ILWS 12 June 2007ILWS 12 June 2007ASI ProgramASI Program

Ester AntonucciEster Antonucci

Participation In Flight MissionsParticipation In Flight Missions

•SOHO (UVCS)SOHO (UVCS)•Ulysses Ulysses •CLUSTERCLUSTER•DOUBLE STARDOUBLE STAR

Participation In Data AnalysisParticipation In Data Analysis•TRACETRACE•HINODEHINODE•(STEREO)(STEREO)

Solar System Exploration: Sun (Heliophysics)Solar System Exploration: Sun (Heliophysics)Kickoff 1 June 2007Kickoff 1 June 2007

•Magneto-hydrodynamic modellingMagneto-hydrodynamic modellingDiagnostic tools aimed to address the solar and heliospheric physics issues:• MHD codes to interpret the coronal and heliospheric plasma processes.•Spectroscopic diagnostic codes for interpreting the UV, EUV ed X emission from optically thin plasmas (non-equilibrium ionization etc.). •Turbulence in the solar wind plasma.

•Space Weather Space Weather •Origin of solar perturbations (space data + radio, visible, cosmic rays, magnetic field)•SEP effects

•Magnetospheric network data analysis.•Prototypes developmentPrototypes development•Multiwavelength coronagraphy for the extended corona (Solar Orbiter)(Solar Orbiter)•UV, XUV spectrometry for the inner corona observation (Solar Orbiter)(Solar Orbiter)•UV polarimetry for coronal magnetic field observations (SMESE,COMPASS) (SMESE,COMPASS) •Plasma analyzer (Solar Orbiter)(Solar Orbiter)•Energetic particle analyzer (Solar Orbiter)(Solar Orbiter)

Coronal magnetic fieldCoronal magnetic field

Coronal images give qualitative information about the field topology.

Extrapolation Techniques: potential field: extrapolation to the corona of photospheric magnetic field in the hp: no electric currents. force-free field: hp: electric currents can flow only along magnetic field lines so to exert no magnetic force on the coronal plasma.

Observational UV spectropolarimetry. Hanle effect: resonance polarization in spectral lines is deeply modified by the presence of a magnetic field (UV Lyman alpha series, OVI 1032, allowed coronal lines which are radiatively excited by the radiation coming from the solar disk) (Cosmic Vision 15-25)(Cosmic Vision 15-25)

Solar System Exploration: Sun (Heliosphysics) Solar System Exploration: Sun (Heliosphysics) contcont

•Laboratory developmentsLaboratory developments•Optics for coronal spectro-imaging in the UV/Visibile •Multilayer coating in the EUV •Wide angle coronagraphs formed by nanosatellites •Facility for coronagraphic instrumentation calibration •Upgrade of facility for testing plasma analyzers.

•Observations and analysisObservations and analysis•Instrumentation operating in space

•Future MissionsFuture Missions•High energy particles (LISA)•Coronal magnetic field measurements (COMPASS) •Magnetospheric missions

Helium Resonance Scatter in the Corona Helium Resonance Scatter in the Corona

and Heliosphere Program:and Heliosphere Program: SCORE SCORE NASA LWS ProgramNASA LWS Program

• SCORE (Sounding Coronagraphic Experiment) in the frame of the NASA ‘Living with a Star’ program

• Launch October 2007

Firsts• Helium measurement in the solar corona• Test of multiwavelength coronagraphy in

view of the SolarOrbiter (visible, H, He)

Missione SOLAR Missione SOLAR ORBITERORBITER

• Solar Orbiter first circumsolar mission of the ‘International Living with a Star’ program.

• Solar Orbiter last mission of the ‘Cosmic Vision’ ESA program.

Possible italian contributions to Solar OrbiterPossible italian contributions to Solar Orbiter Letters of Intent 15 Sep 2006Letters of Intent 15 Sep 2006

• CIAO CIAO (Coronal Imaging (Coronal Imaging Advanced Observations)Advanced Observations)

• EUS EUS (Extreme Ultraviolet (Extreme Ultraviolet Spectrometer)Spectrometer)

• DPDDPD (Dust Particle Detector) (Dust Particle Detector)

• NPDNPD (Neutral Particle Detector) (Neutral Particle Detector) • SWA SWA (Solar Wind Plasma (Solar Wind Plasma

Analyzer)Analyzer)

• HETHET (High Energy Telescope)(High Energy Telescope)

Interests in other missionsInterests in other missions

• ASPICS ASPICS CoronagraphyCoronagraphy

• SMESESMESE Coronal magnetic field system Coronal magnetic field system

• KUAFU AKUAFU A UV-visible light coronagraphyUV-visible light coronagraphy

• Solar Probe Solar Probe Heliospheric imagingHeliospheric imaging

‘‘Cosmic Vision 2015-2025’ proposalsCosmic Vision 2015-2025’ proposals

• Compass Compass (leading role)(leading role)• Magnetic field measurements in corona and on the disk: UV Visible Magnetic field measurements in corona and on the disk: UV Visible

spectro polarimetryspectro polarimetry• Spacecrafts in flight formationSpacecrafts in flight formation

• Polaris Polaris (participation)(participation)

COMPASS Formation Flying SpacecraftsCOMPASS Formation Flying Spacecrafts

Payload Spacecraft (P/L-S/C)Payload Spacecraft (P/L-S/C)

““Sunshade” Spacecraft (S-S/C)Sunshade” Spacecraft (S-S/C)

100 m100 m

x

yz

PayloadPayload

The The COMPASSCOMPASS payload will consist of remote sensing instruments with off- payload will consist of remote sensing instruments with off-limb and on-disk fields-of-view (FOV).limb and on-disk fields-of-view (FOV).

- Off-limb FOV:- Off-limb FOV:

• UV coronal spectro-polarimeter (90-120 nm) UV coronal spectro-polarimeter (90-120 nm)

• Visible & IR coronal spectro-polarimeter (0.5-1 Visible & IR coronal spectro-polarimeter (0.5-1 m)m)

- On-Disk FOV:- On-Disk FOV:

• UV spectro-polarimeter (100-200 nm) UV spectro-polarimeter (100-200 nm)

• EUV imaging-polarimeter (17 nm) EUV imaging-polarimeter (17 nm)

• Dopplergraph-magnetograph imager Dopplergraph-magnetograph imager

COMPASS & POLARISCOMPASS & POLARIS

DATA ARCHIVESDATA ARCHIVES

• SOLAR (SOHO archive)SOLAR (SOHO archive)

• SOLARNET (italian solar archives network)SOLARNET (italian solar archives network)

• EGSO (SEC,EGSO (SEC, DSO)DSO)