space research institute graz austrian academy of sciences cern, geneve, june 2006 helmut o. rucker...
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![Page 1: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/1.jpg)
Space Research Institute GrazAustrian Academy of Sciences
CERN, Geneve, June 2006
Helmut O. Rucker
Exploring the Planets and Moons in our Solar System
![Page 2: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/2.jpg)
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
![Page 3: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/3.jpg)
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
![Page 4: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/4.jpg)
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
![Page 5: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/5.jpg)
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
![Page 6: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/6.jpg)
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
![Page 7: Space Research Institute Graz Austrian Academy of Sciences CERN, Geneve, June 2006 Helmut O. Rucker Exploring the Planets and Moons in our Solar System](https://reader036.vdocuments.site/reader036/viewer/2022062518/56649edd5503460f94bee57f/html5/thumbnails/7.jpg)
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
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The central star of our solar system – the Sun
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Mass loss by theexpanding solar atmosphere, i.e. the solar wind:~ 10 E6 tons per second
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Viewgraph: Helmet streamer
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The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)
swv
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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)
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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
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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 %
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Solar wind average properties at r ~ 1 AU:
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Dipole structure
20 sinrr
DM
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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
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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
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3D schematics of the terrestrial magnetosphere
magnetopauseboundary conditions:
0
2/cos 0222
nB
Bnmv
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Magnetic reconnection
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Magnetic reconnection
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Magnetic reconnection
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Courtesy Prange, 2006
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Courtesy Prange, 2006
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1st reconnection = start of the cycle
Courtesy Prange, 2006
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Courtesy Prange, 2006
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Courtesy Prange, 2006
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transportover the poles
Courtesy Prange, 2006
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Courtesy Prange, 2006
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2nd reconnection
Courtesy Prange, 2006
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impulsiveacceleration
Release of energy( the stretched configurationcontains additionalenergy to accelerateplasma)
Courtesy Prange, 2006
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ejection ofplasma intothe magnetotail
Courtesy Prange, 2006
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returning of a« magnetic loop »back to the dayside
Courtesy Prange, 2006
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Courtesy Prange, 2006
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ClusterDouble StarThemisMMS
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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
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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
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Summary:
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Prospect for tomorrow:Saturn, seen by Cassini