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\@writefile{toc}{\contentsline {section}{\numberline {1.}EARLY SOUNDING ROCKET EXPERIMENTS}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces \em  Solar images obtained using pin-hole cameras during the flight of Vertical-1 sounding rocket on 28 November 1970. The Be\nobreakspace  {}50\,$\mu $ and Al\nobreakspace  {}6\,$\mu $ filter images represent emissions from the hotter and cooler plasma. The ''filetr ratio'' technique allowed to determine the temperature structure within individual active regions. The spatial resolution in the images is rather low (1\nobreakspace  {}arcmin), typical for pin-hole technique. }}{1}}
\newlabel{fig:fig1}{{1}{1}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces  Solar Physics Division Launches. }}{2}}
\@writefile{toc}{\contentsline {section}{\numberline {2.}NEW CONCEPTS}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces \em  Left: X-ray spectra of the wavelength region covering a part of so-called Mg{\sc  xi} triplet including (partly) the resonance (R), intercombination (I) and forbidden (F) line complexes. There were no collimator within the spectrometer flown aboard the Vertical-9 rocket. Therefore each active region present on the disk contributed (in projection on the scan direction) to the individual line component as is shown in the right panel. The image shown has been obtained using grazing incidence telescope RTF equipped with Be\nobreakspace  {}50\,$\mu $ filter. The Volter type II mirror used in RTF has been fabricated at the Astronomical Observatory Ondrejov, Czech Republic. }}{2}}
\newlabel{fig:fig2}{{2}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces \em  Left: A scheme of one section of the X-ray Dopplerometer. The crystals are mounted on a common shaft with the crystal planes aligned exactly at the angle $2 \Theta $. Upper right: A scheme of the spectral pattern to be recorded by the Dopplerometer in case of the source plasma being at rest. Note that wavelength scannig is performed in opposite directions in both detectors. Lower right: Spectral pattern for the source moving in the direction towards the observer. }}{2}}
\newlabel{fig:fig3}{{3}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces \em  The Rocket Dopplerometer RDR flown aboard Vertical-11 sounding rocked on 20 October 1983. The main components of the instrument are as follows: {\fam \bffam \ninebf 1}\nobreakspace  {}-\nobreakspace  {}electronic box, {\fam \bffam \ninebf 2, 3}\nobreakspace  {}-\nobreakspace  {} Geiger counters placed behind the rotaionally modulated collimator ({\fam \bffam \ninebf 4}) and scanning collimator ({\fam \bffam \ninebf 5}). Part of the crystal within the Dopplerometer section is seen ({\fam \bffam \ninebf 6}). The scanning multigrid X-ray collimator ($\sim 10$\nobreakspace  {}arcsec resolution) is fixed to the driving shaft of the Dopplerometer and precisely aligned with the bisectrix between the crystal plane. }}{3}}
\newlabel{fig:fig4}{{4}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces \em  Left: X-ray scans across the solar disk obtained from the multigrid collimator (top) and spectra in vicinity of Mg\nobreakspace  {}{\sc  xi} resonance line from two sections of the Dopplerometer. On the horizontal axis the time in minutes elapsed from 04:00 UT is plotted while on the vertical axis the count rate of the appropriate detector is indicated. Right: Detailed Mg\nobreakspace  {}{\sc  xi} resonance line profile (thick line, bottom panel) superimposed on the brightness profile of the sources taken in the plane of dispersion (thin line). In the upper panel, the RTF image of the corresponding pattern of X-ray radiation is shown. Two strongest active regions located on the eastern and western limb contribute to the emission observed in the Mg\nobreakspace  {}{\sc  xi} resonance line. The western (lowest) active region becomes flaring during the period covered by the observations. }}{4}}
\newlabel{fig:fig5}{{5}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {3.}THE SATELLITE EXPERIMENTS}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces \em  Six simultaneous Mg\nobreakspace  {}XI line profiles (thick forward, broken backward). They were recorded around 73, 142, 234, 302, 396 and 461 s during the flight on 20 October 1983. Spectra have been obtained using ADP crystal (2d = 10.64 \r A). It is seen, that the spectral line separation increases with time. Dotted line represents reference profile of the source brightness as recorded using 10\nobreakspace  {}arcsec slit collimator. Verical axis represents count rates and horizontal time in seconds. }}{4}}
\newlabel{fig:fig7x}{{6}{4}}