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\@writefile{toc}{\contentsline {section}{\numberline {1}Introduction}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  {\bf  Left:} Professor Jan Mergentaler (1901--1995), while in charge of the Astronomical Institute of the Wroc{\l }aw University, decided in late 60-ties to take the political opportunity and set-up a group of people designing the first Polish space experiment: the solar XUV spectrometer and X-ray pinhole camera.\newline  {\bf  Middle:} Solar images obtained using pin-hole cameras during the flight of \emph  {Vertical-1} sounding rocket on 28 November 1970. \newline  {\bf  Right}: Dr. Zbigniew Kordylewski designer of the instrument unveils the hardware after the first successful flight which took place on 28\nobreakspace  {}November\nobreakspace  {}1970 aboard the Vertical-1 sounding rocket launched from Kapustin Yar (South of Russia).  }}{1}}
\newlabel{fig:MergKord1}{{1}{1}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces Solar Physics Division Launches}}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  {\bf  Left:} The grazing-incidence Volter type-II solar telescope assembly. The mirror was designed by the Czech group from Ondrejov Astronomical Institute. The mechanical part including the shutter has been developed in Wroc{\l }aw. The instrument has been included aboard the \emph  {Vertical-8} and \emph  {-9} payloads flown in 1979 and 1980 respectively.\newline  {\bf  Centre:} An example of experimental results showing digitized X-ray image of the corona obtained in the spectral range 8\nobreakspace  {}\r A\nobreakspace  {}-\nobreakspace  {}12\nobreakspace  {}\r A\ (upper part) together with the corresponding brightness cut as seen in the resonance line of {\rm  Mg}\nobreakspace  {}{\sc  \nobreakspace  {}xi} ion recorded with the scanning Bragg crystal spectrometer MRF.\newline  {\bf  Right:} Photo of the MRF Bragg, scanning, flat ADP crystal spectrometer (designed by M. H{\l }ond), a part of the Polish instrument packages aboard \emph  {Vertical-8} and \emph  {-9} payloads.  }}{3}}
\newlabel{fig:Vert2}{{2}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {2}RF15-I Photometer-Imager}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  {\bf  Left:} General appearance of the RF15-I soft X-ray Photometer-Imager with the instrument cover removed. The box which contains both the photometer and the imager is placed atop the solar oriented platform of the \emph  {INTERBALL-Tail}.\newline  {\bf  Centre-left:} The rotationally modulated collimator of a novel design, where the three wired grid planes replace five of the standard design, were sufficient to achieve $\sim $10\nobreakspace  {}črcsec angular resolution on the reconstructed image. As shown on the insert, the modullation pattern is present during only a half of the rotation which allows to study the intrinsic solar flux time variability with the resolution of \nobreakspace  {}0.01\nobreakspace  {}s.\newline  {\bf  Centre-right:} The example of the time record of the modulated signal measured on 1995 October 20 around 06:14\nobreakspace  {}UT, when the M1 class flare reached the maximum phase. The time indicated is in [s] elapsed from the beginning of the flare sequence. The spin period of the Sun-pointed satellite was $\sim $120\nobreakspace  {}s. The bottom part shows a part of the record enlarged in order to see the details.\newline  {\bf  Right:} Numerically reconstructed image of the flare showing the overall shape of the active region plasma contributing to the 2\nobreakspace  {}keV\nobreakspace  {}-\nobreakspace  {}4\nobreakspace  {}keV emission. The grid mesh is drawn 50\nobreakspace  {}ačrcsec apart.  }}{4}}
\newlabel{fig:RF3}{{3}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces  {\bf  Left:} The SS-14 Cyclon booster which put the CORONAS-F solar mission on the circular, semi-Sun-synchronous polar 500\nobreakspace  {}km orbit on 31 June 2001.\newline  {\bf  Centre:} The payload consisted of a dozen of solar instruments, including two Polish Bragg spectrometers: flat crystal, scanning {\bf  Diogeness} and bent crystal {\bf  RESIK}.\newline  {\bf  Right:} The background particle environment at the CORONAS-F orbital heights as recorder by RESIK own PIN particle detectors. The SAA region as well as the polar ovals are clearly seen. In these high background areas, the spectrometers' proportional detectors were switched-OFF due to health reasons.  }}{5}}
\newlabel{fig:COR4 }{{4}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {3}Diogeness and RESIK aboard CORONAS-F}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces  {\bf  Left:} Overall view of {\bf  Diogeness} scanning spectrometer. The four Bragg crystals are seen fixed to the moving arm which rocks within the range of $\sim $140\nobreakspace  {}arcmin relative to the line pointing to the Sun centre.\newline  {\bf  Centre:} The scheme of Dopplerometer configuration adopted in the experiment. Bi-sector plane of the crystal pair \#1 and \#4 (dotted line) points momentarily towards the source (flare). Crystals are fixed mechanically at the exactly twice the Bragg angle. By rocking the fixed crystal section back and forward, the Bragg-reflected spectra in the vicinity of strong lines are measured by a pair of double proportional counters. In the ideal case of perfect co-alignment and for the source plasma being at rest, the line centres are recorded in channels \#1 and \#4 at the very same time during the scans performed in the opposite wavelength sense (upper right panels). Any radial motions of the hot flaring plasma will displace (in time) the relative position of lines (lower panel). The displacement is proportional to the line Doppler shift and is independent of the position of the source (flare) on the disc and/or the relative pointing, provided they are stable.\newline  {\bf  Right:} In the upper part an example of measured spectra recorded nearly simultaneously in Dopplerometer channels \#1 and \#4 during the maximum phase of the X5.3 flare is shown plotted against the motor step number. Indicated are the times, when the centre of the strongest resonance line is measured. In the lower part, velocities as determined from X-ray line shifts observed by Diogeness are drawn. A high blue-shifts observed early in flare are of similar value in all lines measured. The uncertainties shown represent combined relative error of wavelength scale determination. For {\rm  Ca}\nobreakspace  {}${\sc  \nobreakspace  {}xix}$\nobreakspace  {}\emph  {w} line the uncertainties of velocity determinations (around the flare maximum phase) are few km/s only.  }}{6}}
\newlabel{fig:Diog5 }{{5}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces  {\bf  Left:} Overall view of the RESIK spectrometers A and B with the back cover removed in order to show the bent crystal supports. The code-names for channels are indicated.\newline  {\bf  Right:} Example reduced RESIK spectrum showing main prominent emission lines atop the X-ray continuum. The ions responsible for the line emission are indicated. The spectrum shown has been collected during the 20-minute rise phase of the M1.9 East-limb flare on 2003 January 21.  }}{7}}
\newlabel{fig:Diog6 }{{6}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces  {\bf  Upper:} A header of one (among thousand) page from the RESIK catalogue showing a well observed flare. The X-ray lightcurves are plotted in red and blue for the GOES and in green for RESIK. Shaded areas correspond to transitions through radiation belts and/or SAA. Hatched areas correspond to spacecraft nights. Color bars correspond to flares which locations are shown on the solar disc in respective colors. The size of the color dot correspond to the flare importance. \newline  {\bf  Middle left:} Pre-flare spectrum recorded several hours before the considered event. The thin line drawn corresponds to the continuum level calculated for the indicated values of temperature and emission measure. \newline  {\bf  Middle right:} Spectrum recorded during the rise phase of flare. The plasma temperature is much higher and many emission lines are seen above the continuum in the spectral range below 5\nobreakspace  {}\r A.\newline  {\bf  Lower left:} Average spectrum showing the spectral region in vicinity of the so-called He-like triplet of {\rm  K}\nobreakspace  {}{\sc  \nobreakspace  {}xviii} ion. This is the first observation of this spectral region with such a gigh spectral resolution.\newline  {\bf  Lower right:} A comparison between the observed (points) and theoretically calculated temperature dependence of the line emissivity in the resonance line of {\rm  K}\nobreakspace  {}{\sc  \nobreakspace  {}xviii} ion. A close match is seen if the theory line is drawn using the potassium abundance of 6.00\,x\,10$^{-7}$, four times the photospheric one.  }}{8}}
\newlabel{fig:Jan7 }{{7}{8}}
\@writefile{toc}{\contentsline {section}{\numberline {4}Summary}{8}}
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