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Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Helmut O. Rucker
Exploring the Planets and Moons in our Solar System
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Exploring the Planets and Moons in our Solar System
• The interplanetary medium, the solar wind and its interaction with magnetized planets
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Exploring the Planets and Moons in our Solar System
• The interplanetary medium, the solar wind and its interaction with magnetized planets
• Space missions to the outer planets
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Exploring the Planets and Moons in our Solar System
• The interplanetary medium, the solar wind and its interaction with magnetized planets
• Space missions to the outer planets
• Specific aspects of magnetospheric physics – radio emission
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Exploring the Planets and Moons in our Solar System
• The interplanetary medium, the solar wind and its interaction with magnetized planets
• Space missions to the outer planets
• Specific aspects of magnetospheric physics – radio emission
• Volcanoes and icy worlds
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Exploring the Planets and Moons in our Solar System
• The interplanetary medium, the solar wind and its interaction with magnetized planets
• Space missions to the outer planets
• Specific aspects of magnetospheric physics – radio emission
• Volcanoes and icy worlds
• Space Missions to the terrestrial planets
Space Research Institute GrazAustrian Academy of Sciences
„
CERN, Geneve, June 2006
Helmut O. Rucker
The interplanetary medium,the solar wind and its interaction with
magnetized planets
The central star of our solar system – the Sun
Mass loss by theexpanding solar atmosphere, i.e. the solar wind:~ 10 E6 tons per second
Viewgraph: Helmet streamer
The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)
swv
The interplanetary magnetic field is a solar magnetic fielddrawn out of the Sunby the highly conducting solar wind plasma.Due to the solar rotationa spiral structure is formed.
IMFB
The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)
sw
sun
v
rtan
Parker spiral:
7.83)5.9(
6.43)0.1(
450
1086.2
)400,8638.25/(2
1
16
AUr
AUr
kmsv
s
s
sw
sun
sun
Solar wind average properties at r ~ 1 AU:
Different types of solar wind (sw):
Fast sw: 400 < v < 800 km/s, Helium 3 – 4 %Slow sw of minimum type: 250 < v < 400 km/s, Helium < 2 %Slow sw of maximum type: 250 < v < 400 km/s, Helium ~ 4 %Coronal mass ejections (CMEs): 400 < v < 2000 km/s, Helium(++) ~ 30 %
Solar wind average properties at r ~ 1 AU:
Dipole structure
20 sinrr
DM
2
1
)(
nm
TTnk
c
cv ie
V
psonic
Interaction between the solar wind and planetary magnetic field
Solar wind bulk flow = super-sonic flow
= super-Alfvenic flow0
BvA
Bow shock:
Transition of solar wind plasmadescribed by theRankine Hugoniot equations
bulk speedparticle densityPlasma pressureplasma temperature
Interaction between the solar wind and planetary magnetic field
3D schematics of the terrestrial magnetosphere
magnetopauseboundary conditions:
0
2/cos 0222
nB
Bnmv
Magnetic reconnection
Magnetic reconnection
Magnetic reconnection
Courtesy Prange, 2006
Courtesy Prange, 2006
1st reconnection = start of the cycle
Courtesy Prange, 2006
Courtesy Prange, 2006
Courtesy Prange, 2006
transportover the poles
Courtesy Prange, 2006
Courtesy Prange, 2006
2nd reconnection
Courtesy Prange, 2006
impulsiveacceleration
Release of energy( the stretched configurationcontains additionalenergy to accelerateplasma)
Courtesy Prange, 2006
ejection ofplasma intothe magnetotail
Courtesy Prange, 2006
returning of a« magnetic loop »back to the dayside
Courtesy Prange, 2006
Courtesy Prange, 2006
ClusterDouble StarThemisMMS
EarthDynamic Explorer )
UV - 130 nm(Courtesy . L. Frank)
SaturnHST-STIS
UV - 130 nm(R. Prangé & L Pallier)
JupiterHST-STIS
UV - 150 nm(R. Prangé & L Pallier)
PLANETARY AURORAE
a fascinating phenomen at and around the magnetis poles of magnetized planets
EarthDynamic Explorer )
UV - 130 nm(Courtesy . L. Frank)
SaturnHST-STIS
UV - 130 nm(R. Prangé & L Pallier)
JupiterHST-STIS
UV - 150 nm(R. Prangé & L Pallier)
PLANETARY AURORAE
a fascinating phenomen at and around the magnetis poles of magnetized planets
Summary:
Prospect for tomorrow:Saturn, seen by Cassini
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