TESIS on CORONAS-PHOTON S. V. Kuzin (XRAS) and TESIS Team

TESIS: scientific tasks Scientific tasks:  Investigation of the most dynamic processes in the solar atmosphere, such as flares, coronal mass ejections, dimmings etc.  Investigation of processes in far solar corona (up to 4 solar radii) in EUV  Study of evolution of large-scale long-life coronal structures: active regions, coronal loops, giant arcades, coronal holes and others.  Determination of the physical parameters (electron temperature and density, differential emission measure) of plasma of coronal structures.

TESIS: targets of observations Targets of observations:  Solar flares – their dynamics, energy balance and physical characteristics  Eruptive processes in the solar atmosphere – triggers and methods of forecasting  Coronal mass ejections – their formation and dynamics  Spectroscopy of coronal plasma in wide temperature range  Investigation of upper Earth atmosphere

TESIS INSTRUMENT OVERVIEW ChannelAimsDescriptionWave- length band Field of view Angular resolution MgXII Imaging Spectro- heliometer (MISH) 10 MK plasma: dynamics, parameters Soft X-ray full-disk Bragg spectroheliometer with spherical bent crystal mirror MgXII A and A doublet 1°.15 (Full solar disk) 2 arc sec / pixel EUV Spectro- heliometer (EUSH) From “cold” to “hot” plasma: parameters by means of imaging spectroscopy EUV full-disk spectroheliometer with grazing incidence diffraction grating and focusing multilayer parabolic mirror A1°.24 (Full solar disk compressed along dispersion) 4.4 arc sec (perpendicular to dispersion) 1.5 arc min (along dispersion) Full-disk EUV Telescopes (FET) High resolution and high cadence images of 0.05 MK and 15 MK plasma Herschelian telescopes with multilayer parabolic mirrors A (telescope I) A (telescope II) 1°.0 (Full solar disk) 1.7 arc sec / pixel Solar EUV Coronograph (SEC) CME structure and dynamics up to 4 solar radii Coronograph based on the Ritchey- Chretien scheme A2°.5 (inner and outer corona from 0.7 to 4 solar radii) 5 arc sec / pixel

METHODS OF TESIS OBSERVATIONS HeII 304 A MgXII 8.42 A FeXX 132 A EUV A TESIS will provide simultaneous imaging of the Sun in 4 spectral channels, including EUV channel A, which allows to derive the density and the temperature composition of the plasma.  Multi-wavelength simultaneous observations of full Sun in 4 spectral channels

 Bragg angle………………………………… 82°.08  Wavelength band…… ………. MgXII A and A doublet  Focal length…………………………… mm  Mirror Aperture………………………71× 103 mm  Field of view ……..………………………….. 1°.15  Angular resolution……………….……. 2 arc sec  Cadence…….………….. up to 1 s (partial frame) 10 sec (full frame)  Image detector….…………..… backside CCD of 2048 × 2048 pixels  CCD pixel size …………………… μ × 13.5 μ MgXII IMAGING SPECTROHELIOMETER overview

MgXII IMAGING SPECTROHELIOMETER CCD detector Back-side 2048x2048 pixel 13.5x13.5 mkm 14 bit ADC Noise - 6e/sec (0  C)

MgXII IMAGING SPECTROHELIOMETER temperature response

 Wavelength band….… – 136 A (telescope I) 290 – 320 A (telescope II)  Focal length……………………………… mm  Mirror Aperture…………………. 100 mm diameter  Field of view ……..……………………………... 1°.0  Angular resolution…………………..…. 1.7 arc sec  Cadence…….…………………1 sec (partial frame) 60 sec (full frame)  Image detector….…………….… backside CCD of 2048 × 2048 pixels  CCD pixel size ………………..…… μ × 13.5 μ FULL-DISK EUV TELESCOPES overview

 Wavelength band….… – 136 A (telescope I) 290 – 320 A (telescope II)  Focal length……………………………… mm  Mirror Aperture…………………. 100 mm diameter  Field of view ……..……………………………... 1°.0  Angular resolution…………………..…. 1.7 arc sec  Cadence…….…………………1 sec (partial frame) 60 sec (full frame)  Image detector….…………….… backside CCD of 2048 × 2048 pixels  CCD pixel size ………………..…… μ × 13.5 μ FULL-DISK EUV TELESCOPES overview

FULL-DISK EUV TELESCOPES temperature response Fe XX (132 A)  T min = 5 × 10 6 K  T max = 1.2 × 10 7 K MgXII channel  T min ………… about 4 × 10 6 K  T max ……………….…… K

 Wavelength band…… ……….…. 280 – 330 A  Ions…..……HeII, SiIX, SiXI, FeXIV-FeXVI, MgVIII, NiXVIII, CaXVII, AlIX, FeXXII and others  Focal length………………………………. 600 mm  Entrance Aperture………………………5× 80 mm  Field of view ……..………………………….. 1°.24 ( Full solar disk compressed along dispersion )  Angular resolution………………..…. 4.4 arc sec  Cadence…….……………………….. 30 – 600 sec  Image detector….…………..… backside CCD of 1024 × 2048 pixels  CCD pixel size …………………… μ × 13.5 μ EUV SPECTROHELIOMETER overview

EUV SPECTROHELIOMETER targets of observations  Spectral diagnostic of solar active regions

SOLAR EUV CORONOGRAPH  Wavelength band……………….………290 – 320 A  Focal length……………………………..…. 600 mm  Mirror aperture…ring of 25 and 85 mm diameters  Field of view ……..……………………………... 2°.5 ( inner and outer corona from 0.7 to 4 solar radii )  Angular resolution…………………….…. 5 arc sec  Temporal resolution…………………..…… 600 sec  Image detector….…………….… backside CCD of 2048 × 2048 pixels  CCD pixel size ………………..…… μ × 13.5 μ

SOLAR EUV CORONOGRAPH

TESIS DAILY DATA TESIS may provide JPEG images (512×512 ) TESIS daily telemetry ~0,5 Gb 250 full FITS files (2048×2048) 1000 Binned FITS files (1024×1024) ~1 hour of movies (10 frames in sec)

TESIS INSTRUMENT  TESIS 6 independent channels (including SPHINX) 2 star trackers 500 MB information per day Full Sun and corona up to 4 solar radii Spatial resolution up to 1.7   OPTICS: large aperture ML normal incidence mirror – new types of high reflective coating Quartz large aperture high quality mirror ML filters  DETECTORS 2048x2048 pixel back-side CCD 14 bit ADC Coated with ML filters

TESIS INSTRUMENT  CONSTRUCTION 16 step microdrivers (doors, shutters, pointing and focusing mechanism etc) Thermo stabilized construction based on thermal pipes Active/passive cooling of CCD  ELECTRONICS 6.4x10 7 operation per second 256MB mass memory Whole instrument control 4 channels readout independently Onboard software updating Onboard processing (including star trackers) Onboard data compression

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