1
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Kurth WS, Sulaiman AH, Hospodarsky GB, Menietti JD, Mauk BH, Clark G, Allegrini F, Valek P, Connerney JEP, Waite JH, Bolton SJ, Imai M, Santolik O, Li W, Duling S, Saur J, Louis C. Juno Plasma Wave Observations at Ganymede. Geophys Res Lett 2022; 49:e2022GL098591. [PMID: 37034392 PMCID: PMC10078157 DOI: 10.1029/2022gl098591] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/09/2022] [Revised: 04/22/2022] [Accepted: 04/27/2022] [Indexed: 06/19/2023]
Abstract
The Juno Waves instrument measured plasma waves associated with Ganymede's magnetosphere during its flyby on 7 June, day 158, 2021. Three distinct regions were identified including a wake, and nightside and dayside regions in the magnetosphere distinguished by their electron densities and associated variability. The magnetosphere includes electron cyclotron harmonic emissions including a band at the upper hybrid frequency, as well as whistler-mode chorus and hiss. These waves likely interact with energetic electrons in Ganymede's magnetosphere by pitch angle scattering and/or accelerating the electrons. The wake is accentuated by low-frequency turbulence and electrostatic solitary waves. Radio emissions observed before and after the flyby likely have their source in Ganymede's magnetosphere.
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Affiliation(s)
- W. S. Kurth
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - A. H. Sulaiman
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | | | - J. D. Menietti
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - B. H. Mauk
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - G. Clark
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - P. Valek
- Southwest Research InstituteSan AntonioTXUSA
| | | | - J. H. Waite
- Southwest Research InstituteSan AntonioTXUSA
| | | | - M. Imai
- Department of Electrical Engineering and Information ScienceNational Institute of Technology (KOSEN), Niihama CollegeNiihamaJapan
| | - O. Santolik
- Department of Space PhysicsInstitute of Atmospheric Physics of the Czech Academy of SciencesPragueCzechia
- Faculty of Mathematics and PhysicsCharles UniversityPragueCzechia
| | - W. Li
- Center for Space PhysicsBoston UniversityBostonMAUSA
| | - S. Duling
- Institute of Geophysics and MeteorologyUniversity of CologneCologneGermany
| | - J. Saur
- Institute of Geophysics and MeteorologyUniversity of CologneCologneGermany
| | - C. Louis
- School of Cosmic Physics, DIAS Dunsink ObservatoryDublin Institute for Advanced StudiesDublinIreland
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2
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Orsini S, Milillo A, Lichtenegger H, Varsani A, Barabash S, Livi S, De Angelis E, Alberti T, Laky G, Nilsson H, Phillips M, Aronica A, Kallio E, Wurz P, Olivieri A, Plainaki C, Slavin JA, Dandouras I, Raines JM, Benkhoff J, Zender J, Berthelier JJ, Dosa M, Ho GC, Killen RM, McKenna-Lawlor S, Torkar K, Vaisberg O, Allegrini F, Daglis IA, Dong C, Escoubet CP, Fatemi S, Fränz M, Ivanovski S, Krupp N, Lammer H, Leblanc F, Mangano V, Mura A, Rispoli R, Sarantos M, Smith HT, Wieser M, Camozzi F, Di Lellis AM, Fremuth G, Giner F, Gurnee R, Hayes J, Jeszenszky H, Trantham B, Balaz J, Baumjohann W, Cantatore M, Delcourt D, Delva M, Desai M, Fischer H, Galli A, Grande M, Holmström M, Horvath I, Hsieh KC, Jarvinen R, Johnson RE, Kazakov A, Kecskemety K, Krüger H, Kürbisch C, Leblanc F, Leichtfried M, Mangraviti E, Massetti S, Moissenko D, Moroni M, Noschese R, Nuccilli F, Paschalidis N, Ryno J, Seki K, Shestakov A, Shuvalov S, Sordini R, Stenbeck F, Svensson J, Szalai S, Szego K, Toublanc D, Vertolli N, Wallner R, Vorburger A. Inner southern magnetosphere observation of Mercury via SERENA ion sensors in BepiColombo mission. Nat Commun 2022; 13:7390. [PMID: 36450728 PMCID: PMC9712576 DOI: 10.1038/s41467-022-34988-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/24/2022] [Accepted: 11/14/2022] [Indexed: 12/03/2022] Open
Abstract
Mercury's southern inner magnetosphere is an unexplored region as it was not observed by earlier space missions. In October 2021, BepiColombo mission has passed through this region during its first Mercury flyby. Here, we describe the observations of SERENA ion sensors nearby and inside Mercury's magnetosphere. An intermittent high-energy signal, possibly due to an interplanetary magnetic flux rope, has been observed downstream Mercury, together with low energy solar wind. Low energy ions, possibly due to satellite outgassing, were detected outside the magnetosphere. The dayside magnetopause and bow-shock crossing were much closer to the planet than expected, signature of a highly eroded magnetosphere. Different ion populations have been observed inside the magnetosphere, like low latitude boundary layer at magnetopause inbound and partial ring current at dawn close to the planet. These observations are important for understanding the weak magnetosphere behavior so close to the Sun, revealing details never reached before.
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Affiliation(s)
- S Orsini
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy.
| | - A Milillo
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - H Lichtenegger
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - A Varsani
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - S Barabash
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - S Livi
- Southwest Research Institute, San Antonio, TX, USA
- University of Michigan, Department of Climate and Space Sciences and Engineering, Ann Arbor, MI, USA
| | - E De Angelis
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - T Alberti
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - G Laky
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - H Nilsson
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - M Phillips
- Southwest Research Institute, San Antonio, TX, USA
| | - A Aronica
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - E Kallio
- Aalto University, Department of Electronics and Nanoengineering, School of Electrical Engineering, Helsinki, Finland
| | - P Wurz
- University of Bern, Institute of Physics, Bern, Switzerland
| | | | | | - J A Slavin
- University of Michigan, Department of Climate and Space Sciences and Engineering, Ann Arbor, MI, USA
| | - I Dandouras
- Institut de Recherche en Astrophysique et Planétologie, CNRS, CNES, Université de Toulouse, Toulouse, France
| | - J M Raines
- University of Michigan, Department of Climate and Space Sciences and Engineering, Ann Arbor, MI, USA
| | | | - J Zender
- ESA-ESTEC, Noordwijk, The Netherlands
| | | | - M Dosa
- Wigner Research Centre for Physics, Budapest, Hungary
| | - G C Ho
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723, USA
| | - R M Killen
- NASA/Goddard Space Flight Center, Greenbelt, MD, 20771, USA
| | | | - K Torkar
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - O Vaisberg
- IKI Space Research Institute, Moscow, Russia
| | - F Allegrini
- Southwest Research Institute, San Antonio, TX, USA
- University of Texas at San Antonio, Department of Physics and Astronomy, San Antonio, TX, USA
| | - I A Daglis
- National and Kapodistrian University of Athens, Department of Physics, Athens, Greece
- Hellenic Space Center, Athens, Greece
| | - C Dong
- Princeton Plasma Physics Laboratory and Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | | | - S Fatemi
- Department of Physics, Umeå University, Umeå, Sweden
| | - M Fränz
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077, Göttingen, Germany
| | - S Ivanovski
- Astronomincal Observatory, INAF, Trieste, Italy
| | - N Krupp
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077, Göttingen, Germany
| | - H Lammer
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - V Mangano
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - A Mura
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - R Rispoli
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - M Sarantos
- NASA/Goddard Space Flight Center, Greenbelt, MD, 20771, USA
| | - H T Smith
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723, USA
| | - M Wieser
- Swedish Institute of Space Physics, Kiruna, Sweden
| | | | | | - G Fremuth
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - F Giner
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - R Gurnee
- Laboratory for Atmospheric and Space Physics, Boulder, CO, USA
| | - J Hayes
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723, USA
| | - H Jeszenszky
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - B Trantham
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - J Balaz
- Institute of Experimental Physics SAS, Slovak Academy of Sciences, 040 01, Košice, Slovakia
| | - W Baumjohann
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | | | - M Delva
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - M Desai
- Southwest Research Institute, San Antonio, TX, USA
| | - H Fischer
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077, Göttingen, Germany
| | - A Galli
- University of Bern, Institute of Physics, Bern, Switzerland
| | - M Grande
- Aberystwyth University, Aberystwyth, Ceredigion, UK
| | - M Holmström
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - I Horvath
- Wigner Research Centre for Physics, Budapest, Hungary
| | - K C Hsieh
- University of Arizona, Tucson, AZ, USA
| | - R Jarvinen
- Aalto University, Department of Electronics and Nanoengineering, School of Electrical Engineering, Helsinki, Finland
- Finnish Meteorological Institute FMI, Helsinki, Finland
| | - R E Johnson
- University of Virginia, Charlottesville, VA, 22904, USA
| | - A Kazakov
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - K Kecskemety
- Wigner Research Centre for Physics, Budapest, Hungary
| | - H Krüger
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077, Göttingen, Germany
| | - C Kürbisch
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - M Leichtfried
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - S Massetti
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - D Moissenko
- IKI Space Research Institute, Moscow, Russia
| | - M Moroni
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - R Noschese
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - F Nuccilli
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - N Paschalidis
- NASA/Goddard Space Flight Center, Greenbelt, MD, 20771, USA
| | - J Ryno
- Finnish Meteorological Institute FMI, Helsinki, Finland
| | - K Seki
- University of Tokyo, Department of Earth and Planetary Science, Graduate School of Science, Tokyo, Japan
| | - A Shestakov
- IKI Space Research Institute, Moscow, Russia
| | - S Shuvalov
- IKI Space Research Institute, Moscow, Russia
| | - R Sordini
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - F Stenbeck
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - J Svensson
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - S Szalai
- Wigner Research Centre for Physics, Budapest, Hungary
| | - K Szego
- Wigner Research Centre for Physics, Budapest, Hungary
| | - D Toublanc
- Institut de Recherche en Astrophysique et Planétologie, CNRS, CNES, Université de Toulouse, Toulouse, France
| | - N Vertolli
- Institute of Space Astrophysics and Planetology, INAF, Roma, Italy
| | - R Wallner
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - A Vorburger
- University of Bern, Institute of Physics, Bern, Switzerland
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3
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Al Saati S, Clément N, Louis C, Blanc M, Wang Y, André N, Lamy L, Bonfond B, Collet B, Allegrini F, Bolton S, Clark G, Connerney JEP, Gérard J, Gladstone GR, Kotsiaros S, Kurth WS, Mauk B. Magnetosphere-Ionosphere-Thermosphere Coupling Study at Jupiter Based on Juno's First 30 Orbits and Modeling Tools. J Geophys Res Space Phys 2022; 127:e2022JA030586. [PMID: 36591321 PMCID: PMC9787687 DOI: 10.1029/2022ja030586] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/26/2022] [Revised: 08/26/2022] [Accepted: 09/15/2022] [Indexed: 06/17/2023]
Abstract
The dynamics of the Jovian magnetosphere is controlled by the interplay of the planet's fast rotation, its solar-wind interaction and its main plasma source at the Io torus, mediated by coupling processes involving its magnetosphere, ionosphere, and thermosphere. At the ionospheric level, these processes can be characterized by a set of parameters including conductances, field-aligned currents, horizontal currents, electric fields, transport of charged particles along field lines including the fluxes of electrons precipitating into the upper atmosphere which trigger auroral emissions, and the particle and Joule heating power dissipation rates into the upper atmosphere. Determination of these key parameters makes it possible to estimate the net transfer of momentum and energy between Jovian upper atmosphere and equatorial magnetosphere. A method based on a combined use of Juno multi-instrument data and three modeling tools was developed by Wang et al. (2021, https://doi.org/10.1029/2021ja029469) and applied to an analysis of the first nine orbits to retrieve these parameters along Juno's magnetic footprint. We extend this method to the first 30 Juno science orbits and to both hemispheres. Our results reveal a large variability of these parameters from orbit to orbit and between the two hemispheres. They also show dominant trends. Southern current systems are consistent with the generation of a region of sub-corotating ionospheric plasma flows, while both super-corotating and sub-corotating plasma flows are found in the north. These results are discussed in light of the previous space and ground-based observations and currently available models of plasma convection and current systems, and their implications are assessed.
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Affiliation(s)
- S. Al Saati
- IRAPCNRSUniversité Toulouse III‐Paul SabatierCNESToulouseFrance
- CPHTCNRSInstitut Polytechnique de ParisPalaiseauFrance
| | - N. Clément
- IRAPCNRSUniversité Toulouse III‐Paul SabatierCNESToulouseFrance
- Laboratoire d’Astrophysique de BordeauxUniversité de BordeauxBordeauxFrance
| | - C. Louis
- IRAPCNRSUniversité Toulouse III‐Paul SabatierCNESToulouseFrance
- School of Cosmic PhysicsDIAS Dunsink ObservatoryDublin Institute for Advanced StudiesDublinIreland
| | - M. Blanc
- IRAPCNRSUniversité Toulouse III‐Paul SabatierCNESToulouseFrance
- LAMPythéasAix Marseille UniversitéCNRSCNESMarseilleFrance
| | - Y. Wang
- State Key Laboratory of Space WeatherNational Space Science CenterChinese Academy of SciencesBeijingChina
| | - N. André
- IRAPCNRSUniversité Toulouse III‐Paul SabatierCNESToulouseFrance
| | - L. Lamy
- LAMPythéasAix Marseille UniversitéCNRSCNESMarseilleFrance
- LESIAObservatoire de ParisUniversité PSLCNRSSorbonne UniversitéUniversité de ParisMeudonFrance
| | | | - B. Collet
- LAMPythéasAix Marseille UniversitéCNRSCNESMarseilleFrance
| | | | | | | | | | | | | | - S. Kotsiaros
- Technical University of DenmarkKongens LyngbyDenmark
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4
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Allegrini F, Olivieri AC. Linear or non-linear multivariate calibration models? That is the question. Anal Chim Acta 2022; 1226:340248. [DOI: 10.1016/j.aca.2022.340248] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/14/2022] [Revised: 08/05/2022] [Accepted: 08/07/2022] [Indexed: 11/16/2022]
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5
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Sulaiman AH, Mauk BH, Szalay JR, Allegrini F, Clark G, Gladstone GR, Kotsiaros S, Kurth WS, Bagenal F, Bonfond B, Connerney JEP, Ebert RW, Elliott SS, Gershman DJ, Hospodarsky GB, Hue V, Lysak RL, Masters A, Santolík O, Saur J, Bolton SJ. Jupiter's Low-Altitude Auroral Zones: Fields, Particles, Plasma Waves, and Density Depletions. J Geophys Res Space Phys 2022; 127:e2022JA030334. [PMID: 36247326 PMCID: PMC9539694 DOI: 10.1029/2022ja030334] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 01/28/2022] [Revised: 06/15/2022] [Accepted: 07/21/2022] [Indexed: 06/16/2023]
Abstract
The Juno spacecraft's polar orbits have enabled direct sampling of Jupiter's low-altitude auroral field lines. While various data sets have identified unique features over Jupiter's main aurora, they are yet to be analyzed altogether to determine how they can be reconciled and fit into the bigger picture of Jupiter's auroral generation mechanisms. Jupiter's main aurora has been classified into distinct "zones", based on repeatable signatures found in energetic electron and proton spectra. We combine fields, particles, and plasma wave data sets to analyze Zone-I and Zone-II, which are suggested to carry upward and downward field-aligned currents, respectively. We find Zone-I to have well-defined boundaries across all data sets. H+ and/or H3 + cyclotron waves are commonly observed in Zone-I in the presence of energetic upward H+ beams and downward energetic electron beams. Zone-II, on the other hand, does not have a clear poleward boundary with the polar cap, and its signatures are more sporadic. Large-amplitude solitary waves, which are reminiscent of those ubiquitous in Earth's downward current region, are a key feature of Zone-II. Alfvénic fluctuations are most prominent in the diffuse aurora and are repeatedly found to diminish in Zone-I and Zone-II, likely due to dissipation, at higher altitudes, to energize auroral electrons. Finally, we identify significant electron density depletions, by up to 2 orders of magnitude, in Zone-I, and discuss their important implications for the development of parallel potentials, Alfvénic dissipation, and radio wave generation.
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Affiliation(s)
- A. H. Sulaiman
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - B. H. Mauk
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - J. R. Szalay
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - G. Clark
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - G. R. Gladstone
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - S. Kotsiaros
- DTU‐SpaceTechnical University of DenmarkKongens LyngbyDenmark
| | - W. S. Kurth
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - F. Bagenal
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - B. Bonfond
- Space SciencesTechnologies and Astrophysics Research InstituteLPAPUniversité de LiègeLiègeBelgium
| | - J. E. P. Connerney
- Space Research CorporationAnnapolisMDUSA
- NASA/Goddard Space Flight CenterGreenbeltMDUSA
| | - R. W. Ebert
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - S. S. Elliott
- Minnetota Institute for AstrophysicsSchool of Physics and AstronomyUniversity of MinnesotaMinneapolisMNUSA
| | | | | | - V. Hue
- Southwest Research InstituteSan AntonioTXUSA
| | - R. L. Lysak
- Minnetota Institute for AstrophysicsSchool of Physics and AstronomyUniversity of MinnesotaMinneapolisMNUSA
| | - A. Masters
- Blackett LaboratoryImperial College LondonLondonUK
| | - O. Santolík
- Department of Space PhysicsInstitute of Atmospheric Physics of the Czech Academy of SciencesPragueCzechia
- Faculty of Mathematics and PhysicsCharles UniversityPragueCzechia
| | - J. Saur
- Institute of Geophysics and MeteorologyUniversity of CologneCologneGermany
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6
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Szalay JR, Clark G, Livadiotis G, McComas DJ, Mitchell DG, Rankin JS, Sulaiman AH, Allegrini F, Bagenal F, Ebert RW, Gladstone GR, Kurth WS, Mauk BH, Valek PW, Wilson RJ, Bolton SJ. Closed Fluxtubes and Dispersive Proton Conics at Jupiter's Polar Cap. Geophys Res Lett 2022; 49:e2022GL098741. [PMID: 35859815 PMCID: PMC9285739 DOI: 10.1029/2022gl098741] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/16/2022] [Revised: 04/14/2022] [Accepted: 04/16/2022] [Indexed: 05/08/2023]
Abstract
Two distinct proton populations are observed over Jupiter's southern polar cap: a ∼1 keV core population and ∼1-300 keV dispersive conic population at 6-7 RJ planetocentric distance. We find the 1 keV core protons are likely the seed population for the higher-energy dispersive conics, which are accelerated from a distance of ∼3-5 RJ. Transient wave-particle heating in a "pressure-cooker" process is likely responsible for this proton acceleration. The plasma characteristics and composition during this period show Jupiter's polar-most field lines can be topologically closed, with conjugate magnetic footpoints connected to both hemispheres. Finally, these observations demonstrate energetic protons can be accelerated into Jupiter's magnetotail via wave-particle coupling.
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Affiliation(s)
- J. R. Szalay
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - G. Clark
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - G. Livadiotis
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - D. J. McComas
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - D. G. Mitchell
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - J. S. Rankin
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | | | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - F. Bagenal
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - R. W. Ebert
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | | | | | - B. H. Mauk
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - P. W. Valek
- Southwest Research InstituteSan AntonioTXUSA
| | - R. J. Wilson
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
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7
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Szalay JR, Smith HT, Zirnstein EJ, McComas DJ, Begley LJ, Bagenal F, Delamere PA, Wilson RJ, Valek PW, Poppe AR, Nénon Q, Allegrini F, Ebert RW, Bolton SJ. Water-Group Pickup Ions From Europa-Genic Neutrals Orbiting Jupiter. Geophys Res Lett 2022; 49:e2022GL098111. [PMID: 35864892 PMCID: PMC9286426 DOI: 10.1029/2022gl098111] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/28/2022] [Revised: 04/07/2022] [Accepted: 04/08/2022] [Indexed: 06/15/2023]
Abstract
Water-group gas continuously escapes from Jupiter's icy moons to form co-orbiting populations of particles or neutral toroidal clouds. These clouds provide insights into their source moons as they reveal loss processes and compositions of their parent bodies, alter local plasma composition, and act as sources and sinks for magnetospheric particles. We report the first observations of H2 + pickup ions in Jupiter's magnetosphere from 13 to 18 Jovian radii and find a density ratio of H2 +/H+ = 8 ± 4%, confirming the presence of a neutral H2 toroidal cloud. Pickup ion densities monotonically decrease radially beyond 13 R J consistent with an advecting Europa-genic toroidal cloud source. From these observations, we derive a total H2 neutral loss rate from Europa of 1.2 ± 0.7 kg s-1. This provides the most direct estimate of Europa's H2 neutral loss rate to date and underscores the importance of both ion composition and neutral toroidal clouds in understanding satellite-magnetosphere interactions.
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Affiliation(s)
- J. R. Szalay
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - H. T. Smith
- The Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - E. J. Zirnstein
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - D. J. McComas
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - L. J. Begley
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - F. Bagenal
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - P. A. Delamere
- Geophysical InstituteUniversity of Alaska FairbanksFairbanksAKUSA
| | - R. J. Wilson
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - P. W. Valek
- Southwest Research InstituteSan AntonioTXUSA
| | - A. R. Poppe
- Space Sciences LaboratoryUniversity of CaliforniaBerkeleyCAUSA
| | - Q. Nénon
- Institut de Recherche en Astrophysique et PlanétologieCNRS‐UPS‐CNESToulouseFrance
| | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - R. W. Ebert
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
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8
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Hart ST, Dayeh MA, Reisenfeld DB, Janzen PH, McComas DJ, Allegrini F, Fuselier SA, Ogasawara K, Szalay JR, Funsten HO, Petrinec SM. Probing the Magnetosheath Boundaries Using Interstellar Boundary Explorer (IBEX) Orbital Encounters. J Geophys Res Space Phys 2021; 126:e2021JA029278. [PMID: 35865412 PMCID: PMC9286846 DOI: 10.1029/2021ja029278] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/23/2021] [Revised: 06/16/2021] [Accepted: 06/16/2021] [Indexed: 06/15/2023]
Abstract
Inside the magnetosheath, the IBEX-Hi energetic neutral atom (ENA) imager measures a distinct background count rate that is more than 10 times the typical heliospheric ENA emissions observed when IBEX is outside the magnetosheath. The source of this enhancement is magnetosheath ions of solar wind (SW) origin that deflect around the Earth's magnetopause (MP), scatter and neutralize from the anti-sunward part of the IBEX-Hi sunshade, and continue into the instrument as neutral atoms, behaving indistinguishably from ENAs emitted from distant plasma sources. While this background pollutes observations of outer heliospheric ENAs, it provides a clear signature of IBEX crossings over the magnetospheric boundaries. In this study, we investigate IBEX encounters with the magnetosheath boundaries using ∼8 yr of orbital data, and we determine the MP and bow shock (BS) locations derived from this background signal. We find 280 BS crossings from X GSE ∼ 11 Re to X GSE ∼ -36 Re and 241 MP crossings from X GSE ∼ 6 Re to X GSE ∼ -48 Re. We compare IBEX BS and MP crossing locations to those from IMP-8, Geotail, Cluster, Magion-4, ISEE, and Magnetospheric Multiscale Mission, and we find that IBEX crossing locations overlap with the BS and MP locations inferred from these other data sets. In this paper, we demonstrate how IBEX can be used to identify magnetosheath crossings, and extend boundary observations well past the terminator, thus further constraining future models of magnetosheath boundaries. Furthermore, we use the IBEX data set to show observational evidence of near-Earth magnetotail squeezing during periods of strong interplanetary magnetic field B y.
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Affiliation(s)
- S. T. Hart
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - M. A. Dayeh
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | | | - P. H. Janzen
- Department of Physics and AstronomyUniversity of MontanaMissoulaMTUSA
| | - D. J. McComas
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - S. A. Fuselier
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | | | - J. R. Szalay
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | | | - S. M. Petrinec
- Lockheed Martin Advanced Technology CenterPalo AltoCAUSA
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9
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Orsini S, Livi SA, Lichtenegger H, Barabash S, Milillo A, De Angelis E, Phillips M, Laky G, Wieser M, Olivieri A, Plainaki C, Ho G, Killen RM, Slavin JA, Wurz P, Berthelier JJ, Dandouras I, Kallio E, McKenna-Lawlor S, Szalai S, Torkar K, Vaisberg O, Allegrini F, Daglis IA, Dong C, Escoubet CP, Fatemi S, Fränz M, Ivanovski S, Krupp N, Lammer H, Leblanc F, Mangano V, Mura A, Nilsson H, Raines JM, Rispoli R, Sarantos M, Smith HT, Szego K, Aronica A, Camozzi F, Di Lellis AM, Fremuth G, Giner F, Gurnee R, Hayes J, Jeszenszky H, Tominetti F, Trantham B, Balaz J, Baumjohann W, Brienza D, Bührke U, Bush MD, Cantatore M, Cibella S, Colasanti L, Cremonese G, Cremonesi L, D'Alessandro M, Delcourt D, Delva M, Desai M, Fama M, Ferris M, Fischer H, Gaggero A, Gamborino D, Garnier P, Gibson WC, Goldstein R, Grande M, Grishin V, Haggerty D, Holmström M, Horvath I, Hsieh KC, Jacques A, Johnson RE, Kazakov A, Kecskemety K, Krüger H, Kürbisch C, Lazzarotto F, Leblanc F, Leichtfried M, Leoni R, Loose A, Maschietti D, Massetti S, Mattioli F, Miller G, Moissenko D, Morbidini A, Noschese R, Nuccilli F, Nunez C, Paschalidis N, Persyn S, Piazza D, Oja M, Ryno J, Schmidt W, Scheer JA, Shestakov A, Shuvalov S, Seki K, Selci S, Smith K, Sordini R, Svensson J, Szalai L, Toublanc D, Urdiales C, Varsani A, Vertolli N, Wallner R, Wahlstroem P, Wilson P, Zampieri S. SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo. Space Sci Rev 2021; 217:11. [PMID: 33487762 PMCID: PMC7803725 DOI: 10.1007/s11214-020-00787-3] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/02/2020] [Accepted: 12/03/2020] [Indexed: 06/12/2023]
Abstract
The ESA-JAXA BepiColombo mission to Mercury will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric particle dynamics at Mercury as well as their interactions with solar wind, solar radiation, and interplanetary dust. The particle instrument suite SERENA (Search for Exospheric Refilling and Emitted Natural Abundances) is flying in space on-board the BepiColombo Mercury Planetary Orbiter (MPO) and is the only instrument for ion and neutral particle detection aboard the MPO. It comprises four independent sensors: ELENA for neutral particle flow detection, Strofio for neutral gas detection, PICAM for planetary ions observations, and MIPA, mostly for solar wind ion measurements. SERENA is managed by a System Control Unit located inside the ELENA box. In the present paper the scientific goals of this suite are described, and then the four units are detailed, as well as their major features and calibration results. Finally, the SERENA operational activities are shown during the orbital path around Mercury, with also some reference to the activities planned during the long cruise phase.
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Affiliation(s)
- S Orsini
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - S A Livi
- Southwest Research Institute, San Antonio, TX USA
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI USA
| | - H Lichtenegger
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - S Barabash
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - A Milillo
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - E De Angelis
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M Phillips
- Southwest Research Institute, San Antonio, TX USA
| | - G Laky
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - M Wieser
- Swedish Institute of Space Physics, Kiruna, Sweden
| | | | | | - G Ho
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 USA
| | - R M Killen
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - J A Slavin
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI USA
| | - P Wurz
- Physics Institute, University of Bern, Bern, Switzerland
| | | | - I Dandouras
- Institut de Recherche en Astrophysique et Planétologie, CNRS, CNES, Université de Toulouse, Toulouse, France
| | - E Kallio
- School of Electrical Engineering, Department of Electronics and Nanoengineering, Aalto University, Helsinki, Finland
| | | | - S Szalai
- Wigner Research Centre for Physics, Budapest, Hungary
| | - K Torkar
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - O Vaisberg
- IKI Space Research Institute, Moscow, Russia
| | - F Allegrini
- Southwest Research Institute, San Antonio, TX USA
| | - I A Daglis
- Department of Physics, National and Kapodistrian University of Athens, Athens, Greece
- Hellenic Space Center, Athens, Greece
| | - C Dong
- Department of Astrophysical Sciences and Princeton Plasma Physics Laboratory, Princeton University, Princeton, NJ USA
| | | | - S Fatemi
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - M Fränz
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - S Ivanovski
- Astronomical Observatory, INAF, Trieste, Italy
| | - N Krupp
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - H Lammer
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - V Mangano
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - A Mura
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - H Nilsson
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - J M Raines
- Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI USA
| | - R Rispoli
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - M Sarantos
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - H T Smith
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 USA
| | - K Szego
- Wigner Research Centre for Physics, Budapest, Hungary
| | - A Aronica
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | | | | | - G Fremuth
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - F Giner
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - R Gurnee
- Laboratory for Atmospheric and Space Physics, Boulder, CO USA
| | - J Hayes
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 USA
| | - H Jeszenszky
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - B Trantham
- Southwest Research Institute, San Antonio, TX USA
| | - J Balaz
- Institute of Experimental Physics SAS, Slovak Academy of Sciences, 040 01 Košice, Slovakia
| | - W Baumjohann
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - D Brienza
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - U Bührke
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - M D Bush
- Physics Institute, University of Bern, Bern, Switzerland
| | | | - S Cibella
- Istituto di Struttura della Materia (CNR-ISM), 00133 Roma, Italy
| | - L Colasanti
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - G Cremonese
- Astronomical Observatory, INAF, Padova, Italy
| | | | - M D'Alessandro
- Istituto di Struttura della Materia (CNR-ISM), 00133 Roma, Italy
| | | | - M Delva
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - M Desai
- Southwest Research Institute, San Antonio, TX USA
| | - M Fama
- Comisión Nacional de Energía Atómica, cnea, Centro Atómico Bariloche, Bariloche, Argentina
| | - M Ferris
- Southwest Research Institute, San Antonio, TX USA
| | - H Fischer
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - A Gaggero
- Istituto di Struttura della Materia (CNR-ISM), 00133 Roma, Italy
| | - D Gamborino
- Physics Institute, University of Bern, Bern, Switzerland
| | - P Garnier
- Institut de Recherche en Astrophysique et Planétologie, CNRS, CNES, Université de Toulouse, Toulouse, France
| | - W C Gibson
- Southwest Research Institute, San Antonio, TX USA
| | - R Goldstein
- Southwest Research Institute, San Antonio, TX USA
| | - M Grande
- Aberystwyth University, Aberystwyth, Ceredigion SY23 3FL UK
| | - V Grishin
- IKI Space Research Institute, Moscow, Russia
| | - D Haggerty
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 USA
| | - M Holmström
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - I Horvath
- Wigner Research Centre for Physics, Budapest, Hungary
| | - K-C Hsieh
- University of Arizona, Tucson, AZ USA
| | - A Jacques
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - R E Johnson
- University of Virginia, Charlottesville, VA 22904 USA
| | - A Kazakov
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - K Kecskemety
- Wigner Research Centre for Physics, Budapest, Hungary
| | - H Krüger
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - C Kürbisch
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | | | - M Leichtfried
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | | | - A Loose
- Max-Planck-Institut für Sonnensystemforschung, MPS, 37077 Göttingen, Germany
| | - D Maschietti
- Istituto Fotonica e Nanotecnologie, CNR-IFN, Roma, Italy
| | - S Massetti
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | | | - G Miller
- Southwest Research Institute, San Antonio, TX USA
| | - D Moissenko
- IKI Space Research Institute, Moscow, Russia
| | - A Morbidini
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - R Noschese
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - F Nuccilli
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - C Nunez
- Southwest Research Institute, San Antonio, TX USA
| | - N Paschalidis
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771 USA
| | - S Persyn
- Southwest Research Institute, San Antonio, TX USA
| | - D Piazza
- Physics Institute, University of Bern, Bern, Switzerland
| | - M Oja
- Swedish Institute of Space Physics, Kiruna, Sweden
| | - J Ryno
- Finnish Meteorological Institute FMI, Helsinki, Finland
| | - W Schmidt
- Finnish Meteorological Institute FMI, Helsinki, Finland
| | | | - A Shestakov
- IKI Space Research Institute, Moscow, Russia
| | - S Shuvalov
- IKI Space Research Institute, Moscow, Russia
| | - K Seki
- Department of Earth and Planetary Science, Graduate School of Science, University of Tokyo, Tokyo, Japan
| | - S Selci
- Istituto di Struttura della Materia (CNR-ISM), 00133 Roma, Italy
| | - K Smith
- Southwest Research Institute, San Antonio, TX USA
| | - R Sordini
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | | | - L Szalai
- Wigner Research Centre for Physics, Budapest, Hungary
| | - D Toublanc
- Institut de Recherche en Astrophysique et Planétologie, CNRS, CNES, Université de Toulouse, Toulouse, France
| | - C Urdiales
- Southwest Research Institute, San Antonio, TX USA
| | - A Varsani
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - N Vertolli
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
| | - R Wallner
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - P Wahlstroem
- Physics Institute, University of Bern, Bern, Switzerland
| | - P Wilson
- Southwest Research Institute, San Antonio, TX USA
| | - S Zampieri
- Institute of Space Astrophysics and Planetology, INAF, via del Fosso del Cavaliere 100, 00133 Rome, Italy
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10
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Chiappini FA, Allegrini F, Goicoechea HC, Olivieri AC. Sensitivity for Multivariate Calibration Based on Multilayer Perceptron Artificial Neural Networks. Anal Chem 2020; 92:12265-12272. [DOI: 10.1021/acs.analchem.0c01863] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Affiliation(s)
- Fabricio A. Chiappini
- Laboratorio de Desarrollo Analítico y Quimiometría (LADAQ), Cátedra de Química Analítica I, Facultad de Bioquímica y Ciencias Biológicas, Universidad Nacional del Litoral, Ciudad Universitaria, Santa Fe S3000ZAA, Argentina
- Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Godoy Cruz 2290 CABA C1425FQB, Argentina
| | | | - Héctor C. Goicoechea
- Laboratorio de Desarrollo Analítico y Quimiometría (LADAQ), Cátedra de Química Analítica I, Facultad de Bioquímica y Ciencias Biológicas, Universidad Nacional del Litoral, Ciudad Universitaria, Santa Fe S3000ZAA, Argentina
- Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Godoy Cruz 2290 CABA C1425FQB, Argentina
| | - Alejandro C. Olivieri
- Departamento de Química Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET), Suipacha 531, Rosario S2002LRK, Argentina
- Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Godoy Cruz 2290 CABA C1425FQB, Argentina
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11
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Allen RC, Paranicas CP, Bagenal F, Vines SK, Hamilton DC, Allegrini F, Clark G, Delamere PA, Kim TK, Krimigis SM, Mitchell DG, Smith TH, Wilson RJ. Energetic Oxygen and Sulfur Charge States in the Outer Jovian Magnetosphere: Insights From the Cassini Jupiter Flyby. Geophys Res Lett 2019; 46:11709-11717. [PMID: 31894172 PMCID: PMC6919296 DOI: 10.1029/2019gl085185] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/28/2019] [Revised: 10/11/2019] [Accepted: 10/14/2019] [Indexed: 06/10/2023]
Abstract
On 10 January 2001, Cassini briefly entered into the magnetosphere of Jupiter, en route to Saturn. During this excursion into the Jovian magnetosphere, the Cassini Magnetosphere Imaging Instrument/Charge-Energy-Mass Spectrometer detected oxygen and sulfur ions. While Charge-Energy-Mass Spectrometer can distinguish between oxygen and sulfur charge states directly, only 95.9 ± 2.9 keV/e ions were sampled during this interval, allowing for a long time integration of the tenuous outer magnetospheric (~200 RJ) plasma at one energy. For this brief interval for the 95.9 keV/e ions, 96% of oxygen ions were O+, with the other 4% as O2+, while 25% of the energetic sulfur ions were S+, 42% S2+, and 33% S3+. The S2+/O+ flux ratio was observed to be 0.35 (±0.06 Poisson error).
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Affiliation(s)
- R. C. Allen
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - C. P. Paranicas
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - F. Bagenal
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - S. K. Vines
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - D. C. Hamilton
- Department of PhysicsUniversity of MarylandCollege ParkMDUSA
| | - F. Allegrini
- Space Science and Engineering DivisionSouthwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - G. Clark
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - P. A. Delamere
- Geophysical InstituteUniversity of Alaska FairbanksFairbanksAKUSA
| | - T. K. Kim
- Space Science and Engineering DivisionSouthwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - S. M. Krimigis
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - D. G. Mitchell
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - T. H. Smith
- Applied Physics LaboratoryJohns Hopkins UniversityLaurelMDUSA
| | - R. J. Wilson
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
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12
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Ebert RW, Greathouse TK, Clark G, Allegrini F, Bagenal F, Bolton SJ, Connerney JEP, Gladstone GR, Imai M, Hue V, Kurth WS, Levin S, Louarn P, Mauk BH, McComas DJ, Paranicas C, Szalay JR, Thomsen MF, Valek PW, Wilson RJ. Comparing Electron Energetics and UV Brightness in Jupiter's Northern Polar Region During Juno Perijove 5. Geophys Res Lett 2019; 46:19-27. [PMID: 30828110 PMCID: PMC6378591 DOI: 10.1029/2018gl081129] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/29/2018] [Revised: 12/14/2018] [Accepted: 12/20/2018] [Indexed: 05/24/2023]
Abstract
We compare electron and UV observations mapping to the same location in Jupiter's northern polar region, poleward of the main aurora, during Juno perijove 5. Simultaneous peaks in UV brightness and electron energy flux are identified when observations map to the same location at the same time. The downward energy flux during these simultaneous observations was not sufficient to generate the observed UV brightness; the upward energy flux was. We propose that the primary acceleration region is below Juno's altitude, from which the more intense upward electrons originate. For the complete interval, the UV brightness peaked at ~240 kilorayleigh (kR); the downward and upward energy fluxes peaked at 60 and 700 mW/m2, respectively. Increased downward energy fluxes are associated with increased contributions from tens of keV electrons. These observations provide evidence that bidirectional electron beams with broad energy distributions can produce tens to hundreds of kilorayleigh polar UV emissions.
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Affiliation(s)
- R. W. Ebert
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | | | - G. Clark
- Johns Hopkins University Applied Physics LabLaurelMDUSA
| | - F. Allegrini
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - F. Bagenal
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | | | | | - G. R. Gladstone
- Southwest Research InstituteSan AntonioTXUSA
- Department of Physics and AstronomyUniversity of Texas at San AntonioSan AntonioTXUSA
| | - M. Imai
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - V. Hue
- Southwest Research InstituteSan AntonioTXUSA
| | - W. S. Kurth
- Department of Physics and AstronomyUniversity of IowaIowa CityIAUSA
| | - S. Levin
- Jet Propulsion LaboratoryPasadenaCAUSA
| | - P. Louarn
- Institut de Recherche en Astrophysique et PlanétologieToulouseFrance
| | - B. H. Mauk
- Johns Hopkins University Applied Physics LabLaurelMDUSA
| | - D. J. McComas
- Southwest Research InstituteSan AntonioTXUSA
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | - C. Paranicas
- Johns Hopkins University Applied Physics LabLaurelMDUSA
| | - J. R. Szalay
- Department of Astrophysical SciencesPrinceton UniversityPrincetonNJUSA
| | | | - P. W. Valek
- Southwest Research InstituteSan AntonioTXUSA
| | - R. J. Wilson
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
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13
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Ebert RW, Greathouse TK, Clark G, Allegrini F, Bagenal F, Bolton SJ, Connerney JEP, Gladstone GR, Imai M, Hue V, Kurth WS, Levin S, Louarn P, Mauk BH, McComas DJ, Paranicas C, Szalay JR, Thomsen MF, Valek PW, Wilson RJ. Comparing Electron Energetics and UV Brightness in Jupiter's Northern Polar Region During Juno Perijove 5. Geophys Res Lett 2019; 46:19-27. [PMID: 30828110 DOI: 10.1029/2019gl084146] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/29/2018] [Revised: 12/14/2018] [Accepted: 12/20/2018] [Indexed: 05/24/2023]
Abstract
We compare electron and UV observations mapping to the same location in Jupiter's northern polar region, poleward of the main aurora, during Juno perijove 5. Simultaneous peaks in UV brightness and electron energy flux are identified when observations map to the same location at the same time. The downward energy flux during these simultaneous observations was not sufficient to generate the observed UV brightness; the upward energy flux was. We propose that the primary acceleration region is below Juno's altitude, from which the more intense upward electrons originate. For the complete interval, the UV brightness peaked at ~240 kilorayleigh (kR); the downward and upward energy fluxes peaked at 60 and 700 mW/m2, respectively. Increased downward energy fluxes are associated with increased contributions from tens of keV electrons. These observations provide evidence that bidirectional electron beams with broad energy distributions can produce tens to hundreds of kilorayleigh polar UV emissions.
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Affiliation(s)
- R W Ebert
- Southwest Research Institute San Antonio TX USA
- Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
| | | | - G Clark
- Johns Hopkins University Applied Physics Lab Laurel MD USA
| | - F Allegrini
- Southwest Research Institute San Antonio TX USA
- Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
| | - F Bagenal
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder CO USA
| | - S J Bolton
- Southwest Research Institute San Antonio TX USA
| | | | - G R Gladstone
- Southwest Research Institute San Antonio TX USA
- Department of Physics and Astronomy University of Texas at San Antonio San Antonio TX USA
| | - M Imai
- Department of Physics and Astronomy University of Iowa Iowa City IA USA
| | - V Hue
- Southwest Research Institute San Antonio TX USA
| | - W S Kurth
- Department of Physics and Astronomy University of Iowa Iowa City IA USA
| | - S Levin
- Jet Propulsion Laboratory Pasadena CA USA
| | - P Louarn
- Institut de Recherche en Astrophysique et Planétologie Toulouse France
| | - B H Mauk
- Johns Hopkins University Applied Physics Lab Laurel MD USA
| | - D J McComas
- Southwest Research Institute San Antonio TX USA
- Department of Astrophysical Sciences Princeton University Princeton NJ USA
| | - C Paranicas
- Johns Hopkins University Applied Physics Lab Laurel MD USA
| | - J R Szalay
- Department of Astrophysical Sciences Princeton University Princeton NJ USA
| | | | - P W Valek
- Southwest Research Institute San Antonio TX USA
| | - R J Wilson
- Laboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder CO USA
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14
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Pellegrino Vidal RB, Allegrini F, Olivieri AC. The effect of constraints on the analytical figures of merit achieved by extended multivariate curve resolution-alternating least-squares. Anal Chim Acta 2018; 1003:10-15. [DOI: 10.1016/j.aca.2017.12.008] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/10/2017] [Revised: 10/30/2017] [Accepted: 12/11/2017] [Indexed: 11/30/2022]
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15
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Connerney JEP, Adriani A, Allegrini F, Bagenal F, Bolton SJ, Bonfond B, Cowley SWH, Gerard JC, Gladstone GR, Grodent D, Hospodarsky G, Jorgensen JL, Kurth WS, Levin SM, Mauk B, McComas DJ, Mura A, Paranicas C, Smith EJ, Thorne RM, Valek P, Waite J. Jupiter's magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits. Science 2018; 356:826-832. [PMID: 28546207 DOI: 10.1126/science.aam5928] [Citation(s) in RCA: 94] [Impact Index Per Article: 15.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/13/2016] [Accepted: 04/20/2017] [Indexed: 11/02/2022]
Abstract
The Juno spacecraft acquired direct observations of the jovian magnetosphere and auroral emissions from a vantage point above the poles. Juno's capture orbit spanned the jovian magnetosphere from bow shock to the planet, providing magnetic field, charged particle, and wave phenomena context for Juno's passage over the poles and traverse of Jupiter's hazardous inner radiation belts. Juno's energetic particle and plasma detectors measured electrons precipitating in the polar regions, exciting intense aurorae, observed simultaneously by the ultraviolet and infrared imaging spectrographs. Juno transited beneath the most intense parts of the radiation belts, passed about 4000 kilometers above the cloud tops at closest approach, well inside the jovian rings, and recorded the electrical signatures of high-velocity impacts with small particles as it traversed the equator.
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Affiliation(s)
- J E P Connerney
- Space Research Corporation, Annapolis, MD 21403, USA. .,NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - A Adriani
- Institute for Space Astrophysics and Planetology, National Institute for Astrophysics, Rome, 00133, Italy
| | - F Allegrini
- Southwest Research Institute, San Antonio, TX 78238, USA
| | - F Bagenal
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA
| | - S J Bolton
- Southwest Research Institute, San Antonio, TX 78238, USA
| | - B Bonfond
- Institut d'Astrophysique et de Geophysique, Universite de Liege, Liege, B-4000 Belgium
| | | | - J-C Gerard
- Institut d'Astrophysique et de Geophysique, Universite de Liege, Liege, B-4000 Belgium
| | - G R Gladstone
- Southwest Research Institute, San Antonio, TX 78238, USA
| | - D Grodent
- Institut d'Astrophysique et de Geophysique, Universite de Liege, Liege, B-4000 Belgium
| | | | - J L Jorgensen
- National Space Institute, Technical University of Denmark, Kongens Lyngby, 2800, Denmark
| | - W S Kurth
- University of Iowa, Iowa City, IA 52242, USA
| | - S M Levin
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA 91109, USA
| | - B Mauk
- Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, USA
| | - D J McComas
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - A Mura
- Institute for Space Astrophysics and Planetology, National Institute for Astrophysics, Rome, 00133, Italy
| | - C Paranicas
- Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, USA
| | - E J Smith
- Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA 91109, USA
| | - R M Thorne
- Department of Atmospheric and Oceanic Sciences, University of California-Los Angeles, Los Angeles, CA 90095, USA
| | - P Valek
- Southwest Research Institute, San Antonio, TX 78238, USA
| | - J Waite
- Southwest Research Institute, San Antonio, TX 78238, USA
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16
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Mastroianni A, Allegrini F, Nardi S, Donatucci D, Girelli F, Guidi C. Carpal tunnel syndrome in HIV-positive patients coinfected with HCV. Reumatismo 2017; 69:164-169. [PMID: 29320842 DOI: 10.4081/reumatismo.2017.1010] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/09/2017] [Accepted: 08/02/2017] [Indexed: 11/23/2022] Open
Abstract
A wide range of rheumatic and peripheral nervous system disorders may develop in patients with HIV infection, leading to pain, sensory symptoms, and muscle weakness. Over the past three decades, the progress in management of HIV disease with anti-retroviral therapy (ART) has resulted in increased life expectancy for people living with HIV disease. With this new chronicity of the disease has a constellation of chronic musculoskeletal, orthopaedic and rheumatic manifestations has emerged, as potential complications of the disease itself and/or the results of ART treatment regimen and/or because of expected age-related symptoms/manifestations. The incidence of CTS in the general population is around 3.8% with clinical examination and, when electroneuromyography is used, it is 2.7%. In the HIV-positive population, the incidence is very close to that of the general population. The aim of this study was to evaluate the incidence of CTS and to identify factors influencing the development of CTS in HIV-infected patients attending our clinic. This syndrome has been associated with advanced HIV disease and the use of ART possibly due to an increased inflammatory state and the presence of concurrent HCV infection.
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Affiliation(s)
- A Mastroianni
- Unità Operativa Malattie Infettive, Presidio Ospedaliero G.B. Morgagni - L. Pierantoni, Forlì.
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17
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Abstract
With the proliferation of multivariate calibration methods based on artificial neural networks, expressions for the estimation of figures of merit such as sensitivity, prediction uncertainty, and detection limit are urgently needed. This would bring nonlinear multivariate calibration methodologies to the same status as the linear counterparts in terms of comparability. Currently only the average prediction error or the ratio of performance to deviation for a test sample set is employed to characterize and promote neural network calibrations. It is clear that additional information is required. We report for the first time expressions that easily allow one to compute three relevant figures: (1) the sensitivity, which turns out to be sample-dependent, as expected, (2) the prediction uncertainty, and (3) the detection limit. The approach resembles that employed for linear multivariate calibration, i.e., partial least-squares regression, specifically adapted to neural network calibration scenarios. As usual, both simulated and real (near-infrared) spectral data sets serve to illustrate the proposal.
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Affiliation(s)
- Franco Allegrini
- Departamento de Química Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET) , Suipacha 531, Rosario S2002LRK, Argentina
| | - Alejandro C Olivieri
- Departamento de Química Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET) , Suipacha 531, Rosario S2002LRK, Argentina
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18
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Allegrini F, Wentzell PD, Olivieri AC. Generalized error-dependent prediction uncertainty in multivariate calibration. Anal Chim Acta 2016; 903:51-60. [DOI: 10.1016/j.aca.2015.11.028] [Citation(s) in RCA: 22] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/31/2015] [Revised: 11/19/2015] [Accepted: 11/23/2015] [Indexed: 11/29/2022]
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19
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Desai MI, Ogasawara K, Ebert RW, McComas DJ, Allegrini F, Weidner SE, Alexander N, Livi SA. An integrated time-of-flight versus residual energy subsystem for a compact dual ion composition experiment for space plasmas. Rev Sci Instrum 2015; 86:054501. [PMID: 26026539 DOI: 10.1063/1.4921706] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/04/2023]
Abstract
We have developed a novel concept for a Compact Dual Ion Composition Experiment (CoDICE) that simultaneously provides high quality plasma and energetic ion composition measurements over 6 decades in ion energy in a wide variety of space plasma environments. CoDICE measures the two critical ion populations in space plasmas: (1) mass and ionic charge state composition and 3D velocity and angular distributions of ∼10 eV/q-40 keV/q plasma ions—CoDICE-Lo and (2) mass composition, energy spectra, and angular distributions of ∼30 keV-10 MeV energetic ions—CoDICE-Hi. CoDICE uses a common, integrated Time-of-Flight (TOF) versus residual energy (E) subsystem for measuring the two distinct ion populations. This paper describes the CoDICE design concept, and presents results of the laboratory tests of the TOF portion of the TOF vs. E subsystem, focusing specifically on (1) investigation of spill-over and contamination rates on the start and stop microchannel plate (MCP) anodes vs. secondary electron steering and focusing voltages, scanned around their corresponding model-optimized values, (2) TOF measurements and resolution and angular resolution, and (3) cross-contamination of the start and stop MCPs' singles rates from CoDICE-Lo and -Hi, and (4) energy resolution of avalanche photodiodes near the lower end of the CoDICE-Lo energy range. We also discuss physical effects that could impact the performance of the TOF vs. E subsystem in a flight instrument. Finally, we discuss advantages of the CoDICE design concept by comparing with capabilities and resources of existing flight instruments.
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Affiliation(s)
- M I Desai
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - K Ogasawara
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - R W Ebert
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - D J McComas
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - F Allegrini
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - S E Weidner
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - N Alexander
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
| | - S A Livi
- Space Science and Engineering Division, Southwest Research Institute, 6220 Culebra Road, San Antonio, Texas 78238-5166, USA
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20
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Ruckebusch C, Bernex R, Allegrini F, Sliwa M, Hofkens J, Dedecker P. Mapping Pixel Dissimilarity in Wide-Field Super-Resolution Fluorescence Microscopy. Anal Chem 2015; 87:4675-82. [PMID: 25844921 DOI: 10.1021/ac504295p] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/02/2023]
Affiliation(s)
- Cyril Ruckebusch
- Université de Lille Sciences et technologies, LASIR CNRS, 59655 Villeneuve d’Ascq
cedex, France
| | - Romain Bernex
- Université de Lille Sciences et technologies, LASIR CNRS, 59655 Villeneuve d’Ascq
cedex, France
| | - Franco Allegrini
- Université de Lille Sciences et technologies, LASIR CNRS, 59655 Villeneuve d’Ascq
cedex, France
- Departamento
de Química Analítica, Facultad de Ciencias Bioquímicas
y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET), Suipacha 531, Rosario S2002LRK, Argentina
| | - Michel Sliwa
- Université de Lille Sciences et technologies, LASIR CNRS, 59655 Villeneuve d’Ascq
cedex, France
| | - Johan Hofkens
- Department
of Chemistry, KU Leuven, Celestijnenlaan 200F, 3001 Heverlee, Belgium
| | - Peter Dedecker
- Department
of Chemistry, KU Leuven, Celestijnenlaan 200F, 3001 Heverlee, Belgium
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21
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Affiliation(s)
- Franco Allegrini
- Departamento de Química
Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET), Suipacha 531, Rosario S2002LRK, Argentina
| | - Alejandro C. Olivieri
- Departamento de Química
Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario, Instituto de Química de Rosario (IQUIR-CONICET), Suipacha 531, Rosario S2002LRK, Argentina
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22
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Allegrini F, Desai MI, Livi S, McComas DJ, Ho GC. The SupraThermal Ion Monitor for space weather predictions. Rev Sci Instrum 2014; 85:054501. [PMID: 24880387 DOI: 10.1063/1.4873327] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Measurement of suprathermal energy ions in the heliosphere has always been challenging because (1) these ions are situated in the energy regime only a few times higher than the solar wind plasma, where intensities are orders of magnitude higher and (2) ion energies are below or close to the threshold of state-of-art solid-state detectors. Suprathermal ions accelerated at coronal mass ejection-driven shocks propagate out ahead of the shocks. These shocks can cause geomagnetic storms in the Earth's magnetosphere that can affect spacecraft and ground-based power and communication systems. An instrument with sufficient sensitivity to measure these ions can be used to predict the arrival of the shocks and provide an advance warning for potentially geo-effective space weather. In this paper, we present a novel energy analyzer concept, the Suprathermal Ion Monitor (STIM) that is designed to measure suprathermal ions with high sensitivity. We show results from a laboratory prototype and demonstrate the feasibility of the concept. A list of key performances is given, as well as a discussion of various possible detectors at the back end. STIM is an ideal candidate for a future space weather monitor in orbit upstream of the near-earth environment, for example, around L1. A scaled-down version is suitable for a CubeSat mission. Such a platform allows proofing the concept and demonstrating its performance in the space environment.
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Affiliation(s)
- F Allegrini
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228, USA and Physics and Astronomy Department, University of Texas at San Antonio, San Antonio, Texas 78249, USA
| | - M I Desai
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228, USA and Physics and Astronomy Department, University of Texas at San Antonio, San Antonio, Texas 78249, USA
| | - S Livi
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228, USA and Physics and Astronomy Department, University of Texas at San Antonio, San Antonio, Texas 78249, USA
| | - D J McComas
- Southwest Research Institute, P.O. Drawer 28510, San Antonio, Texas 78228, USA and Physics and Astronomy Department, University of Texas at San Antonio, San Antonio, Texas 78249, USA
| | - G C Ho
- Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland 20723, USA
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23
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Allegrini F, Olivieri AC. An integrated approach to the simultaneous selection of variables, mathematical pre-processing and calibration samples in partial least-squares multivariate calibration. Talanta 2013; 115:755-60. [DOI: 10.1016/j.talanta.2013.06.051] [Citation(s) in RCA: 20] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/02/2013] [Revised: 06/24/2013] [Accepted: 06/25/2013] [Indexed: 10/26/2022]
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24
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Clark G, Allegrini F, Randol BM, McComas DJ, Louarn P. Response in electrostatic analyzers due to backscattered electrons: case study analysis with the Juno Jovian Auroral Distribution Experiment-Electron instrument. Rev Sci Instrum 2013; 84:105109. [PMID: 24182165 DOI: 10.1063/1.4824352] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
In this study, we introduce a model to characterize electron scattering in an electrostatic analyzer. We show that electrons between 0.5 and 30 keV scatter from internal surfaces to produce a response up to ~20% of the ideal, unscattered response. We compare our model results to laboratory data from the Jovian Auroral Distribution Experiment-Electron sensor onboard the NASA Juno mission. Our model reproduces the measured energy-angle response of the instrument well. Understanding and quantifying this scattering process is beneficial to the analysis of scientific data as well as future instrument optimization.
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Affiliation(s)
- G Clark
- Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, Texas 78249, USA
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25
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Affiliation(s)
- Franco Allegrini
- Departamento de Química
Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario and Instituto de Química Rosario (IQUIR-CONICET), Suipacha 531, Rosario (S2002LRK), Argentina
| | - Alejandro C. Olivieri
- Departamento de Química
Analítica, Facultad de Ciencias Bioquímicas y Farmacéuticas, Universidad Nacional de Rosario and Instituto de Química Rosario (IQUIR-CONICET), Suipacha 531, Rosario (S2002LRK), Argentina
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26
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Randol BM, Ebert RW, Allegrini F, McComas DJ, Schwadron NA. Reflections of ions in electrostatic analyzers: a case study with New Horizons/Solar Wind Around Pluto. Rev Sci Instrum 2010; 81:114501. [PMID: 21133487 DOI: 10.1063/1.3499367] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/30/2023]
Abstract
Electrostatic analyzers (ESAs), in various forms, are used to measure plasma in a range of applications. In this article, we describe how ions reflect from the interior surfaces of an ESA, the detection of which constitutes a fundamentally nonideal response of ESAs. We demonstrate this effect by comparing laboratory data from a real ESA-based space instrument, the Solar Wind Around Pluto (SWAP) instrument, aboard the NASA New Horizons spacecraft, to results from a model based on quantum mechanical simulations of particles reflected from the instrument's surfaces combined with simulations of particle trajectories through the instrument's applied electrostatic fields. Thus, we show, for the first time, how reflected ions in ESAs lead to nonideal effects that have important implications for understanding the data returned by these instruments, as well as for designing new low-background ESA-based instruments. Specifically, we show that the response of SWAP widens considerably below a level of 10(-3) of the peak response. Thus, a direct measurement of a plasma distribution with SWAP will have an energy-dependent background on the order of ≤10(-3) of the peak of the signal due to that distribution. We predict that this order of magnitude estimate for the background applies to a large number of ESA-based instruments because ESAs operate using a common principle. However, the exact shape of the energy-dependent response will be different for different instruments. The principle of operation is that ions outside the ideal range of energy-per-charge are deflected into the walls of the ESA. Therefore, we propose that a new design paradigm is necessary to mitigate the effect of ion reflections and thus accurately and directly measure the energy spectrum of a plasma using ESAs. In this article, we build a framework for minimizing the effect of ion reflections in the design of new ESAs. Through the use of existing computer simulation software, a design team can use our method to quantify the amount of reflections in their instrument and iteratively change design parameters before fabrication, conserving resources. A possible direction for the new design paradigm is having nonsolid walls of the ESA, already used in some applications.
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Affiliation(s)
- B M Randol
- Department of Physics and Astronomy, University of Texas at San Antonio, San Antonio, Texas 78229, USA
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27
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McComas DJ, Allegrini F, Bochsler P, Bzowski M, Christian ER, Crew GB, DeMajistre R, Fahr H, Fichtner H, Frisch PC, Funsten HO, Fuselier SA, Gloeckler G, Gruntman M, Heerikhuisen J, Izmodenov V, Janzen P, Knappenberger P, Krimigis S, Kucharek H, Lee M, Livadiotis G, Livi S, MacDowall RJ, Mitchell D, Möbius E, Moore T, Pogorelov NV, Reisenfeld D, Roelof E, Saul L, Schwadron NA, Valek PW, Vanderspek R, Wurz P, Zank GP. Global observations of the interstellar interaction from the Interstellar Boundary Explorer (IBEX). Science 2009; 326:959-962. [PMID: 19833923 DOI: 10.1007/s11214-009-9499-4] [Citation(s) in RCA: 23] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/17/2008] [Accepted: 03/23/2009] [Indexed: 05/23/2023]
Abstract
The Sun moves through the local interstellar medium, continuously emitting ionized, supersonic solar wind plasma and carving out a cavity in interstellar space called the heliosphere. The recently launched Interstellar Boundary Explorer (IBEX) spacecraft has completed its first all-sky maps of the interstellar interaction at the edge of the heliosphere by imaging energetic neutral atoms (ENAs) emanating from this region. We found a bright ribbon of ENA emission, unpredicted by prior models or theories, that may be ordered by the local interstellar magnetic field interacting with the heliosphere. This ribbon is superposed on globally distributed flux variations ordered by both the solar wind structure and the direction of motion through the interstellar medium. Our results indicate that the external galactic environment strongly imprints the heliosphere.
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Affiliation(s)
- D J McComas
- Southwest Research Institute, San Antonio, TX 78228, USA.
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28
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Fuselier SA, Allegrini F, Funsten HO, Ghielmetti AG, Heirtzler D, Kucharek H, Lennartsson OW, McComas DJ, Möbius E, Moore TE, Petrinec SM, Saul LA, Scheer JA, Schwadron N, Wurz P. Width and variation of the ENA flux ribbon observed by the Interstellar Boundary Explorer. Science 2009; 326:962-4. [PMID: 19833916 DOI: 10.1126/science.1180981] [Citation(s) in RCA: 143] [Impact Index Per Article: 9.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The dominant feature in Interstellar Boundary Explorer (IBEX) sky maps of heliospheric energetic neutral atom (ENA) flux is a ribbon of enhanced flux that extends over a broad range of ecliptic latitudes and longitudes. It is narrow (approximately 20 degrees average width) but long (extending over 300 degrees in the sky) and is observed at energies from 0.2 to 6 kilo-electron volts. We demonstrate that the flux in the ribbon is a factor of 2 to 3 times higher than that of the more diffuse, globally distributed heliospheric ENA flux. The ribbon is most pronounced at approximately 1 kilo-electron volt. The average width of the ribbon is nearly constant, independent of energy. The ribbon is likely the result of an enhancement in the combined solar wind and pickup ion populations in the heliosheath.
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Affiliation(s)
- S A Fuselier
- Lockheed Martin Advanced Technology Center, Palo Alto, CA 94304, USA.
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29
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McComas DJ, Allegrini F, Bochsler P, Bzowski M, Christian ER, Crew GB, DeMajistre R, Fahr H, Fichtner H, Frisch PC, Funsten HO, Fuselier SA, Gloeckler G, Gruntman M, Heerikhuisen J, Izmodenov V, Janzen P, Knappenberger P, Krimigis S, Kucharek H, Lee M, Livadiotis G, Livi S, MacDowall RJ, Mitchell D, Möbius E, Moore T, Pogorelov NV, Reisenfeld D, Roelof E, Saul L, Schwadron NA, Valek PW, Vanderspek R, Wurz P, Zank GP. Global observations of the interstellar interaction from the Interstellar Boundary Explorer (IBEX). Science 2009; 326:959-62. [PMID: 19833923 DOI: 10.1126/science.1180906] [Citation(s) in RCA: 390] [Impact Index Per Article: 26.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Sun moves through the local interstellar medium, continuously emitting ionized, supersonic solar wind plasma and carving out a cavity in interstellar space called the heliosphere. The recently launched Interstellar Boundary Explorer (IBEX) spacecraft has completed its first all-sky maps of the interstellar interaction at the edge of the heliosphere by imaging energetic neutral atoms (ENAs) emanating from this region. We found a bright ribbon of ENA emission, unpredicted by prior models or theories, that may be ordered by the local interstellar magnetic field interacting with the heliosphere. This ribbon is superposed on globally distributed flux variations ordered by both the solar wind structure and the direction of motion through the interstellar medium. Our results indicate that the external galactic environment strongly imprints the heliosphere.
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Affiliation(s)
- D J McComas
- Southwest Research Institute, San Antonio, TX 78228, USA.
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30
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Funsten HO, Allegrini F, Crew GB, DeMajistre R, Frisch PC, Fuselier SA, Gruntman M, Janzen P, McComas DJ, Möbius E, Randol B, Reisenfeld DB, Roelof EC, Schwadron NA. Structures and spectral variations of the outer heliosphere in IBEX energetic neutral atom maps. Science 2009; 326:964-6. [PMID: 19833918 DOI: 10.1126/science.1180927] [Citation(s) in RCA: 173] [Impact Index Per Article: 11.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Interstellar Boundary Explorer (IBEX) has obtained all-sky images of energetic neutral atoms emitted from the heliosheath, located between the solar wind termination shock and the local interstellar medium (LISM). These flux maps reveal distinct nonthermal (0.2 to 6 kilo-electron volts) heliosheath proton populations with spectral signatures ordered predominantly by ecliptic latitude. The maps show a globally distributed population of termination-shock-heated protons and a superimposed ribbonlike feature that forms a circular arc in the sky centered on ecliptic coordinate (longitude lambda, latitude beta) = (221 degrees, 39 degrees), probably near the direction of the LISM magnetic field. Over the IBEX energy range, the ribbon's nonthermal ion pressure multiplied by its radial thickness is in the range of 70 to 100 picodynes per square centimeter AU (AU, astronomical unit), which is significantly larger than the 30 to 60 picodynes per square centimeter AU of the globally distributed population.
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Affiliation(s)
- H O Funsten
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA.
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Allegrini F, Desai MI, Livi R, Livi S, McComas DJ, Randol B. The entrance system laboratory prototype for an advanced mass and ionic charge composition experiment. Rev Sci Instrum 2009; 80:104502. [PMID: 19895078 DOI: 10.1063/1.3247906] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/28/2023]
Abstract
Electrostatic analyzers (ESA) have been used extensively for the characterization of plasmas in a variety of space environments. They vary in shape, geometry, and size and are adapted to the specific particle population to be measured and the configuration of the spacecraft. Their main function is to select the energy per charge of the particles within a passband. An energy-per-charge range larger than that of the passband can be sampled by varying the voltage difference between the ESA electrodes. The voltage sweep takes time and reduces the duty cycle for a particular energy-per-charge passband. Our design approach for an advanced mass and ionic charge composition experiment (AMICCE) has a novel electrostatic analyzer that essentially serves as a spectrograph and selects ions simultaneously over a broad range of energy-per-charge (E/q). Only three voltage settings are required to cover the entire range from approximately 10 to 270 keV/q, thus dramatically increasing the product of the geometric factor times the duty cycle when compared with other instruments. In this paper, we describe the AMICCE concept with particular emphasis on the prototype of the entrance system (ESA and collimator), which we designed, developed, and tested. We also present comparisons of the laboratory results with electrostatic simulations.
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Affiliation(s)
- F Allegrini
- Southwest Research Institute, San Antonio, Texas 78238, USA
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Allegrini F, Ebert RW, Alquiza J, Broiles T, Dunn C, McComas DJ, Silva I, Valek P, Westlake J. A mass analysis technique using coincidence measurements from the Interstellar Boundary Explorer-Hi (approximately 0.3- approximately 6 keV) detector. Rev Sci Instrum 2008; 79:096107. [PMID: 19044461 DOI: 10.1063/1.2987691] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
NASA's Interstellar Boundary Explorer (IBEX) mission, scheduled to launch in October 2008, will make the first observations of charge exchange energetic neutral atoms (ENAs) produced near the edge of the heliosphere. IBEX will measure these ENAs with two ultra-high sensitivity, single-pixel ENA sensors in the energy range of approximately 0.01- approximately 2 keV (IBEX-Lo) and approximately 0.3- approximately 6 keV (IBEX-Hi), respectively. The primary purpose of IBEX is to measure hydrogen ENAs from the outer heliosphere, but it will also be sensitive to heavier species of ENAs produced anywhere throughout the solar system. For this study, we measured the coincidence response of the IBEX-Hi detector section to H, He, N, and O ions. Based on these results, we have developed an innovative technique in estimating the hydrogen to heavy ion ratio in the signal. This new technique can be applied more widely than the IBEX-Hi detector section, and the basic principle may be useful for other, future space and ground-based measurements.
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Affiliation(s)
- F Allegrini
- Space Science and Engineering Division, Southwest Research Institute, San Antonio, Texas 78238, USA
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Prested C, Schwadron N, Passuite J, Randol B, Stuart B, Crew G, Heerikhuisen J, Pogorelov N, Zank G, Opher M, Allegrini F, McComas DJ, Reno M, Roelof E, Fuselier S, Funsten H, Moebius E, Saul L. Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007ja012758] [Citation(s) in RCA: 60] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- C. Prested
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
| | - N. Schwadron
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
| | - J. Passuite
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
| | - B. Randol
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
- Space Science and Engineering Division; Southwest Research Institute; San Antonio Texas USA
| | - B. Stuart
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
- Institute for Astronomy; University of Hawaii; Honolulu Hawaii USA
| | - G. Crew
- Department of Astronomy, Center for Space Physics and Center for Integrated Space Weather Modeling; Boston University; Boston Massachusetts USA
- Kavli Institute for Astrophysics and Space Research; Massachusetts Institute for Technology; Cambridge Massachusetts USA
| | - J. Heerikhuisen
- Institute of Geophysics and Planetary Physics; University of California; Riverside California USA
| | - N. Pogorelov
- Institute of Geophysics and Planetary Physics; University of California; Riverside California USA
| | - G. Zank
- Institute of Geophysics and Planetary Physics; University of California; Riverside California USA
| | - M. Opher
- Department of Physics and Astronomy; George Mason University; Fairfax Virginia USA
| | - F. Allegrini
- Space Science and Engineering Division; Southwest Research Institute; San Antonio Texas USA
| | - D. J. McComas
- Space Science and Engineering Division; Southwest Research Institute; San Antonio Texas USA
| | - M. Reno
- Space Science and Engineering Division; Southwest Research Institute; San Antonio Texas USA
| | - E. Roelof
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - S. Fuselier
- Space Physics Laboratory; Lockheed Martin; Palo Alto California USA
| | - H. Funsten
- Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - E. Moebius
- Space Science Center and Department of Physics; University of New Hampshire; Durham New Hampshire USA
| | - L. Saul
- Physikalisches Institut, Space and Planetary Sciences; University of Bern; Bern Switzerland
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McComas DJ, Allegrini F, Bagenal F, Crary F, Ebert RW, Elliott H, Stern A, Valek P. Diverse plasma populations and structures in Jupiter's magnetotail. Science 2007; 318:217-20. [PMID: 17932282 DOI: 10.1126/science.1147393] [Citation(s) in RCA: 77] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Jupiter's magnetotail is the largest cohesive structure in the solar system and marks the loss of vast numbers of heavy ions from the Jupiter system. The New Horizons spacecraft traversed the magnetotail to distances exceeding 2500 jovian radii (R(J)) and revealed a remarkable diversity of plasma populations and structures throughout its length. Ions evolve from a hot plasma disk distribution at approximately 100 R(J) to slower, persistent flows down the tail that become increasingly variable in flux and mean energy. The plasma is highly structured-exhibiting sharp breaks, smooth variations, and apparent plasmoids-and contains ions from both Io and Jupiter's ionosphere with intense bursts of H(+) and H(+)(3). Quasi-periodic changes were seen in flux at approximately 450 and approximately 1500 R(J) with a 10-hour period. Other variations in flow speed at approximately 600 to 1000 R(J) with a 3- to 4-day period may be attributable to plasmoids moving down the tail.
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Affiliation(s)
- D J McComas
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA.
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Alessandrini F, Allegrini F, Baldari U, Cancellieri C. Widespread cutaneous cryptococcosis occurring in an immunocompromised patient treated with high doses of fluconazole for oro-pharyngeal candidosis. Acta Derm Venereol 1997; 77:480. [PMID: 9394988 DOI: 10.2340/0001555577480] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [MESH Headings] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/05/2023] Open
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