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Istituto di Astrofisica Spaziale e Fisica Cosmica

Istituto di Fisica dello Spazio Interplanetario. Istituto di Astrofisica Spaziale e Fisica Cosmica. SFSI Fisica del Plasma nel Sistema Solare

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Istituto di Astrofisica Spaziale e Fisica Cosmica

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  1. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica SFSI Fisica del Plasma nel Sistema Solare I plasmi astrofisici nel laboratorio naturale del Sistema Solare; l’unico vento stellare che possiamo osservare direttamente in situ, e dettagliatamente nei suoi effetti sui pianeti Corona solare • Sole-Vento solare-Eliosfera Relazioni Sole-Altri Pianeti • L’interazione Sole-Altri Pianeti Relazioni Sole-Terra • L’interazione Sole-Terra • L’interazione Magnetosfera-Ionosfera Relatore: M. Candidi Roma, 15-16 dicembre 2003

  2. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Sun and solar atmosphere NASA TRACE The Sun is the driver Coronal loop; the picture shows the features of the Sun’s magnetic fields The magnetic field may convert energy through reconnection of adjacent loops Energisation of the plasma may result through several mechanisms of transport to higher altitudes ESA SOHO Relatore: M. Candidi Roma, 15-16 dicembre 2003

  3. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Cosmic rays in the heliosphere • Heliosphere: the region of space where the solar wind dominates over the interstellar gas • Cosmic Rays are modulated by the geometry of this region and their detection is affected (at Earth or in the space around Earth) Relatore: M. Candidi Roma, 15-16 dicembre 2003

  4. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Solar wind The solar wind transfers mass, momentum and energy to the Earth system. It may be observed al L1 by monitoring spacecraft, tens of minutes before it reaches the magnetosphere boundary The parameters of the incoming solar wind determine the strenght of coupling with the magnetosphere (mainly Bz, and nv, the plasma dynamic pressure). When Bz is south, coupling between the solar wind and the magnetosphere is favoured. Mag field (B,Bz) Azimuth Density (n) Velocity (v) Temperature NASA ACE Relatore: M. Candidi Roma, 15-16 dicembre 2003

  5. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Magnetosphere The magnetosphere responds to the inputs Electric current systems develop : Tail Field aligned Polar Ionospheric Ring Chapman-Ferraro These change in time, driven by the varying solar wind input Relatore: M. Candidi Roma, 15-16 dicembre 2003 Roma, 5-6 novembre 2003

  6. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Ionosphere Effects in the human environment follow Theta aurora over Antarctica Auroras form on magnetised planets with an atmosphere in a stellar wind Relatore: M. Candidi Roma, 15-16 dicembre 2003

  7. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica SPACE WEATHER …to observe, study and forecast the effects of solar phenomena which…. ..may endanger life in space and performance of space and terrestrial systems… ..NASA “Living with a star”and the “space weather” initiative of ESA. … is a part of solar terrestrial and space physics. Intense flux of high energy electrons damages commercial satellites at synchronous orbit Strong magnetic field variations couple inductively to long power lines and generate intense electric currents. Damage to system determines black-outs Relatore: M. Candidi Roma, 15-16 dicembre 2003

  8. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica From “The Sun to the Earth-and beyond” a Decadal Research Strategy in Solar and Space Physics” (US National Research Council, 2003) • Important answers have been given through the accomplishments of the last decades about “the physics of the Sun, the interplanetary medium and the space environments of the Earth and other solar system bodies”. • Five challenges remain to be answered for the next dacade (2003-2013), due to lack of observations in key regions and limited capabilities and infrastructures. • The structure and dynamics of the Sun interior (generation of mag. fields, origin of solar cycle, causes of solar activity, structure and dynamics of corona) • Heliospheric structure (distribution of mag. fields and matter, interaction of solar atmosphere with local interstellar medium) • Space environment of Earth and other solar system bodies and dynamical response to external influences. • Basic physical principles in processes observed in solar and space plasmas. • Develop near-real-time predictive capability for understanding and quantifying impact on human activities (space weather). Relatore: M. Candidi Roma, 15-16 dicembre 2003

  9. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Solar Terrestrial Plasma Physics at IFSI • Solar wind processes such as energy transport and plasma waves • Cosmic Rays interaction with heliospheric structures • MHD turbulence and coherent structures in the Solar Wind • Study of magnetopause microprocesses such as plasma transport and reconnection • Cusp and high latitude boundaries of the magnetosphere • Polar ionosphere phenomena such as plasma convection and field aligned currents • Space weather • Cosmic rays interactions with neutral atmosphere • Electrodynamic interactions for conductive tethers in orbit Relatore: M. Candidi Roma, 15-16 dicembre 2003

  10. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Ruoli nei Progetti Europei ed Internazionali di Space Weather ESA Space Weather Working Team OA Turin OA Trieste ESA Space Weather Pilot Projects Uni Turin IROE/CNR Florence Programmi approvati : E. Amata GIFINT Iniziative Europee di Space Weather Uni L’Aquila Uni Rome OA Rome IFSI/CNR Rome INGV Rome ESF COST Action 724 on Space Weather OA Naples Rappresentante nazionale : M. Candidi Uni Naples EU-Solar Terrestrial and Atmospheric Res. E-STAR OA Catania Proponente : E. Amata Uni Catania Iniziativa Nazionale di Space Weather EU Research and Training Network Responsabile : G. Consolini Relatore: M. Candidi Roma, 15-16 dicembre 2003

  11. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica ILWS NASA/ESA/RASA/JAEA/CSA WG’s Solar Terrestrial Physics and Space Weather: International Committes ESA Space Weather pilot projects (16) Ionosphere Thermosphere Ground Based Obs. Magnetosphere GIFINT IFSI/INGV/RAL/Obs.Athens E. Amata Others Others SCOSTEP (ICSU) WG’s Bureau member M. Candidi EU COST Action 724 WG’s National rep. Solar Influenceon Climate Space Climatology Space Weather Atmospheric Coupling Space Weather Observations and Services M. Candidi Solar Wind Disturbances at Earth Solar Activity M. Messerotti Radiation Environment Relatore: M. Candidi Roma, 15-16 dicembre 2003

  12. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica What are we doing about it? • Space missions: • Ulysses • Cluster • Double Star • Ground based instruments • All-sky cameras • SuperDARN radars • Cosmic ray detectors • Theory Tutti saranno descritti nelle seguenti presentazioni, salvo alcuni aspetti che darò subito, per alcune cose che non saranno dettagliate dopo Relatore: M. Candidi Roma, 15-16 dicembre 2003

  13. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Cosmic rays in the heliosphere • Prompt data for Space Weather • Revised data for Space Climatology • Data files in the international formats for the World-Wide Network of detectors • High-speed solar wind streams identification • Cosmic ray induced effects in the terrestrial environment (air mass, atmospheric temperature, electric fields, geomagnetic and latitude dependences, north-south differences, secular variations, jerks, geomagnetic anomalies, …) • Study of solar and galactic cosmic rays and their relation with modulation phenomena (short-, medium- and long-term basis) Ulteriori dettagli nella presentazione della stazione SVIRCO e delle stazioni LARC, ESO, OLC Relatore: M. Candidi Roma, 15-16 dicembre 2003

  14. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica IFSI all-sky cameras: Arctic and Antarctic Baia Terra Nova, March 22nd, 2001, 13:40 GUT (=428nm) Ny Alesund Zackenberg Northern hemisphere polar sites equipped with all-sky cameras by IFSI/CNR (NyAlesund, Svalbard; Zackenberg, Greenland). Longitudinal array, MIRACLE Italian antarctic instrumentation sites: Baia Terra Nova Dome-C Relatore: M. Candidi Roma, 15-16 dicembre 2003

  15. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Active experiments Operational criterion for long term tether stability Tether should operate for 3 months with angular oscillations, both in plane and out of plane not overtaking 20 degrees I0 < 0.94 amperes Bare tether : in plane oscillations STAIF 2002 Albuquerque NM February 3-7 2002 Relatore: M. Candidi Roma, 5-6 novembre 2003

  16. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Solar wind andMagnetosphere CLUSTER Double Star Relatore: M. Candidi Roma, 15-16 dicembre 2003

  17. Istituto di Fisica dello Spazio Interplanetario Istituto di Astrofisica Spaziale e Fisica Cosmica Remote sensing of the motion of ionospheric irregularities; Doppler shift of radar signal with pairs of crossed ground based radars. SuperDARN radars Relatore: M. Candidi Roma, 5-6 novembre 2003

  18. Figure 3. Maps of the Super Dual Auroral Radar Network (SuperDARN) arrays over the northern (left) and southern (right) polar regions. The Antarctic map shows 6 existing (yellow) and 5 planned (light brown) radars that will provide complete coverage of the southern polar region above 60 corrected geomagnetic latitude.

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