz wave, and as the dusk side is shown to be more stable than the dawn side, we judge the observed waves not to be fully developed Kelvin-Helmholtz waves, but they may be an initial perturbation that could cause Kelvin-Helmholtz waves further down the tail. (C) 2010 Elsevier Ltd. All rights reserved.

  • 13.
    Sundberg, Torbjörn
    et al.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Boardsen, S.A.
    Slavin, J.A.
    Blomberg, Lars G.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Cumnock, Judy A.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Solomon, S. C.
    Anderson, B. J.
    Korth, H.
    Reconstruction of propagating Kelvin-Helmholtz vortices at Mercury's magnetopause2011In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 59, no 15, p. 2051-2057Article in journal (Refereed)
    Abstract [en]

    A series of quasi-periodic magnetopause crossings were recorded by the MESSENGER spacecraft during its third flyby of Mercury on 29 September 2009, likely caused by a train of propagating Kelvin-Helmholtz (KH) vortices. We here revisit the observations to study the internal structure of the waves. Exploiting MESSENGER's rapid traversal of the magnetopause, we show that the observations permit a reconstruction of the structure of a rolled-up KH vortex directly from the spacecraft's magnetic field measurements. The derived geometry is consistent with all large-scale fluctuations in the magnetic field data, establishes the non-linear nature of the waves, and shows their vortex-like structure. In several of the wave passages, a reduction in magnetic field strength is observed in the middle of the wave, which is characteristic of rolled-up vortices and is related to the increase in magnetic pressure required to balance the centrifugal force on the plasma in the outer regions of a vortex, previously reported in computer simulations. As the KH wave starts to roll up, the reconstructed geometry suggests that the vortices develop two gradual transition regions in the magnetic field, possibly related to the mixing of magnetosheath and magnetospheric plasma, situated at the leading edges from the perspectives of both the magnetosphere and the magnetosheath.

  • 14. Wahlund, J. E.
    et al.
    Andre, M.
    Eriksson, A. I. E.
    Lundberg, M.
    Morooka, M. W.
    Shafiq, M.
    Averkarnp, T. F.
    Gurnett, D. A.
    Hospodarsk, G. B.
    Kurth, W. S.
    Jacobsen, K. S.
    Pedersen, A.
    Farrell, W.
    Ratynskaia, Svetlana V.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Piskunov, N.
    Detection of dusty plasma near the E-ring of Saturn2009In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 57, no 14-15, p. 1795-1806Article in journal (Refereed)
    Abstract [en]

    We present several independent in-situ measurements, which provide evidence that charged dust in the E-ring interacts collectively with the dense surrounding plasma disk of Saturn, i.e., form a system of dust-plasma interaction. The results are based on data sampled by the Radio and Plasma Wave Science (RPWS) investigation onboard Cassini, which allows for interferometry of plasma density inhomogeneities (delta n/n) with two antenna elements and a Langmuir probe sensor. The interferometer experiment detects two ion populations: one co-rotating with the planetary magnetic field and another moving with near Keplerian speed around Saturn. The full range of RPWS measurements indicates that the Keplerian population consists of colder ions (T-i

  • 15. Wurz, Peter
    et al.
    Blomberg, Lars G.
    KTH, Superseded Departments, Alfvén Laboratory. KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Particle populations in Mercury's magnetosphere2001In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 49, no 14-15, p. 1643-1653Article in journal (Refereed)
    Abstract [en]

    Observations by Mariner 10 during its first and third flybys showed that Mercury possesses an intrinsic magnetic field resulting in a small magnetosphere that can keep the solar wind from directly interacting with the planet's surface under usual conditions. Since Mercury occupies a large fraction of its magnetosphere, regions of trapped charged particles in the inner magnetosphere, the plasmasphere and the energetic radiation belts, would all be absent. During the first flyby, energetic particle bursts were detected and interpreted as hermean substroms analogous to the terrestrial magnetosphere. Moreover, during this flyby, ULF waves and field-aligned currents were detected in the data. Earth-based observations of Na, K, and Ca populations in the exosphere strongly suggest the existence of dynamic magnetospheric processes at high latitudes interacting with the planet's surface.

  • 16.
    Yaroshenko, V.V.
    et al.
    Max-Planck-Institute für extraterrestriche Physik, Germany.
    Ratynskaia, Svetlana V.
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Olson, Jonas
    KTH, School of Electrical Engineering (EES). KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Brenning, Nils
    KTH, School of Electrical Engineering (EES), Space and Plasma Physics.
    Wahlund, J.-E.
    Swedish Instituet of Space Physics, Uppsala.
    Morooka, M.
    Swedish Institute of Space Physics, Uppsala.
    Kurth, W.S.
    Department of Physics and Astronomy, University of Iowa, USA.
    Gurnett, D.A.
    Department of Physics and Astronomy, University of Iowa, USA.
    Morfill, G.E.
    Characteristics of charged dust inferred from the Cassini RPWS measurements in the vicinity of Enceladus2009In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088, Vol. 57, no 14-15, p. 1807-1812Article in journal (Refereed)
    Abstract [en]

    The data obtained by the Cassini Radio and Plasma Wave Science (RPWS) instrument during the shallow (17.02.2005) and the steep (14.07.2005) crossings of the E-ring revealed a considerable electron depletion in proximity to Enceladus's orbit (the difference between the ion and electron densities can reach similar to 70 cm(-3)). Assuming that this depletion is a signature of the presence of charged dust particles, the main characteristics of dust down to submicron sized particles are derived. The differential size distribution is found to be well described by a power law with an index mu similar to 5.5-6 for the lower size limit a(min) = 0.03 mu m and mu similar to 7.3-8 for a(min) = 0.1 mu m. The calculated average integral dust number density is weakly affected by values of mu and a(min). For a greater than or similar to 0.1 mu m, both flybys gave the maximum dust density about 0.1-0.3 cm(-3) in the vicinity of Enceladus. Our results imply that the dust structure near Enceladus is characterized by approximately the same vertical length scale of 8000 km and reaches a maximum at the same radial distance (displaced outward of the orbit of Enceladus) as found by Kempf et al. [2008. The E-ring in the vicinity of Enceladus. Spatial distribution and properties of the ring particles. Icarus 193, 420-437], from the dust impact data.

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