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\@writefile{toc}{\contentsline {section}{INTRODUCTION}{1}}
\@writefile{toc}{\contentsline {section}{Teams involved}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces \em  Schematic drawing of BS spectrometer and the scheme of so-called dopplerometer section. The key numbers have the following meaning: 1\nobreakspace  {}-\nobreakspace  {} strain gauge doubly compensated angle readout sensor, 2\nobreakspace  {}-\nobreakspace  {}scanning collimator (10\nobreakspace  {}arc sec FWHM) mounted on the moving arm, 3\nobreakspace  {}-\nobreakspace  {}rotating Archimedean cam moving the arm, 4\nobreakspace  {}-\nobreakspace  {}stepper motor and reduction gear, 5\nobreakspace  {}-\nobreakspace  {}double proportional counters, 6\nobreakspace  {}-\nobreakspace  {}four crystals with two of them organized as Dopplerometer, 7\nobreakspace  {}-\nobreakspace  {}microprocessor controller, 8\nobreakspace  {}-\nobreakspace  {}pre-amplifiers and HV power supply. As concerns the Dopplerometer, the situation is shown (left panel) when the bisector plane of the pair of identical crystals points towards the source (flare). Therefore, the Bragg condition for the chosen Ca\nobreakspace  {}{\sc  XIX}\nobreakspace  {}{\em  w} line is fulfilled at the same time for both crystals. Provided the lines are Doppler-shifted, the maxima of lines will not coincide in time and precise estimates of plasma radial velocities can be made. }}{2}}
\@writefile{toc}{\contentsline {section}{DIOGENESS Description}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces \em  A sample of the flare spectrum to be observed within the Dopplerometer section of BS. The numbers above the stronger spectral features correspond to the following transitions: 3\nobreakspace  {}-\nobreakspace  {}{\rm  Ar\nobreakspace  {}XVIII} $1s\,^2{\rm  S}_{1/2}$ - $4p\,^2{\rm  P}_{1/2,3/2}$; 4\nobreakspace  {}-\nobreakspace  {}{\rm  Fe\nobreakspace  {}XXV} $1s\,^1{\rm  S}$ - $1s4p\,^1{\rm  P}$ (2nd order); 5\nobreakspace  {}-\nobreakspace  {}{\rm  K\nobreakspace  {}XVIII} $1s\,^1{\rm  S}_{\rm  0}$ - $1s3p\,^1{\rm  P}_{\rm  1}$; 6\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XX} $1s\,^2{\rm  S}_{\rm  1/2}$ - $2p\,^2{\rm  P}_{\rm  3/2}$ (Ly$_{\alpha _{1}}$); 7\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XX} $1s\,^2{\rm  S}_{\rm  1/2}$ - $2p\,^2{\rm  P}_{\rm  1/2}$ (Ly$_{\alpha _{2}}$); 8\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XIX} $1s2p\,^1{\rm  P}_{\rm  1}$ - $2p^2\,^1{\rm  D}_{\rm  2}$ (J-satellite); 11\nobreakspace  {}-\nobreakspace  {}{\rm  Ar\nobreakspace  {}XVIII} $1s\,^2{\rm  S}_{1/2}$ - $3p\,^2{\rm  P}_{1/2,3/2}$; 12\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XIX} $1s^2\,^1{\rm  S}_{\rm  0}$ - $1s2p\,^1{\rm  P}_{\rm  1}$ ({\em  w}); 19\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XVIII} $1s^22p\,^2{\rm  P}_{\rm  1/2}$ - $1s2p^2\,^2{\rm  D}_{\rm  3/2}$ ({\em  k} -satellite); 21\nobreakspace  {}-\nobreakspace  {}{\rm  Ca\nobreakspace  {}XIX} $1s^2\,^1{\rm  S}_{\rm  0}$ - $1s2s\,^3{\rm  S}_{\rm  1}$ ({\em  z}). The Figure has been compiled based on spectral measurements made from NRL P-78 satellite in 1979.}}{4}}
\@writefile{toc}{\contentsline {section}{RESIK Description}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces \em  The wavelength coverage of individual bands of DIOGENESS (upper dot--limited bars) and RESIK (lower bars) at the first second and third orders of reflection. The background spectrum is one of the few available covering the entire range.}}{6}}
\@writefile{toc}{\contentsline {section}{Conclusions}{6}}
\@writefile{toc}{\contentsline {section}{ACKNOWLEDGMENTS}{6}}