Magnetic fine structure in coronal holes.

Details Magnetic fine structure in coronal holes. Magnetic fine structure in coronal holes.

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998arbes...4..115d&link_type=abstract

Astrophysics Reports, Special Issue, No. 4, p. 115 - 117

Astronomy and Astrophysics

Astrophysics

Solar Coronal Holes: Magnetic Fields

Scientific paper

Statistical results are summarized about the magnetic fine structure in coronal holes (CHs) and other structure (Hα bright points, He I dark point, soft X-ray bright points (XBPs) in solar atmosphere issued in 1973 - 1993. The magnetic helicity of an ephemeral region (ER) is estimated to use the data of photospheric fine magnetic fields observed in 26 - 30 Sept 1989. The upper limit of the magnetic flux in an ER ejected is about 6% of the total flux into the interplanetary space. The difference of the magnetic helicity between a CH and solar quiet region is about 2×1037MX2. The boundary region of a CH is contracting when XBPs in the CH become brighter associated with ERs increasing, if XBPs are correlated with ERs. The boundary region of the CH is expanding when XBPs become dimming associated with ERs decaying.

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