Hida/DST, Norikura & SoHO CDS, EIT, MDI coordinated observation
2005 October 17-21th


Abstract 

TITLE: JOP 179 - ENERGY PROPAGATION IN XBPs 

PARTICIPATING INSTRUMENTS: SoHO CDS EIT (MDI), DST (Hida Observatory, Kyoto U.) & Norikura (NAOJ)

DATES: October 17 - 21, 2005 (21:00 - 06:00 UT) 

WHO: Tetsuya Watanabe, Kuniko Hori, Satoru UeNo 

ACTIVITY: .
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 appearing on the solar disk during the period. The target will be selected 
by CDS, with pointing sent to Goddard and Japan by 16:00 UT at the latest. 
The target line of the DST/vertical spectorometer is the CaII K absorption line. 

STUDIES TO RUN: (TBC) XBP_TW1/v4 (duration 10min); XBP_TW2/v13 (duration 4min)

SEQUENCE(CDS): A different study should be run depending on the size of the bright point. 
XBP_TW1 covers an area of 40x120 arcsec^2 and XBP_TW2 covers an area of 20x100 arcsec^2. 
The bright point should fit entirely within the raster field-of-view. 
SEQUENCE(DST): DST covers areas of 40x128 arcsec^2 or 60x128 arcsec^2 whose centers 
correspond to the center of the CDS raster FOV.
The scan step is 2 arcsec. The slit width corresponds to 1.28 arcsec.
The required time for one raster-scan is 100 sec (40x128arcsec^2) or 150 sec
(60x128arcsec^2).

NOTES FOR PLANNER: each raster should be corrected for solar rotation. The planner 
needs to request that the operator run the study with the MIRROR option in CPT. 

DURATION: several hours 


Link

(1) The CDS Atlas for October 2005
(2) CDS Catalog
  *2005.10.18-19
  *2005.10.19-20
  *2005.10.20-21
(3) Hida/DST H-alpha Monitor Images