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Space Research Institute Graz Austrian Academy of Sciences

Exploring the and in our

Helmut O. Rucker

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

Exploring the Planets and Moons in our Solar System • The , the and its interaction with magnetized planets

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

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

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

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

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

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

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

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

CERN, Geneve, June 2006 Space Research Institute Graz Austrian Academy of Sciences

The interplanetary medium, the solar wind and its interaction with magnetized planets Helmut O. Rucker

CERN, Geneve, June 2006 The central star of our solar system – the Mass loss by the expanding solar atmosphere, i.e. the solar wind: ~ 1 Mill. tons per second Viewgraph: Helmet streamer The solar wind = expanding atmosphere of the Sun highly conducting , radially propagating (300 km/s < v < 2000 km/s)

r vsw The solar wind = expanding atmosphere of the Sun highly conducting plasma, radially propagating (300 km/s < v < 2000 km/s)

The interplanetary is a solar magnetic field r B drawn out of the Sun IMF by the highly conducting solar wind plasma. Due to the solar rotation a spiral structure is formed. Parker spiral: ω r tan =Ψ sun vsw

ωsun = π × s)400,8638.25/(2 −− 16 ωsun ×= 1086.2 s −1 vsw = 450kms

ψ AUr 6.43)0.1( °== ψ AUr 7.83)5.9( °== 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

r M D

2 = rr 0 sin ϑ Interaction between the solar wind and planetary magnetic field

1 ⎛ c +TTnk )( ⎞ 2 Solar wind bulk flow = super-sonic flow ⎜ p ie ⎟ vsonic = ⎜ ⎟ ⎝ cV nm ⎠ B = super-Alfvenic flow vA = 0 ρμ Interaction between the solar wind and planetary magnetic field

Bow shock:

Transition of solar wind plasma described by the Rankine Hugoniot equations. Change after transition: bulk speed particle density plasma pressure plasma temperature 3D schematics of the terrestrial

magnetopause boundary conditions:

22 2 nmv cos α = B 2/ μ 0

B n = 0 Magnetotail cross section at r = 20 Re Magnetic reconnection

B

B Magnetic reconnection

B

B Magnetic reconnection

B

B Courtesy Prange, 2006 Courtesy Prange, 2006 1st reconnection = start of the cycle

Courtesy Prange, 2006 Courtesy Prange, 2006 Courtesy Prange, 2006 transport over the poles

Courtesy Prange, 2006 Courtesy Prange, 2006 2nd reconnection

Courtesy Prange, 2006 impulsive acceleration Release of energy ( the stretched configuration contains additional energy to accelerate plasma)

Courtesy Prange, 2006 ejection of plasma into the magnetotail

Courtesy Prange, 2006 returning of a « magnetic loop » back to the dayside

Courtesy Prange, 2006 Courtesy Prange, 2006 dawn

Inner-magnetospheric electric fields

dusk

dawn Inner-magnetospheric particle drift paths and plasmasphere iso-potential lines, resp.

dusk Cluster Double Star Themis MMS PLANETARY AURORAE a fascinating phenomenon at and around the magnetic poles of magnetized planets

Earth Dynamic Explorer ) HST-STIS HST-STIS UV - 130 nm UV - 150 nm UV - 130 nm (Courtesy . L. Frank) (R. Prangé & L Pallier) (R. Prangé & L Pallier) PLANETARY AURORAE a fascinating phenomenon at and around the magnetic poles of magnetized planets

Earth Jupiter Saturn Dynamic Explorer ) HST-STIS HST-STIS UV - 130 nm UV - 150 nm UV - 130 nm (Courtesy . L. Frank) (R. Prangé & L Pallier) (R. Prangé & L Pallier)

Summary: Magnetic field representation −= gradB Φ

∞ n n+1 ⎧ m m m ⎫ =Φ pp )/( ⎨∑∑ n ϑ []n cos)(cos ϕ + n sin mhmgPrrr ϕ ⎬ n=1 ⎩m=0 ⎭

Φ magnetic potential rp planetary radius m Legendre polynom Pn ϑ polar distance angle m m spherical harmonic coefficients n ,hg n ϕ planetocentric longitude Magnetic properties of the magnetized planets Classification of magnetospheric structures

r r r M dipole Ω n

plane, seen edge on solar wind bulk velocity

t0 t0 + ½ planetary rotation r r r Ω , nr Ω, M Earth 23.45° 11.4° Jupiter 3.1° 9.6° „symmetrical“ Saturn 26.7° +/- 0° Magnetic field of Jupiter Classification of magnetospheric structures

Uranus (1986) nr

ecliptic plane, seen edge on r solar wind bulk velocity Ω r M dipole

t0 t0 + ½ planetary rotation r r r Ω , nr Ω, M 97.8° 58.6° 28.3° 46.9° „oblique rotators“ Classification of magnetospheric structures

Neptune (1989) r r M dipole Ω nr

ecliptic plane, seen edge on solar wind bulk velocity

t0 t0 + ½ planetary rotation r r r Ω , nr Ω, M Uranus 97.8° 58.6° Neptune 28.3° 46.9° „oblique rotators“ „Advertisement“ for tomorrow: Space missions to the outer planets

Saturn, as seen by Cassini