CORONAS

CORONAS-F Tracking

DIOGENESS

X-Ray Spectrometer and Photometer

Institutions:
Space Research Centre, Polish Academy of Sciences, Wroclaw, Poland
Astronomical Institute of the Check Republic
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Troitsk, Russia.

Principal Investigators:
Z.Kordylevsky, J. Sylwester

Scientific goals

Study of the X-Ray emission from the solar active regions and flares. Measurements of temperature, element composition and radial velocities of the solar hot coronal plasma. Localization of the solar sources of X-Ray emission and study of their structure.

Technical parameters

Spectrometry

The observations are carried out in four separate channels

Channel 1 2 3 4
Crystal Quartz ADP Beryl Quartz
Plane 1011 101 1010 1011
2d1 6.6855 10.5657 15.9585 6.6875
lobs 3.1779 5.0348 6.6492 3.1779
ltheor 3.1781 5.0374 6.6488 3.1781
Line Ca XIX w S XV w Si XIII w CaXIX w
lmin 3.1436 4.9807 6.1126 2.9601
lmax 3.3915 5.3721 6.7335 3.2123
RC [mrd] 91 91 15 90
FWHM [arcsec] 24.1 68.1 94.1 25.6

Scan time of each spectrum: 120 seconds
Accumulation time of a single spectrum point: 0.4 - 0.6 - 0.8 seconds
(The accumulation time of a single spectrum point and the resulting number of measurement points in a spectrum for each scan is determined automatically using the maximum level of the previous spectrum).

Photometry

Energy interval: 2-4 and 4-8 keV
Detector apertures: 0.3 and 0.01 cm²

Duration of single measurement:	2 seconds for low solar activity
	0.125 econds during solar flare

Structure and localization of an X-Ray source

Energy interval: 2-4 and 4-8 keV
Spatial resolution (FWHM): 10 arc seconds
Scan speed: one arc minute per second

Contact address

More detailed information, data access policy and cooperation opportunities can be obtained at this location:

Last modified: Feb 08 2003 17:29 MSK
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