In the display above (click to enlarge), the solar X-ray fluence seen by RESIK (black points)  is plotted atop GOES red line. Only periods with good spectral measurements are indicated. The total number of good spectral measurements is given in the title line.

New mode:	Tests of the '3rd order reflections' (ORD3) operating  mode have been performed (on Nov 19 03:30:00 UT)  with full success. We have new 'standard' mode 'ORD3' from 20 Nov 17:00:00 UT .  The settings are below.
Calibrations made:	No calibrations  made
ADS Settings:	HV: Det. A - 1450 V, Det. B - 1389 V.  ADS  are  below.
	Channel		l Band	ADS
	#1	#2	3.37 - 3.88 Å : 35 -   85
	#2	#0	3.82 - 4.33 Å : 70 - 120
	#3	#3	4.31 - 4.89 Å : 55 - 110
	#4	#1	4.96 - 6.09 Å : 90 - 160
			software indexes
		spectroscopic notation (papers)

 
                    
Data gaps due to missing telemetry: ~10 hours.

Examples of Well-observed Events:

 03 August 2002, 19:07 UT

For this time we have selected short duration limb flare of GOES class X. The event has been observed by RESIK in dynamic DGI operation mode.

 

	Date:	03 August 2002
	Start, Max, End [UT]:	18:59:00, 19:07:00, 19:11:00
	GOES Importance:	X1.0
	Duration:	~12 min.
	Ha Class:	SF
	NOAA AR association:	9893
	Location (EIT):	S16 W87

Below, the specta integrated over characteristic phases of this flare evolution are presented.

The spectra integrated over the flare rise phase (19.0 UT-10.1 UT).

The spectra integrated over the flare maximum (19.10 UT-19.15 UT).

The spectra integrated over the early decay (19.15 UT-19.25 UT).

The spectra integrated over the late decay (19.25 UT-19.35 UT).

As the flare evolves the relative intensity ratios of the line observed in individual channels are changing. Some peculiarities can be noted which make this flare distinguishable from other events.

 In #1 the He-like K XVIII ion triplet (bins  80-100) and the Ly-a line (uresolved spin doublet) due to H-like  Ar XVIII (bin no. ~170) are evident even during the decay.
In #2 the most prominent feature is He-like Ar XVII triplet (320-350 bins). The relative ratio of resonance and forbidden line intensities does not become reversed during the late decay as is usually observed when plasma is cool enough. All these indicate for existing some amount of the hot plasma at that time. Around the bin no. 390 the S XV line corresponding to the transition 1s²- 1s4p is also present over this time. As concerns #3 the most intense is the Ly-a doublet of S XVI ion (bin no. ~675). The intensity of this line in comparison with near by continuum changes during the flare evolution very much. The most evident changes of relative intensities in #4 occur for the resonance line of S XV (~bin no. 790) and Si XIII 1s²-1s3p transition (at ~910 bin no.).

(The spectra taken at the flare maximum are severly   distorted due to detector's A saturation, so #1 and #3 can not be used to the analysis during that time.)

 Report prepared by: Barbara Sylwester bs@cbk.pan.wroc.pl

The report presented  has been done in "real time" and so it may contain jargon, blunders, or trivialities. We do not have also an English native speaker in our Wroclaw group! We would be happy to discuss problems mentioned above in more details  if necessary.
RESIK data are in the open public domain and can be requested from: http://surfwww.mssl.ucl.ac.uk/surf/data_request.html.

Previous RESIK_weekly notes are in the archive:
http://www.cbk.pan.wroc.pl/resik_archive.htm

Page made on 28November 2002 by: Jarek Bakala jb@cbk.pan.wroc.pl