Hida/DST & SoHO CDS, EIT, MDI coordinated observation
2004 October 18-23th

Abstract (from http://sohowww.nascom.nasa.gov/soc/JOPs/jop179.txt) JOP179 Energy Propagation in XBPs Received 29 July 2004 (draft) Modified 27 September 2004 (by SOC) Scientists and institutes: Tetsuya Watanabe (NAOJ, PI) Kuniko Hori (NICT) Satoru UeNo (Hida, Kyoto U.) Reizaburo Kitai (Hida, Kyoto U.) Participating instruments: SoHO CDS EIT (MDI) DST (Hida Observatory, Kyoto U.) Scientific Objective: Simultaneous spectroscopic observations of chromospheric, transition-region, and low T coronal lines of XBPs, one of the simplest magnetic elements apprearing on the solar disk will be conducted to understand the energy propagation in an XBP from upper photosphere to corona. Reasonbly high enough cadence should be taken so that both internsity and line-of-sight velocity changes could be measured along with time. Target: XBPs apprearing on the solar disk during the period Observing Sequences: 18 October to 23 October : Before 21 UT: identifying and targeting XBPs (using the most recent EIT images) Observations: 21 UT - 3 UT (+ 1 day)* DST: CaII K line sepctral observation (slit width 1 arcsec x length 128 arcsec , sp range: 3925-3945A, rastering a few arcsec) CDS: Reasonably high cadence observation with a FOV stuck to XBPs. EIT: 195A CME Watch MDI: Full Disk Mags and Doppler, 1 minute cadence when possible * A part of CDS daily synoptic observation during 0-3 UT might conflict.
Link (1) The CDS Atlas for October 2004 (2) The most recent CDS images received at the SOHO operations facility located in the Goddard Space Flight Center