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