2008-01-01T23:11:06.000Z http://sot.lmsal.com Ed DeLuca SAO http://hea-www.harvard.edu MS 58, 60 Garden St, Cambridge, MA 02138 +1-617-496-7725 edeluca@cfa.harvard.edu Hinode XRT ARIKAWA, Yusuke NARUKAGE, Noriyuki ISHIBASHI,Kazunori 53 0 null Enginnering Exposures for MDP Comression QS QR 0 0 0 0 0 2007-12-30T06:09:54.000Z 2008-01-04T10:05:00.000Z 0 0 CORE: SOT continuous magnetic field observations for investigating mechanisms responsible for XBPs and QS dynamics Engineering_Compression_Test Daily Note: ***** OP start after OKN1 pass. ***** The OP to be uploaded covers the observing final plan and backup until Jan 4. 4 commanding paaaes are scheduled because the memory size of the OP will be larger than usual. Note: XRT is conducting Remote Operations this week. Please continue to use Yugma for the Morning Operations Meetings, and dial in to the telecon phone number (see telephone-number card in Hinode morning-meeting room). To contact the XRT Chief Observer, please call +1-617-496-1156 (US phone number). XRT * Continue flare detection mode. * Conduct test for Full Sun Movie program * Engineering test for XRT data compression EIS: * Quiet region near disk center (including HOP53) Continuous tracking for a few days is preferred * TOO: Active region loops near the limb SOT: * HOP53 * TOO: dark filament; Request to XRT HOP Number 0053: ; Other Instruments: NONE; Scientific Objectives: Previous magnetic-field observations (/w 1-2 arcsec spatial resolution, longitudinal only) shows that magnetic cancellation is involved in many XBPs and magnetic emergence in a limited number of XBPs (e.g., Harvey et al.) Priest and Parnell (1994) proposed a magnetic canceling model for explaining the overall evolution of XBPs. However, this model has not yet been confirmed with observations. SOT has not yet performed magnetic-field observations suitable for investigating mechanisms responsible for XBPs (see Kotoku et al. 2007 PASJ). The biggest problem in the observations made so far with Hinode is that continuous SOT observations are available only in a few - several hours, which is much shorter than the lifetime of XBPs (8 hrs for small typical XBPs, 48hrs for bigger XBPs) and time-scale of small-scale magnetic field evolution (Schrijver et al. 1998). We are lack of observations with continuous a-few days tracking of a quiet region with Hinode SOT coodinated with XRT and EIS.