Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus
Justin C. Kasper,Justin C. Kasper,R. Abiad,Gerry Austin,Marianne Balat-Pichelin,Stuart D. Bale,John W. Belcher,Peter Berg,Henry Bergner,Matthieu Berthomier,Jay Bookbinder,Etienne Brodu,David Caldwell,Anthony W. Case,Benjamin D. G. Chandran,Peter Cheimets,Jonathan Cirtain,Steven R. Cranmer,D. W. Curtis,Peter Daigneau,Greg Dalton,Brahmananda Dasgupta,David DeTomaso,M. Diaz-Aguado,Blagoje Djordjevic,Bill Donaskowski,Michael Effinger,Vladimir Florinski,N. J. Fox,Mark D. Freeman,Dennis L. Gallagher,S. Peter Gary,T. Gauron,Richard Gates,M. L. Goldstein,Leon Golub,D. Gordon,R. S. Gurnee,Giora Guth,Jasper Halekas,Ken Hatch,Jacob Heerikuisen,George C. Ho,Qiang Hu,Greg Johnson,Steven P. Jordan,Kelly E. Korreck,Davin Larson,Alan J. Lazarus,Gang Li,Roberto Livi,Michael Ludlam,Milan Maksimovic,James P. McFadden,William Marchant,B. Maruca,David J. McComas,David J. McComas,Luciana Messina,Tony Mercer,Sang Park,Andrew M. Peddie,Nikolai V. Pogorelov,Matthew J. Reinhart,John D. Richardson,M. S. Robinson,Irene Rosen,Ruth M. Skoug,Amanda Slagle,John T. Steinberg,Michael L. Stevens,Adam Szabo,E. Taylor,Chris Tiu,Paul Turin,Marco Velli,G. M. Webb,Phyllis Whittlesey,K. H. Wright,S. T. Wu,Gary P. Zank +80 more
TLDR
The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Solar Probe Plus is a four sensor instrument suite that provides complete measurements of the electrons and ionized helium and hydrogen that constitute the bulk of solar wind and coronal plasma.Abstract:
The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Solar Probe Plus is a four sensor instrument suite that provides complete measurements of the electrons and ionized helium and hydrogen that constitute the bulk of solar wind and coronal plasma. SWEAP consists of the Solar Probe Cup (SPC) and the Solar Probe Analyzers (SPAN). SPC is a Faraday Cup that looks directly at the Sun and measures ion and electron fluxes and flow angles as a function of energy. SPAN consists of an ion and electron electrostatic analyzer (ESA) on the ram side of SPP (SPAN-A) and an electron ESA on the anti-ram side (SPAN-B). The SPAN-A ion ESA has a time of flight section that enables it to sort particles by their mass/charge ratio, permitting differentiation of ion species. SPAN-A and -B are rotated relative to one another so their broad fields of view combine like the seams on a baseball to view the entire sky except for the region obscured by the heat shield and covered by SPC. Observations by SPC and SPAN produce the combined field of view and measurement capabilities required to fulfill the science objectives of SWEAP and Solar Probe Plus. SWEAP measurements, in concert with magnetic and electric fields, energetic particles, and white light contextual imaging will enable discovery and understanding of solar wind acceleration and formation, coronal and solar wind heating, and particle acceleration in the inner heliosphere of the solar system. SPC and SPAN are managed by the SWEAP Electronics Module (SWEM), which distributes power, formats onboard data products, and serves as a single electrical interface to the spacecraft. SWEAP data products include ion and electron velocity distribution functions with high energy and angular resolution. Full resolution data are stored within the SWEM, enabling high resolution observations of structures such as shocks, reconnection events, and other transient structures to be selected for download after the fact. This paper describes the implementation of the SWEAP Investigation, the driving requirements for the suite, expected performance of the instruments, and planned data products, as of mission preliminary design review.read more
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Journal ArticleDOI
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star
N. J. Fox,Marco Velli,Stuart D. Bale,R. B. Decker,Andrew Driesman,Russell A. Howard,Justin C. Kasper,Justin C. Kasper,James Kinnison,M. Kusterer,David Lario,Mary Kae Lockwood,David J. McComas,David J. McComas,N.-E. Raouafi,Adam Szabo +15 more
TL;DR: The first spacecraft to fly into the low solar corona is the Solar Probe Plus (SPP) as discussed by the authors, which is scheduled for launch in mid-2018 and will perform 24 orbits over a 7-year nominal mission duration.
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The FIELDS Instrument Suite for Solar Probe Plus: Measuring the Coronal Plasma and Magnetic Field, Plasma Waves and Turbulence, and Radio Signatures of Solar Transients.
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TL;DR: The scientific objectives targeted by the SPP/FIELDS instrument, the instrument design itself, and the instrument concept of operations and planned data products are described.
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Highly structured slow solar wind emerging from an equatorial coronal hole
Stuart D. Bale,Samuel T. Badman,John W. Bonnell,Trevor A. Bowen,David Burgess,Anthony W. Case,Cynthia A Cattell,Benjamin D. G. Chandran,C. C. Chaston,Christopher H. K. Chen,James Drake,T. Dudok de Wit,Jonathan Eastwood,Robert E. Ergun,William M. Farrell,C. Fong,Keith Goetz,Melvyn L. Goldstein,Melvyn L. Goldstein,Katherine Goodrich,Peter Harvey,Timothy S. Horbury,Gregory G. Howes,Justin C. Kasper,Justin C. Kasper,Paul J. Kellogg,James A. Klimchuk,Kelly E. Korreck,Vladimir Krasnoselskikh,Säm Krucker,Säm Krucker,R. Laker,Davin Larson,Robert J. MacDowall,Milan Maksimovic,David M. Malaspina,J. C. Martínez-Oliveros,D. J. McComas,Nicole Meyer-Vernet,Michel Moncuquet,F. S. Mozer,Tai Phan,Marc Pulupa,N.-E. Raouafi,Chadi Salem,David Stansby,Michael L. Stevens,Adam Szabo,Marco Velli,T. Woolley,John R. Wygant +50 more
TL;DR: Measurements from the Parker Solar Probe show that slow solar wind near the Sun’s equator originates in coronal holes, and plasma-wave measurements suggest the existence of electron and ion velocity-space micro-instabilities that are associated with plasma heating and thermalization processes.
Journal ArticleDOI
Alfvénic velocity spikes and rotational flows in the near-Sun solar wind
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TL;DR: Observations of solar-wind plasma at heliocentric distances of about 35 solar radii reveal an increasing rotational component to the flow velocity of the solar wind around the Sun, peaking at 35 to 50 kilometres per second—considerably above the amplitude of the waves.
Journal ArticleDOI
Recent progress in astrophysical plasma turbulence from solar wind observations
TL;DR: In this paper, the authors summarise some of the recent progress that has been made in understanding astrophysical plasma turbulence in the solar wind, from in situ spacecraft observations, along with comparison to recent models of strong Alfvenic turbulence.
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