<html><head><meta http-equiv="Content-Type" content="text/html charset=utf-8"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;" class=""><div class="">Dear all,</div><div class=""><br class=""></div><div class="">Here is a paper that Yi-Ming Wang has asked me to send for him. He’s not a member of the mailing list yet.</div><div class=""><br class=""></div><div class="">Best regards,</div><div class="">Ignacio</div><div class=""><br class=""></div><div class=""><br class=""></div><div class=""><a href="http://iopscience.iop.org/article/10.3847/2041-8205/820/1/L13" class="">http://iopscience.iop.org/article/10.3847/2041-8205/820/1/L13</a></div><div class=""><br class=""></div><div class=""><h1 itemprop="headline" class="wd-jnl-art-title" style="margin: 0px 1em 0.25em 0px; padding: 0px; border: 0px; font-weight: inherit; font-stretch: inherit; line-height: 1.25; font-family: franklin-gothic-urw-cond, sans-serif; vertical-align: baseline; color: rgb(51, 51, 51); widows: 1;"><span style="font-size: 12px;" class="">"THE UBIQUITOUS PRESENCE OF LOOPLIKE FINE STRUCTURE INSIDE SOLAR ACTIVE REGIONS"</span></h1></div><div class=""><span style="font-size: 12px;" class="">Y.-M. Wang</span></div><div class=""><span style="color: rgb(51, 51, 51); line-height: 1.25; widows: 1;" class=""><br class=""></span></div><div class=""><span style="color: rgb(51, 51, 51); line-height: 1.25; widows: 1;" class="">Abstract</span></div><div class=""><div class="wd-jnl-art-abstract cf article-text" itemprop="description" style="margin: 0px; padding: 0px; border: 0px; font-stretch: inherit; line-height: 1.5; vertical-align: baseline; color: rgb(51, 51, 51); widows: 1;"><p style="margin: 0px 0px 1em; padding: 0px; border: 0px; font-style: inherit; font-variant: inherit; font-stretch: inherit; line-height: inherit; vertical-align: baseline;" class="">Although most of the solar surface outside active regions (ARs) is pervaded by small-scale fields of mixed polarity, this magnetic "carpet" or "junkyard" is thought to be largely absent inside AR plages and strong network. However, using extreme-ultraviolet images and line-of-sight magnetograms from the <i style="margin: 0px; padding: 0px; border: 0px; font-variant: inherit; font-stretch: inherit; line-height: inherit; vertical-align: baseline;" class="">Solar Dynamics Observatory</i>, we find that unipolar flux concentrations, both inside and outside ARs, often have small, loop-shaped Fe <span class="sml" style="margin: 0px; padding: 0px; border: 0px; font-style: inherit; font-variant: inherit; font-stretch: inherit; line-height: inherit; vertical-align: baseline;">ix</span> 17.1 and Fe <span class="sml" style="margin: 0px; padding: 0px; border: 0px; font-style: inherit; font-variant: inherit; font-stretch: inherit; line-height: inherit; vertical-align: baseline;">xii</span> 19.3 nm features embedded within them, even though no minority-polarity flux is visible in the corresponding magnetograms. Such looplike structures, characterized by horizontal sizes of ~3–5 Mm and varying on timescales of minutes or less, are seen inside bright 17.1 nm moss, as well as in fainter moss-like regions associated with weaker network outside ARs. We also note a tendency for bright coronal loops to show compact, looplike features at their footpoints. Based on these observations, we suggest that present-day magnetograms may be substantially underrepresenting the amount of minority-polarity flux inside plages and strong network, and that reconnection between small bipoles and the overlying large-scale field could be a major source of coronal heating both in ARs and in the quiet Sun.</p></div></div></body></html>