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Y. Yamauchi, H. Wang (NJIT), R.L. Moore (NASA/MSFC)
Small-scale solar dynamics, e.g., spicules and macrospicules, in coronal holes are believed to play an important role in the coronal heating and solar wind acceleration. Since photospheric magnetic flux observations have shown that there is a small fraction of opposite polarity in the coronal holes [e.g., DeForest et al., 1997, Sol. Phys., v175(2), 393-410], network magnetic fields in supergranule boundary are likely to be the most important factors responsible for the dynamics. However, the formation mechanism of macrospicules remains controversial, in particular in the relation with magnetic field arrangement at the base of macrospicules. At the last SPD meeting, from H-alpha limb observations from Big Bear Solar Observatory (BBSO), we reported that most macrospicules have one or the other of two forms, that of an erupting loop or that of a spiked jet. Each of these magnetic structural forms indicates that the macrospicule is rooted in mixed polarity magnetic flux [Yamauchi et al 2004, ApJ, in press]. Here, we have investigated BBSO on-disk H-alpha and magnetic data in coronal holes to find the disk counterparts of each type of macrospicules on the limb, such as microflares, mini-filament eruptions, or H-alpha jets. We will report results from the analysis and discuss the production of macrospicules in relation to the polarity arrangement and evolution of the network magnetic flux.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.