The Origin of the Magnetic Fields Divergence in Coronal Holes

Details The Origin of the Magnetic Fields Divergence in Coronal Holes The Origin of the Magnetic Fields Divergence in Coronal Holes

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..591f&link_type=abstract

MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp

Other

Solar Corona, Magnetic Fields, Solar Wind, Particle Emission, Solar Wind, Magnetohydrodynamics And Plasmas

Scientific paper

The solar atmosphere presents complexe magnetic structures, such as loops and coronal holes, which are intrinsically bounded to the solar wind acceleration and driven mechanism. UVCS/SOHO and ground observations gave a new insight on the problem. Using H I Lyman alpha and O VI line intensity distributions it is possible to identify the coronal holes boundaries, showing a super-radial geometry with diverging factor fmax ranging from 6.0 to 7.5. It is not clear yet if other stars present such structures. However, the diverging magnetic fields play an important role in the stellar winds. In this work we develop a method for determining the magnetic divergence based on its tension generated by an increase in gas pressure at the wind basis.

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