2007-12-27T23:11:06.000Z 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 SAKAO, Taro SUEMATSU, Yoshinori SAKAO, Taro 53 0 null Helioseismology HOP15 QS, XBP QR 0 -15.3 -0.1 0 0 2007-12-24T19:59:54.000Z 2007-12-25T08:14:54.000Z -15.3 -0.1 CORE: SOT continuous magnetic field observations for investigating mechanisms responsible for XBPs and QS dynamics HOP15 Daily Note: HOP15, SOT synoptic observation and EIS calibration will be performed rather than HOP53 XRT * Collaborative observations with SOLIS during EIS sensitivity monitoring, 1600-2000UT, with start during radiation-free time (or, no more than 6 minutes before radiation-free). [XRT-CO, use SSQ 006C] * Continue flare detection mode. * Support HOP 53 (QS and XBP), if no ARs are present on the disk. EIS * Sensitivity monitoring (3.5hr) * Quiet region near disk center (including HOP53) Continuous tracking for a few days is preferred. SOT * HOP15: Helioseismology observations with SOT (if solar activity is low) - lat = 30 degrees for 12 hours (cancel of one synoptic observation) requires cancel of synoptic observation for 12 hours continuous observation * One 30-minute synoptic obs for NFI test * 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.