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“…From previous publications (Harvey et al, 1982;DeForest et al, 1997;Wilhelm, 2000;Belenko, 2001) we know that the magnetic flux in coro- There is a clear trend for the loop height to decrease with Bz |Bz| , the correlation coefficient between these two quantities being r c = −0.87. Interestingly the loop length is not so strongly correlated (r c = −0.57), mainly because of CH3 and CH6, which have anomalously long loops (but not strikingly high ones).…”
Section: What Magnetic Features Are Responsible For Coronal Holes?mentioning
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“…From previous publications (Harvey et al, 1982;DeForest et al, 1997;Wilhelm, 2000;Belenko, 2001) we know that the magnetic flux in coro- There is a clear trend for the loop height to decrease with Bz |Bz| , the correlation coefficient between these two quantities being r c = −0.87. Interestingly the loop length is not so strongly correlated (r c = −0.57), mainly because of CH3 and CH6, which have anomalously long loops (but not strikingly high ones).…”
Section: What Magnetic Features Are Responsible For Coronal Holes?mentioning
“…The magnetic field strength in the photosphere beneath coronal holes has been measured by several authors, (e.g., Levine 1977, Bohlin and Sheeley 1978, Harvey et al 1982, DeForest et al 1997, Belenko 2001. The magnetic flux in coronal holes clearly shows a dominant polarity.…”
Section: Introductionmentioning
“…The number of non-polar coronal holes increases during the rising phase of the solar cycle (Belenko 2001). Locations of individual coronal holes change significantly on the solar disk every day.…”
Section: Analysis and Resultsmentioning
“…The smaller details are represented by the harmonics of higher order. The harmonic coefficients for 1904-1984Carrington rotations (1996-2001 from the Wilcox Solar Observatory were used.…”
Section: Analysis and Resultsmentioning
“…A detailed analysis of high-resolution magnetograms shows that network magnetic elements within the coronal holes are predominately of the same polarity. The ratio of areas occupied by opposite polarities is 1:4 within the coronal holes, while it is about 1:1 in quiet regions (Varsik et al 1999;Belenko 2001). In regions of mixed polarities, a lot of field lines do not rise high into the corona as they connect the nearby patches of opposite polarity, whereas in the regions of predominant polarity most of the field lines reach high altitude (Fig.…”
Section: Introductionmentioning