g i§ C x @4 &® \ O C . 2 EE .!\/ ’X' : ’·’ heliosphere will be presented. collisionless shocks in the solar system. Some specific space projects exploring the fields; the diversities of charged particle acceleration, in particular the role of planetary magnetospheres by interactions between the solar wind and planetary magnetic large scale structures of the interplanetary medium to climatic changes; formation of sun in farming the heliosphere; manifestations of solar activity and the solar cycle, from magnetospheres, and energetic particles in the solar system. This includes the role of the The main topics will deal with the sun, the interplanetary plasma, planetary The lecture series will start with some fundamental principles of cosmic plasma physics. ABSTRACT ure 3 :15May Energetic particles into the heliosphere ture 2 2 14 May Planetary magnetospheres ture 1 : 13 May The Sun and the iriterplanetary medium ze! 9 Awe/· T?¤·M PLACE Auditorium E ·iV `xrw May 13, 14, 15 from 11.00 t012.00 hrs :T las.? TITLE Plasma physics in the solar system SPEAKER G. WIBBERENZ / Kiel University :4%/V/A ' 1990 — 1991 ACADEMIC TRAINING PROGRAMME W % W 0% 7 / i / A A100000301 , / %% FIGS Z // UT S UT _V / / r ,; 1 Y w gg · L1BRAR1ES, GENEVA / `X , / 4 7/ 7 ’ / 6 ~ } [ _(§ / / %4 " "`\`` ``* ``` »// >\;\¤; *s¤<:s>>»>` szvk x ~i>~\i ;\ ;~§s\ *<r: \: ~:;$>;:;:><rie<:;»\ :; *>; *:;i*¤;; :s;** $;»¤;:iis* ixw * > \@i€w2<»§;>\:*; ¤ \¤;~—;¤\¤\ xv `iiwN?\»»®2¤.t~<:i`<>¤=\ ’ wxsw~~> =s·~\i<ss \;<>¤>\¤*x;v; >ss>i \i <; ¤~~w \x\x_x=g> \;~< x \ x xssx ~\\w~ ;»\_¤x\¤~~
39
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TITLE :T las.? - CERN · The solar wind. Individual features (sunspots, filaments, arches, complex). The structure of the solar corona (unipolar, bipolar, Sun. • The solar cycle
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/ OCR Output
g i§ C x @4&® \
O C.2 EE
.!\/’X' : ’·’
heliosphere will be presented.collisionless shocks in the solar system. Some specific space projects exploring thefields; the diversities of charged particle acceleration, in particular the role ofplanetary magnetospheres by interactions between the solar wind and planetary magneticlarge scale structures of the interplanetary medium to climatic changes; formation ofsun in farming the heliosphere; manifestations of solar activity and the solar cycle, frommagnetospheres, and energetic particles in the solar system. This includes the role of theThe main topics will deal with the sun, the interplanetary plasma, planetaryThe lecture series will start with some fundamental principles of cosmic plasma physics.
ABSTRACT
ure 3 :15May Energetic particles into the heliosphereture 2 2 14 May Planetary magnetospheresture 1 : 13 May The Sun and the iriterplanetary medium ze! 9
Awe/· T?¤·M
PLACE Auditorium
E ·iV `xrwMay 13, 14, 15 from 11.00 t012.00 hrs :T las.?TITLE Plasma physics in the solar system
¤ \¤;~—;¤\¤\ xv `iiwN?\»»®2¤.t~<:i`<>¤=\ ’ wxsw~~> =s·~\i<ss \;<>¤>\¤*x;v; >ss>i \i <; ¤~~w \x\x_x=g> \;~< x \ x xssx ~\\w~ ;»\_¤x\¤~~
HELIOS and ULYSSES. OCR Outputof the University of Kiel to the International Sun Earth Explorer (ISEE) and the space probesspecific space projects exploring the heliosphere will be presented, in particular contributionsparticle acceleration, in particular the role of collisionless shocks in the solar system. Someinteractions between the solar wind and planetary magnetic fields; the diversities of chargedof the interplanetary medium to climatic changes; formation of planetary magnetospheres byheliosphere; manifestations of solar activity and the solar cycle, from large scale structuresenergetic particles in the solar system. This includes the role of the Sun in forming themain topics deal with the Sun, the interplanetary plasma, planetary magnetospheres, andThe lecture series starts with some fundamental principles of cosmic plasma physics. The
loops to open field lines! OCR OutputOrigin of slow solar wind: transition from closed
the corona.
Related to general question of the heating of
coronal holes (supply of sufficient energy).Realistic model for high speed streams from
OCR OutputSOLAR WIND: SOME OPENOPROBLEMS
T0p010gica.1 structure 0f the Ea,rth’s magnetosphere OCR Output
PARTICLE ENTRY!
AND CLOSED FIELD LINES
REGION BETWEEN OPEN
AURORAL OVAL:
CAPSPOLAR
TMLM ·PAUSE
L 4L>\’<\`\ \L
,._\\I , \ ~. . ..
:· Z · ` 1) I.
'`°··‘ ;?·I;='
CUSP
INDTRAPPED RADIATION
SOLAR
/ BOW SHOCK
closed form available.) OCR Output(Well developed theory, results inmagnetic field.large- and small-scale structures of theParticles are used as probes for the
Wave-particle interactions, generation of turbulence and
A variety of effetcs leads to particle acceleration.
The thermal plasma has a tail of suprathermal particles.
electric fields.
Space charges (double layers) and magnetic field aligned
ACTIVE PLASMA:
27 —OCR Output
reconnection
(Fermi-effect)moving magnetic fieldsdo/dt ~ {Eds b)(Betatron)temporal changes2. 6B/at qé 0
(: turbulence with 6E B, "stochastic" HF!)q Q
—I— electrostatic vvaves1. Space charges
How de we get electric fields?
z PARTICLE ACCELERATION 75 O)
netic fields)(Notably near bcundaries and in complex mag
ELECTRIC FIELDS IN "AC'I`IVE" PLASMA
= hypothetical
MHD-turbulence) I (anomalous comp.)?(self-generated I termination shockat shocks solar Hares? 10 GeV?) OCR OutputFermi-effect 500 KeV)interplanetary shocks I (Qnon-linear 50 KeV)Earth’s bow shock I (3Fermi—effect) acceleration?(2nd order interplanetary turbulence
acceleration (second phase?); I sumcientstochastic solar Hares fast for
PLASMAS I fixed energyACTIVE I double layers aurora] particles I peak at
substorms
tail bursts magneticmagnetic energy) I magnetospheric —-> I origin of(release of (first phase);
fast reconnection I solar Hares
cosmic rays:
MHD low energy solar hypotheticalE.L Bi i
slow reconnection I solar corona?energy gainshocks
gyration, focusing/ mirroring, and driftCharged particle propagation in smooth magnetic fields:
KN Q<O
Driftrichtungu GO 0 QO C)
»·"I"·
,·'I"`*
.·"I"—
/"
iw
I953 to I988 OCR Output
CLIMAX AVERAGE COSMIC RAY INTENSITY
3000
3500
Flv/U,
4000
fl“llf`“ll * iW"
4500CYCLE 2lCYCLE 20CYCLE I9
54 58 62 |66 70 74 I 78 82 86I 90
80
120
160
200
240 MONTHLY MEAN SUNSPOT NUMBERS
cosmic my intensity with the solar cycle (below)Variation of Sunspot numberl(above) and
L_(/\9W LS SEN )'A1lSN31Nl OCR Output [DV]T"v—v·—•*1'•'—
GOOOOOOQ.
LDCNLO Ln ·¢ 0O_ N
G
- 3 5 OCR OutputImprlmé au CERN. Prlx : 1.90 Fr.
bers 2-3, 1984.
Waves, Nucleosynthesis and Cosmic Rays, Adv. Space Res. Vol. 4, Num12. L. Koch-Miramond and M.A. Lee, Particle Acceleration Processes, Shock
can Geophysical Union, VVashington, D.C., 1985.sphere: Reviews of Current Research, Geophysical Monograph 35, Ameri·
·*·· 11. B.T. Tsurutani and R.G. Stone (Eds.), Collisionless Shocks in the Helio
Cambridge University Press, London 1972.
10. J.A. Ratcliffe, An Introduction into the Ionosphere and Magnetosphere,
Verlag, Berlin 1970.
J.G. Roederer, Dynamics of Geomagnetically Trapped Radiation, Springer
1 and 2, Springer—Verlag, Vol. 1 (1990), Vol. 2 (in press).R. Schwenn and E. Marsch (Eds.), Physics of the Inner Heliosphere, Vol.
Berlin 1972.
A.J. Hundhausen, Coronal Expansion and Solar Wind, Springer-Verlag,
bridge University Press, 1988.E. Tandberg-Hanssen and A.G. Emslie, The Physics of Solar Flares, Cam
M. Stix, The Sun, Springer-Verlag, Berlin 1989.
Physics, Vol. l—llI, North-Holland Publ. Company, Amsterdam 1979.E.N. Parker, C.F. Kennel, and L.J. Lanzerotti (Eds.), Solar System Plasma
H. Alfvén, Cosmic Plasma, D. Reidel, Dordrecht 1981.
London 1969.
T.J. M. Boyd and J.J. Sanderson, Plasma Dynamics, Nelson and Sons Ltd.,
Oxford 1963.
H. Alfvén, C.G. Falthammar, Cosmical Electrodynamic, Clarendon Press,
ers to enter into some of the fundamental principles and some recent developments.)(The following list of references is far from representative. It will allow interested read