Scientific research related to circumterrestrial and planetary Space Weather in the context of past, current and future space missions with Italian payload contribution.
|Mission||Instrument||Participating Research Institutes in Italy||Observation technique||Type of data||Period covered by the data||Key science goals related to Space Weather|
|ESA/JAXA||SERENA (Italian PI-ship)||INAF-IAPS et al.||In situ neutral and ionized particle detection||Images and particle flux||October 2018–2026 (nominal mission)||Characterization of the solar wind-driven Space Weather at Mercury|
|ESA||CIS||INAF-IAPS et al.||In situ proton-alpha and heavy ions detection with Top-Hat electrostatic analyser||Ions 3D distributions||2001–present (extended to 31st December 2022; subject to a mid-term review in 2020)||3-D characterization of plasma structures|
|CNSA||LIMADOU/HEPD||INFN; UNITOV; UNITN et al.||Particle detection||Single particle/particle flux||February 2018–present||Measurement of the increase of the electron and proton fluxes due to short-time perturbations of the radiation belts|
|CNSA||LIMADOU/EFD||INFN; UNITOV; INAF-IAPS et al.||Electric field detection||Waveform (1 Hz–2 kHz)/Spectrum (1 kHz–5 MHz)||February 2018–present||Measurement of the variation of the ionosphere electric field due to perturbations driven by the solar activity|
|ESA-CNSA||HIA||INAF-IAPS et al.||In situ ions detection with Top-Hat electrostatic analyser||Ions 3D distributions||2003–2008||The data provided by the two Double Star s/c integrated the CLUSTER data, to provide unprecedented multi-point measurements of the near-Earth space.|
|NASA (Rocket Program)||SCORE (Italian PI-ship)||INAF-OATo; UNIFI; UNIPD et al.||VL, UV & EUV coronal imaging||VL, UV (H Ly α) & EUV (He II Ly α) Images||2009 flight||First measurement of the helium abundance and outflow velocity in the solar corona;|
|Herschel||Mapping of the solar wind outflows;|
|Identification of the physical properties of the outer solar corona|
|ISS||ALTEA||UNITOV et al.||Particle detection||Particle flux LET||August 2006–Novomber 2012, not continuous||Radiation environment measurements in the ISS|
|ISS||AMS-2||INFN; UNIBO; UNIMI Bicocca; UNIPG; UNIRoma1; UNIPI; UNITN||Particle detection||Particle flux for nuclear species, electron, positrons, anti-protons||May 2011–present (≥2024)||Measurements of cosmic ray flux and composition in the GeV–TeV energy range;|
|Time profile of the energy spectrum and flux intensity for proton and alpha particles, electrons and positrons, heavier nuclei (C, O, …);|
|Measurements of SEPs.|
|NASA||JIRAM (Italian leadership)||INAF-IAPS; CNR-ISAC Rome; CNR-ISAC Bologna||Image IR spectrometry||Images and Spectra||2016–2021 (foreseen)||Investigation of the H3 + aurora at Jupiter|
|ESA||ASPIICS||INAF-OATo et al.||Multi-band VL coronol imaging||Launch foreseen in 2021||Characterization of the solar wind in the inner corona, prominence formation, prominence eruption and CME early evolution|
|ESA/NASA||UVCS (Italian CoPI-ship)||UNIFI; UNITO; UNIPD; INAF-OATo; INAF-Arcetri; INAF-OACt; et al.||UV Spectroscopy||Spectra (945–1123 Å, 473–561 Å, 1160–1350 Å)||1996–2012 24 h/day observations||Identification of the solar wind sources;|
|SOHO||Images (reconstructed from spectral data)||Diagnostics of the solar wind heating and acceleration processes;|
|Investigation of CME evolution in the outer corona and of CME shock front and energetic particle acceleration|
|ESA||METIS (Italian PI-ship)||INAF-OATo; UNIFI; UNIPD; INAF-OACt; INAF-OAC et al.||VL and UV coronagraph imaging||VL, UV (H Ly α) Images||Launch foreseen in 2020||Identification of the solar wind sources;|
|Solar Orbiter||Characterization of large scale solar wind properties;|
|Investigation of the origin, evolution and propagation of CMEs|
|ESA||SWA (Italian CoPI-ship)||INAF-IAPS et al.||In situ electron, proton-alpha and heavy ion detection by Top-Hat electrostatic analyser with deflectors||Ions 3D distributions||Launch foreseen in 2020||Investigation of solar wind fundamental processes (e.g., acceleration, heating and ICME evolution) and their connection to the Sun’s corona|
|Roscosmos||PAMELA (Italian leadership)||INFN, UNITOV et al.||Particle detection||Particle flux||June 2006–January 2016||Measurements of SEPs in space;|
|Resurs-DK1||Reconstruction of proton and helium energy spectra and time profiles|
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