Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 15-16 dicembre 2003Relatore: M. Candidi
SFSIFisica 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
Relazioni Sole-Altri Pianeti• L’interazione Sole-Altri Pianeti
• L’interazione Sole-Terra
• L’interazione Magnetosfera-Ionosfera
Relazioni Sole-Terra
• Sole-Vento solare-EliosferaCorona solare
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
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
NASA TRACE
ESA SOHO
The Sun is the driver
Sun and solar atmosphere
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
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)
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
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
Mag field (B,Bz)
Azimuth
Density (n)
Velocity (v)
Temperature
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.
NASA ACE
Solar wind
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: M. Candidi
The magnetosphere responds to the inputs
Magnetosphere
Electric current systems develop :
Tail
Field aligned
Polar Ionospheric
Ring
Chapman-Ferraro
These change in time, driven by the varying solar wind input
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
Theta aurora over Antarctica
Auroras form on magnetised planets with an atmosphere in a stellar wind
Effects in the human environment follow
Ionosphere
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
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
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi Roma, 15-16 dicembre 2003
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.
(1) 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)
(2) Heliospheric structure (distribution of mag. fields and matter, interaction of solar atmosphere with local interstellar medium)
(3) Space environment of Earth and other solar system bodies and dynamical response to external influences.
(4) Basic physical principles in processes observed in solar and space plasmas.
(5) Develop near-real-time predictive capability for understanding and quantifying impact on human activities (space weather).
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
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
Roma, 15-16 dicembre 2003
Ruoli nei Progetti Europei ed Internazionali di Space Weather
OA TurinOA TurinOA TurinOA TurinOA TriesteOA TriesteOA TriesteOA Trieste
IROE/CNR FlorenceIROE/CNR FlorenceIROE/CNR FlorenceIROE/CNR Florence
Uni L’AquilaUni L’AquilaUni L’AquilaUni L’Aquila
IFSI/CNR RomeIFSI/CNR RomeIFSI/CNR RomeIFSI/CNR Rome
INGV RomeINGV RomeINGV RomeINGV Rome
OA RomeOA RomeOA RomeOA Rome
OA NaplesOA NaplesOA NaplesOA Naples
OA CataniaOA CataniaOA CataniaOA Catania
Uni RomeUni RomeUni RomeUni Rome
Uni TurinUni TurinUni TurinUni Turin
Uni NaplesUni NaplesUni NaplesUni Naples
Uni CataniaUni CataniaUni CataniaUni Catania
ESA Space Weather Working TeamESA Space Weather Working TeamESA Space Weather Working TeamESA Space Weather Working Team
ESA Space Weather Pilot ProjectsESA Space Weather Pilot ProjectsESA Space Weather Pilot ProjectsESA Space Weather Pilot Projects
EU-Solar Terrestrial and Atmospheric Res.EU-Solar Terrestrial and Atmospheric Res.E-STARE-STAR
EU-Solar Terrestrial and Atmospheric Res.EU-Solar Terrestrial and Atmospheric Res.E-STARE-STAR
ESF COST Action 724 on Space WeatherESF COST Action 724 on Space WeatherESF COST Action 724 on Space WeatherESF COST Action 724 on Space Weather
Iniziativa Nazionaledi Space Weather
Iniziative Europeedi Space Weather
Rappresentante nazionale : M. CandidiRappresentante nazionale : M. CandidiRappresentante nazionale : M. CandidiRappresentante nazionale : M. Candidi
Proponente : E. AmataProponente : E. Amata Proponente : E. AmataProponente : E. Amata
Programmi approvati : E. Amata Programmi approvati : E. Amata GIFINTGIFINT Programmi approvati : E. Amata Programmi approvati : E. Amata GIFINTGIFINT
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi Roma, 15-16 dicembre 2003
EU Research and Training NetworkEU Research and Training NetworkEU Research and Training NetworkEU Research and Training Network
Responsabile : G. ConsoliniResponsabile : G. Consolini Responsabile : G. ConsoliniResponsabile : G. Consolini
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
ESASpace Weather pilot
projects (16)
GIFINTIFSI/INGV/RAL/Obs.Athens
E. Amata
Others
ILWSNASA/ESA/RASA/JAEA/CSA
WG’s
IonosphereThermosphere
Ground Based Obs.
Magnetosphere
EU COST Action 724 WG’sNational rep.
SCOSTEP (ICSU) WG’sBureau member
M. Candidi
Solar Activity
M. Messerotti
Radiation Environment
Solar Wind Disturbances
at Earth
Space Weather Observations and ServicesM. Candidi
Solar Influence
on Climate
Space Weather
AtmosphericCoupling
Space Climatology
Others
Solar Terrestrial Physics and Space Weather: International Committes
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
What are we doing about it?
Space missions: Ulysses Cluster
Double Star
Ground based instruments All-sky cameras
SuperDARN radars Cosmic ray detectors
Theory
Roma, 15-16 dicembre 2003
Tutti saranno descritti nelle seguenti presentazioni, salvo alcuni aspetti che darò subito, per alcune cose che non saranno dettagliate dopo
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
•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)
Cosmic rays in the heliosphere
Roma, 15-16 dicembre 2003
Ulteriori dettagli nella presentazione della stazione SVIRCO e delle stazioni LARC, ESO, OLC
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
Baia Terra Nova, March 22nd, 2001, 13:40 GUT (=428nm)
Northern hemisphere polar sites equipped with all-sky cameras by IFSI/CNR (NyAlesund, Svalbard; Zackenberg, Greenland). Longitudinal array, MIRACLE
IFSI all-sky cameras: Arctic and Antarctic
Italian antarctic instrumentation sites: Baia Terra Nova Dome-C
Roma, 15-16 dicembre 2003
Ny Alesund
Zackenberg
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: M. Candidi
Operational criterion for long term tether stability
STAIF 2002 Albuquerque NM February 3-7 2002
Tether should operate for 3 months with angular oscillations, both in plane and out of plane not overtaking 20 degrees
0 5 10 15 20 25 30-8
-4
0
4
8
12 i
n in
30 35 40 45 50 55 60
-12-8-4048
1216
60 65 70 75 80 85 90
-20
-10
0
10
20
30
in
time (days)time (days)time (days)
Bare tether : in plane oscillations
I0 < 0.94 amperes
Active experiments
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Relatore: M. Candidi
Solar wind andMagnetosphere
Double StarDouble Star
CLUSTERCLUSTER
Roma, 15-16 dicembre 2003
Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario
Roma, 5-6 novembre 2003Relatore: M. Candidi
SuperDARN radars
Remote sensing of the motion of ionospheric irregularities; Doppler shift of radar signal with pairs of crossed ground based radars.
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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