UVCS MISSION LOG
				----------------

	Date:		19 January 2003
	-----

 	Last revision:	21 January 2003 (Wu)
	--------------

	File Name: 	2003.01.19.a.log
	-----------

	Compiled by:	Y.-K. Ko
	------------

	UVCS Activity:	Load Coronal Plasma Compressibility (Coronal Hole) 
	--------------  Observation for 19 - 20 January 2003
                        Load Mini-Synoptic for 20 January 2003
                        Coronal Plasma Compressibility (Coronal Hole)
                        Observation for 20 January 2003
                        Load Synoptic for 20 - 21 January 2003

	SOHO Activity: 
	--------------

	EOF Staff:	X. Li: Lead Scientist
	----------	Y.-K. Ko: Commander, Planner
			M. Uzzo
                        R. Wu

	Command file:	03.01.19.16:46:57.cmd.log

	Activity:
	---------

        1) Coronal Plasma Compressibility (Coronal Hole) Observation

        Sequence: 03.01_Li_CH2.tcl

        SCI_SPEC: The coronal hole study is to investigate the solar wind 
                  outflow and temperatures above coronal holes as the solar 
                  activity is declining. The goal of the study is to 
                  investigate characteristics of the solar wind plasma in 
                  such a phase.  Since current coronal holes are not clean, 
                  the observation will also allow the determination of outflow 
                  speed and ion temperatures of denser channels hidden in 
                  coronal hole structures.

	OBS_PROG: Primary: Spatial Coverage
		  Sub Obj: Spectral Resolution

	SCI_OBJ:  Coronal Dynamics...Outflow Velocities
                  Plasma Properties...Ion Temperatures

	OBJ:      Coronal Hole

	CMP_NAME: Coronal Plasma Compressibility (UVCS/LASCO)

	CMP_NUM:  6919

	Duration: start: 2003.01.19.17:22
                    end: 2003.01.20.00:44

	ONUMs =	18467 (83 exps)

	Instrument configuration:

		- Pointing:  Sun center

		- Roll: 165 Degrees (48820)
 
		- Mirror/Occulter:  1.6, 1.9 Ro
                                    1.5 mm overocculting

		- LYA Slit:    50 um
		- OVI Slit:    50 um 

		- LYA GRTPOS: 128000
		- OVI GRTPOS: 170300

		- LYA mask:   LYA_93_1sec   in slot 2
		- OVI mask:   OVI_170300MPM in slot 5

	Fits Files:

q03.01.19.17:03:45.lya.dat
q03.01.19.17:03:45.ovi.dat
q03.01.19.17:03:45.vld.dat

GAP between 01/19/03|23:54:21( 6071) and 01/19/03|23:56:36( 6289)

	2) Mini-Synoptic Sequence Load and Start

	Sequence: SynopticA:Mini

	SCI_SPEC: Synoptic studies.  LYA HV off / OVI voltage at 210,
		  LYA grating position now at 128000 "permanently".

	OBS_PROG: Synoptic

	SCI_OBJ:  Synoptic

	OBJ:      Entire Corona

	CMP_NAME:

	CMP_NUM:

	Duration: start: 2003.01.20.01:11
		    end: 2003.01.20.04:38

	ONUMs = 41073 (9 exps) 
		41074 (9 exps) 
		41075 (9 exps) 
		41076 (9 exps) 
		41077 (9 exps) 
		41078 (9 exps) 
		41079 (9 exps) 
		41080 (9 exps) 

	Instrument configuration:

		- Pointing:  Sun center

		- Roll: W, NW, N, NE, E, SE, S, SW

		- Mirror/Occulter: 1.6, 1.75 Ro
 				   1.5 mm overocculting (1.6 Ro)
				   2.0 mm overocculting (1.75 Ro)

		- LYA Slits:   50 um
		- OVI Slits:  150 um

		- LYA GRTPOS: 128000
		- OVI GRTPOS: 194372

		- LYA mask:   LYA_93_1sec    in slot 2
		- OVI mask:   OVI_Syn_194372 in slot 2

	Fits Files:

z03.01.20.01:10:31.lya.dat
z03.01.20.01:10:31.ovi.dat
z03.01.20.01:10:31.vld.dat
z03.01.20.01:37:05.lya.dat
z03.01.20.01:37:05.ovi.dat
z03.01.20.01:37:05.vld.dat
z03.01.20.02:03:34.lya.dat
z03.01.20.02:03:34.ovi.dat
z03.01.20.02:03:34.vld.dat
z03.01.20.02:30:03.lya.dat
z03.01.20.02:30:03.ovi.dat
z03.01.20.02:30:03.vld.dat
z03.01.20.02:56:32.lya.dat
z03.01.20.02:56:32.ovi.dat
z03.01.20.02:56:32.vld.dat
z03.01.20.03:23:09.lya.dat
z03.01.20.03:23:09.ovi.dat
z03.01.20.03:23:09.vld.dat
z03.01.20.03:49:44.lya.dat
z03.01.20.03:49:44.ovi.dat
z03.01.20.03:49:44.vld.dat
z03.01.20.04:16:11.lya.dat
z03.01.20.04:16:11.ovi.dat
z03.01.20.04:16:11.vld.dat

        3) Coronal Plasma Compressibility (Coronal Hole) Observation

        Sequence: 03.01_Li_CH3.tcl

        SCI_SPEC: The coronal hole study is to investigate the solar wind 
                  outflow and temperatures above coronal holes as the solar 
                  activity is declining. The goal of the study is to 
                  investigate characteristics of the solar wind plasma in 
                  such a phase.  Since current coronal holes are not clean, 
                  the observation will also allow the determination of outflow 
                  speed and ion temperatures of denser channels hidden in 
                  coronal hole structures.

	OBS_PROG: Primary: Spatial Coverage
		  Sub Obj: Spectral Resolution

	SCI_OBJ:  Coronal Dynamics...Outflow Velocities
                  Plasma Properties...Ion Temperatures

	OBJ:      Coronal Hole

	CMP_NAME: Coronal Plasma Compressibility (UVCS/LASCO)

	CMP_NUM:  6919

	Duration: start: 2003.01.20.04:46
                    end: 2003.01.20.17:22

	ONUMs =	18468 (74 exps)

	Instrument configuration:

		- Pointing:  Sun center

		- Roll: 165 Degrees (48820)
 
		- Mirror/Occulter:  2.1 Ro
                                    1.5 mm overocculting

		- LYA Slit:    50 um
		- OVI Slit:    50 um 

		- LYA GRTPOS: 128000
		- OVI GRTPOS: 170300

		- LYA mask:   LYA_93_1sec   in slot 2
		- OVI mask:   OVI_170300MPM in slot 5

	Fits Files:

q03.01.20.04:38:57.lya.dat
q03.01.20.04:38:57.ovi.dat
q03.01.20.04:38:57.vld.dat