Abstract

1. Abstract Case 2: Active region 10940 and filament structure observed Feb 02, 2007 The combination of multi-wavelength, high resolution, high cadence data from the Hinode X-Ray Telescope (XRT) and the Transition Region And Coronal Explorer (TRACE) give a unique view of solar active region dynamics and topology in different wavelengths. We present results from NOAA active region 10930, observed in December 2006, and active region 10940, observed in February 2007. Co-alignment of XRT and TRACE data yield a striking combination of a filament structure observed in TRACE and hot XRT loops that lie both above and along the filament channel. In the December case, overlying loops exhibit remarkable dynamics while the filament lies dormant, and numerous x- point and triple-leg structures undergo repeated brightenings. We find that TRACE and XRT observations are complementary, and correlation of these data facilitates co-alignment with other instruments. SOLIS LOS magnetic field GHN H-alpha XRT Thin-Be 2007/02/02 08:05 2007/02/02 08:05 Contour overlay Magnetic Field Calculation Non-linear force free field model for 2007 February 2 at 16:37 UT. The model contains a dextral flux rope with an axial flux of 6x1020 Mx and a poloidal flux of -6x10-10 Mx/cm. (a) Contours from SOLIS data (red=positive, green=negative), plotted with selected field lines inside the flux rope. (b) Same contours plotted on H-alpha image from Kanzelhohe Observatory, taken at 08:05 UT. (c) Same contours plotted on TRACE 195 image, taken at 1819 UT. (d) Fieldlines added to TRACE data. (a) (b) (c) (d) The combination of multi-wavelength, high resolution, high cadence data from the Hinode X-Ray Telescope (XRT) and the Transition Region And Coronal Explorer (TRACE) give a unique view of solar active region dynamics and topology in different wavelengths. We present results from NOAA active region 10930, observed in December 2006, and active region 10940, observed in February 2007. Co-alignment of XRT and TRACE data yield a striking combination of a filament structure observed in TRACE and hot XRT loops that lie both above and along the filament channel. In the December case, overlying loops exhibit remarkable dynamics while the filament lies dormant, and numerous x- point and triple-leg structures undergo repeated brightenings. We find that TRACE and XRT observations are complementary, and correlation of these data facilitates co-alignment with other instruments. A Multi-Wavelength View of an Active Region Structure around a Filament ChannelL. Lundquist,1 K. Reeves,1 A. van Ballegooijen,1 T. Sakao,2 and the XRT Team1Harvard Smithsonian Center for Astrophysics 2Institute of Space and Astronautical Science, JAXA Case 1: Active region 10930, Dec 14, 2006 Overlay of XRT and TRACE Overlay of XRT and TRACE XRT AL/poly 2-Feb-2007 18:18 TRACE 195 2-Feb-2007 18:19, with XRT contours Co-alignment of XRT and TRACE data reveal complementary structures and illuminate the relationship between the filament channel and the hot X-ray loops. Loops lying both along and above the filament apparently result in the many x-point reconnection events observed at the intersection of these two types of loops. XRT Thin-Be 2006-Dec-14 10:57 Hot x-ray loops with cool “moss” footpoints arc over the filament TRACE 195 2006-Dec-14 10:57 XRT contours overlaid on TRACE 195 data again show “moss” structures at the base of hot loops. Some X-ray structures appear to lie along the filament Tri-leg reconnection example Tri-leg reconnection event Before small flare During this small flaring event, brightenings along the filament channel are observed, followed by this apparent reconnection of the filament-overlying and filament-parallel structures. Similar examples are repeated about three times. Flare and H-alpha context Conclusions and Future Work Kanzelhohe H-alpha GOES X-ray flux XRT and TRACE present complementary high- and low-temperature views of the active region corona. AR 10930 shows a fascinating example of hot X-ray loops both along and above a filament channel, which reconnect repeatedly in x-point and tri-leg structures. The location and orientation of the hot loops with respect to the filament is made clear only through comparison with TRACE. Aligning data from the two instruments remains challenging, and in this poster, it is still being done at the level of manual feature comparison. In the case of the December 2006 data, we were able to use the footpoint moss structures and presence of a filament channel to align the data sets by eye. In the case of the February 2007 data set, the primary alignment is still done by hand, but we are aided by the additional information from secondary data sets. MDI or SOLIS data, for example, provide a full-sun image that can be aligned by the limb to full-Sun XRT images. They also provide white light data which can be compared to TRACE white light data. Future work will explore the efficacy of this approach. A similar method will be applied to to Hinode XRT-SOT co-alignment in the absence of G-band observations from XRT. The repeated small flares in most cases involves reconnection of the structures lying along the filament and those lying over it.