Kernels and Ribbons

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Introduction

A solar flare has a complicated three-dimensional structure involving all layers of the solar atmosphere. Many of the models that we use to explain them, though, are inherently two-dimensional and indeed often involve the concept of the current sheet, geometrically a manifold with only two dimensions. On the other hand, modern theories of magnetic reconnection require three-dimensionality to make the plasma physics work.

Many of the observations also seem to point to intrinsic two-dimensionality. Chief among these are the flare ribbons, the magnetic footpoints of an arcade of loops that looks entirely consistent with the presence of a large-scale current sheet in the solar corona. One observation that generally does not agree with this picture is the hard X-ray picture (e.g. RHESSI's), and this one is fundamentally important to understand because the hard X-rays show us where the flare energy appears. Instead of ribbons, the hard X-rays usually show a much simpler structure, often two bright compact sources termed "footpoints" on the reasonable assumption that they show the two ends of a thin coronal magnetic loop. This nugget studies the fine structure of footpoints (seen in hard X-rays) and ribbons (seen in the UV) in a search for an answer to the simple geometrical (2D vs 3D?) question.

Revisiting the Bastille Day Flare

To explore the relationship between hard X-ray and UV emissions at the feet of flare loops, we revisit one of the best known two-ribbon flares, the Bastille day [1], which occurred at 10 UT on 2000 July 14, and was observed by Yohkoh and [2] among others. Figure 1 gives snapshots of the flare evolution that these satellites measured in hard X-ray and UV wavelengths, superimposed on an array of [magnetic poles], a simple way to model the complicated solar magnetic field. The color code shows evolution of UV brightening, which spreads both along the magnetic polarity inversion line (PIL) in a nearly organized manner from the west to the east and perpendicular to and away from the PIL as would be expected in the 2D reconnection model. The hard X-ray images in the left panel are obtained by the Maximum Entropy Method embedded in the SolarSoftware package. The >20 keV hard X-ray emission of the flare exhibits 2 to 3 compact sources in magnetic fields of opposite polarities. During the flare evolution, the hard X-ray sources gradually shift along the PIL, similar to the evolution pattern of UV brightening. Figure 2 shows the light curves of the flare observed in hard X-ray, UV 1600~\AA continuum, and soft X-ray 1-8\AA\ by GOES. The UV light curve is a sum of all counts in UV images. It rises and peaks together with hard X-rays, but decays more slowly well after the decay of hard X-rays. Note that for this flare, Yohkoh/HXT only observed from 10:20~UT.

Figure 1: Maps of the Bastille Day flare, superposed on an array of positive (P) and negative (N) poles used to characterize the solar magnetic field. <it>Left:</it> hard X-rays; <it>right:</it> UV ribbons time-coded according to the bar at the bottom. Note that both emissions tend to have EW elongations lying in opposite polarities.

The revisit raises some interesting questions. First, obviously, the evolution and mapping of UV and hard X-ray sources reflect the pattern of magnetic reconnection which is not entirely 2-dimensional, and second, the coincident rise and peak but delayed decay in UV emission with respect to hard X-ray emission suggests some different physics, not directly related to hard X-ray producing process, taking place during the gradual decay of UV emission.