1. Arnold Hanslmeier Institut für Physik/Geophysik, Astrophysik und Meteorologie. Graz arnold.hanslmeier@kfunigraz.ac.at

2.  Basic facts:  G2V star TT  Surface: 5800 K  center: 15 000 000 K  Age: 4.5 Billion years  150 000 000 km distance  Constant star ???

12. Earth

13. 2-D Powerspectra: Velocity ~ k -5/3 Intensity ~ k -5/3 k<k c ~ k -17/3 k>k c K c separates convective from diffusive range Kolmogorov Theory of isotropic turbulence

15.  Variation with solar activity cycle  Observatoire Pic du Midi, Univ. Toulouse  Generation of acoustic flux and its relation to shocks and turbulence  Instituto de Astrofisica de Canarias, Tatranska Lomnica, Kiepenheuer Institut, Univ. of Colorado, Univ. of Chicago  3-D HD and MHD simulations  Univ. of Vienna, Univ. of Colorado

17. Umbra: T 4000 K Penumbra: T 5500 K Photosphere: T 6000 K

18. Sunspots: strong magnetic Fields – Umbra: vertical Penumbra: horizontal

19. The surface intensity shows the sunspot with the dark central umbra surrounded by the somewhat brighter, filamentary penumbra. The second plane cuts from the surface to 24000 km deep showing areas of faster sound speed as reddish colors and slower sound speed as bluish colors. The third plane (bottom) is a horizontal cut at a depth of 22000 km showing the horizontal variation of sound speed.

21.  Dynamo Coriolis, convection Diff. Rotation

22.  Magnetic field  Convection zone – surface  Magnetic buoyancy  Differential rotation   Stellar dynamo   Intermittency??

23. Activity on main sequence: types F  M B-V > 0.4 Evidence of magnetic activity 

24. Sunspot deficit compensation

25. Magnetic flux Tachocline Sunspots, bipolar groups Photosphere Chromosphere Faculae, Flares Corona CMEs, Solar Wind

32. u = u 0 + d u

38.  A variety of effects from the particles:  Total dose  Lattice displacement damage  Single events upsets (SEE)  Noise in sensor  Spacecraft charging

39.  Cosmic radiation: (protons, highly ion. Heavier nuclei); production of atmospheric secondaries (effects in aircraft systems and sea level electronics); SEEs, background noise  Solar particle events : increase of SEEs; significant enhancements in the radiation at supersonic aircraft altitudes.  Inner Radiation Belt: dose damage, noise and SEE  Outer Radiation Belt : energetic electrons; cummulative dose and dammage effects; deep dielecrtic charging (responsible for anomalies and losses); surface charging anomalies.

40.  Temperature, composition and horizontal winds in the Earth‘s atmosphere at orbital altitudes above 120 km are all influenced by variations of solar and geomagnetic activity.  Atmospheric drag: F=C ½  v^2A  Solar radiation force: F=C I/cS, S cross sectional area perpendicular to the direction of solar rays.

42. Red: density increase by 20% during a magnetic storm. Emissions from the sun: UV, X; if in addition Magnetic activity is triggered at Earth, intense currents flowing through the upper Atmosphere and energy deposited by high speed particles increase the heating and expansion of the Atmosphere.

45.  Kanzelhöhe: H-Alpha Magnetograms Intensity at various wavelengths International network

50.  LASCO

51.  Dynamics of the solar atmopshere  Solar convection – models and observations  Flares and CMEs  Wave phenomena in the upper solar atmosphere  Space Weather  Kanzelhöhe: Monitoring  Cooperations:  Hvar Observatory, Cro  Tatranska Lomnica, Sk  Observatoire Pic du Midi, F  Instituto de Astrofisica de Canarias, E  University of Glasgow, UK  Niels Bohr Institute of Astrophysics, Copenhagen, Dk  Kiepenheuer Institut f. Sonnenphysik, Freiburg, D  Astrophysikal. Institut Potsdam, D  Univ. of Colorado, Boulder, USA  Big Bear Solar Observatory, USA  Bangalore Indian Institute of Astrophysics, India