Observations of the Sun's Coronal Magnetic Field and Coronal Holes during the Recent Ulysess Second Polar Pass, and Implications for Particle Observations

Details Observations of the Sun's Coronal Magnetic Field and Coronal Holes during the Recent Ulysess Second Polar Pass, and Implications for Particle Observations Observations of the Sun's Coronal Magnetic Field and Coronal Holes during the Recent Ulysess Second Polar Pass, and Implications for Particle Observations

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh32a0723s&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH32A-0723

Physics

2100 Interplanetary Physics, 2114 Energetic Particles, Heliospheric (7514), 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536)

Scientific paper

We combine magnetic field observations from the Wilcox Solar Observatory and coronal hole observations from the National Solar Observatory/ Kitt Peak. At solar minimum, the Sun's coronal magnetic field was dipolar and aligned along the spin axis. The current sheet was flat and had very little warp. Around solar maximum, during the second Ulysses southern polar pass, the ratio of quadrupole to dipole strength was high for much of the time. This meant that the current sheet was tilted and highly warped, and reached up to high latitudes. Using the dipole and quadrupole terms from the expansion of the coronal magnetic field, we compute the position of the dipole and quadrupole poles. We find that the location of coronal holes follows the motion of the poles of the magnetic field as the poles move across the surface of the Sun. The polar coronal holes break up into groups of smaller holes all with the same polarity as the poles approach the mid-latitude regions. Surprisingly, there were also times close to solar maximum when the quadrupole/dipole ratio was low, and the current sheet was relatively flat, but still highly inclined. We discuss the implications for the observations of energetic particles at Ulysses.

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