Properties of the magnetic fields of coronal holes with active regions

Details Properties of the magnetic fields of coronal holes with active regions Properties of the magnetic fields of coronal holes with active regions

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010bcrao.106....1f&link_type=abstract

Bulletin of the Crimean Astrophysical Observatory, Volume 106, Issue 1, pp.1-7

Astronomy and Astrophysics

Astrophysics

Sun, Coronal Holes, Active Regions, Magnetic Fields

Scientific paper

We determine the structure of the magnetic fields of coronal holes (CHs) and investigate its change in connection with the emergence of active regions (ARs) in CHs. Based on our observations in the HeI 1083 nm line performed with the CrAO TST-2 telescope, we have selected CHs of two types: without (15 CHs) and with (28 CHs) ARs. Magnetograms obtained at the Kitt Peak National Solar Observatory have been used to calculate the magnetic fields of the same objects. We have calculated magnetic field characteristics by Rudenko’s method in the potential approximation at several heights in the corona, namely, the average (over the CH area) radial field component < B r > and its magnitude <| B r |/ B> and the maximum and minimum (over the CH area) values of B r . The distributions of the isolines of these parameters superimposed on the CH images and the field lines of the calculated magnetic field have been constructed with resolutions of 33.4″ and 100.2″ on the solar surface. Analysis of these data has yielded the following results:
The field lines originating in CHs without ARs are open or very high loops that are closed outside CHs. The latter occurs in completely or partially closed CHs.

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