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Primary Goals:

• Characterize the 3-D solar minimum heliosphere
  
• Trace the effects of solar structure and activity through the solar wind to the Earth and other planetary systems

To accomplish the first goal, synoptic observing programs will be run throught WHI, and several targeted observing campaigns have been identified. These observations will be interpreted and connected with the aid of models, providing a phenomenological framework.

Once the 3-D solar minimum heliosphere is characterized in this manner, cross-disciplinary science questions can be addressed (please email Sarah Gibson or Barbara Thompson to suggest revisions/additions to this list):

WHI science questions (* indicates the system needs to cooperate and provide the structure of interest during WHI):

• What is the impact of a solar minimum "ground state", in particular a 3-D solar magnetic field with predominantly open flux and a lack of solar activity, on
• solar-driven Ionosphere-Thermosphere-Mesosphere coupling?
  
• cosmic ray modulation?
• morphology of heliosphere?
• solar and magnetospheric magnetic energy storage/release (see below)?
• and once we've answered these questions, does it help us interpret historical record?
  

• Physics at boundaries
• what can we learn from composition boundaries (at Sun and in solar wind)?
• at plasma/neutral boundaries?
  
• how about density boundaries (plume/interplume, streamer/hole - at Sun and in solar wind)?
• magnetic boundaries (current sheets/sector boundaries, magnetopauses)?
• is there evidence for interchange reconnections at coronal hole boundaries?

• How is magnetic energy transported through system?
• how do solar sub-surface structures/flow relate to magnetic flux emergence?
• how does flux emergence/reconnections/MHD waves affect evolution of solar magnetic structures?
• how do structures (both *eruptive and non) evolve in solar wind from sun to heliopause?
  
• how do they interact with planetary magnetospheres and geospace?
  

   

The Solar Minimum Sun:    3-D Global Magnetic Field    Subsurface Flows and Flux Emergence    Characterize the Solar Chromosphere    *Magnetic Active Regions    *Filaments and cavities    Coronal Streamers    Polar Coronal Holes and Polar Plumes    *Equatorial Coronal Holes Solar Variability:    Irradiance Variations    *Flares and CME's Heliospheric Structure:    Slow Solar Wind    Fast Solar Wind    *Corotating Iteraction Regions (CIR's)    *ICME's and Magnetic Clouds

Geospace Impacts:    Magnetospheric Structure    ITM Coupling    *Magnetic Storms    *Ionospheric Disturbances Planetary Systems:   Mars   Saturn   Jupiter Outer Heliosphere:   Structure at Voyager Orbits   IBEX 3-D Structure