Solar Physics

, Volume 285, Issue 1, pp 9-24

First online:

Probing the Fundamental Physics of the Solar Corona with Lunar Solar Occultation Observations

  • S. Rifai HabbalAffiliated withInstitute for Astronomy, University of Hawaii Email author 
  • , H. MorganAffiliated withInstitute for Astronomy, University of Hawaii
  • , M. DruckmüllerAffiliated withBrno University of Technology
  • , A. DingAffiliated withInstitute of Optics and Atomic Physics, Technische Universitaet Berlin, and Institute of Technical Physics
  • , J. F. CooperAffiliated withHeliophysics Science Division, NASA/GSFC
  • , A. DawAffiliated withHeliophysics Science Division, NASA/GSFC
  • , E. C. SittlerJr.Affiliated withHeliophysics Science Division, NASA/GSFC

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Imaging and spectroscopy of the solar corona, coupled with polarimetry, are the only tools available at present to capture signatures of physical processes responsible for coronal heating and solar wind acceleration within the first few solar radii above the solar limb. With the recent advent of improved detector technology and image processing techniques, broad-band white light and narrow-band multi-wavelength observations of coronal forbidden lines, made during total solar eclipses, have started to yield new views about the thermodynamic and magnetic properties of coronal structures. This paper outlines these unique capabilities, which until present, have been feasible primarily with observations during natural total solar eclipses. This work also draws attention to the exciting possibility of greatly increasing the frequency and duration of solar eclipse observations with Moon orbiting observatories utilizing lunar limb occultation of the solar disk for coronal measurements.


Corona Eclipse Solar wind