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MHD and the Solar Dynamo

  • ARNOLD HANSLMEIER
Part of the ASTROPHYSICS AND SPACE SCIENCE LIBRARY book series (ASSL, volume 347)

Abstract

In this chapter we will explain the basic MHD equations which are needed to understand solar active phenomena such as spots, prominences, flares etc. The solar dynamo is needed to maintain the solar activity cycle1.

Keywords

Solar Wind Solar Activity Drift Velocity Magnetic Reconnection Convection Zone 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer 2007

Authors and Affiliations

  • ARNOLD HANSLMEIER
    • 1
  1. 1.Institute of Physics/ IGAMUniversity of GrazAustria

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