Solar Physics

, Volume 285, Issue 1, pp 9–24

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

Authors

    • Institute for AstronomyUniversity of Hawaii
  • H. Morgan
    • Institute for AstronomyUniversity of Hawaii
  • M. Druckmüller
    • Brno University of Technology
  • A. Ding
    • Institute of Optics and Atomic PhysicsTechnische Universitaet Berlin, and Institute of Technical Physics
  • J. F. Cooper
    • Heliophysics Science DivisionNASA/GSFC
  • A. Daw
    • Heliophysics Science DivisionNASA/GSFC
  • E. C. SittlerJr.
    • Heliophysics Science DivisionNASA/GSFC
OBSERVATIONS AND MODELLING OF THE INNER HELIOSPHERE

DOI: 10.1007/s11207-012-0115-5

Cite this article as:
Habbal, S.R., Morgan, H., Druckmüller, M. et al. Sol Phys (2013) 285: 9. doi:10.1007/s11207-012-0115-5

Abstract

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.

Keywords

CoronaEclipseSolar wind

Copyright information

© Springer Science+Business Media B.V. 2012