Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario Roma, 15-16 dicembre 2003 Relatore: M. Candidi SFSI Fisica

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


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



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)




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, 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




Theta aurora over Antarctica

Auroras form on magnetised planets with an atmosphere in a stellar wind

Effects in the human environment follow

Ionosphere




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

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).



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


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


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



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




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



•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


Ulteriori dettagli nella presentazione della stazione SVIRCO e delle stazioni LARC, ESO, OLC



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


Ny Alesund

Zackenberg



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



Solar wind andMagnetosphere

Double StarDouble Star

CLUSTERCLUSTER




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.

Documents

Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario Roma, 15-16 dicembre 2003 Relatore: M. Candidi SFSI Fisica