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.
www.tesis.lebedev.ru
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
www.tesis.lebedev.ru
TESIS INSTRUMENT OVERVIEW
Channel Aims Description Wave-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 8.418 A and 8.423 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
280-330 A 1°.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
130-136 A (telescope I)
290-320 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
290-320 A 2°.5 (inner and outer corona from 0.7 to 4 solar radii)
5 arc sec / pixel
www.tesis.lebedev.ru
METHODS OF TESIS OBSERVATIONS
HeII 304 A
MgXII 8.42 A
FeXX 132 A
EUV295-315 A
TESIS will provide simultaneous imaging of the Sun in 4 spectral channels, including EUV channel 295-315 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
www.tesis.lebedev.ru
Bragg angle………………………………… 82°.08 Wavelength band…….......………. MgXII 8.418 A
and 8.423 A doublet Focal length……………………………. 1378 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 pixelsCCD pixel size ……………………. 13.5 μ × 13.5 μ
MgXII IMAGING SPECTROHELIOMETERoverview www.tesis.lebedev.ru
MgXII IMAGING SPECTROHELIOMETERCCD detector
•Back-side•2048x2048 pixel•13.5x13.5 mkm•14 bit ADC•Noise - 6e/sec (0C)
www.tesis.lebedev.ru
Wavelength band….…...130 – 136 A (telescope I)
290 – 320 A (telescope II) Focal length………………………………. 1600 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 pixelsCCD pixel size ………………..……. 13.5 μ × 13.5 μ
FULL-DISK EUV TELESCOPESoverview www.tesis.lebedev.ru
Wavelength band….…...130 – 136 A (telescope I)
290 – 320 A (telescope II) Focal length………………………………. 1600 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 pixelsCCD pixel size ………………..……. 13.5 μ × 13.5 μ
FULL-DISK EUV TELESCOPESoverview www.tesis.lebedev.ru
FULL-DISK EUV TELESCOPEStemperature response
Fe XX (132 A)
Tmin = 5 × 10 6 K
Tmax = 1.2 × 10 7 K
MgXII channel Tmin ………… about 4 × 10 6 K
Tmax ……………….…….. 10 7 K
www.tesis.lebedev.ru
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 pixelsCCD pixel size ……………………. 13.5 μ × 13.5 μ
EUV SPECTROHELIOMETER overview www.tesis.lebedev.ru
EUV SPECTROHELIOMETER targets of observations
Spectral diagnostic of solar active regions
www.tesis.lebedev.ru
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 pixelsCCD pixel size ………………..……. 13.5 μ × 13.5 μ
www.tesis.lebedev.ru
TESIS DAILY DATA
TESIS may provide
30 000JPEG images
(512×512 )
TESISdaily
telemetry
~0,5 Gb
250full FITS files(2048×2048)
1000Binned FITS files
(1024×1024)~1 hour of movies
(10 frames in sec)
www.tesis.lebedev.ru
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
www.tesis.lebedev.ru
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• 6.4x107 operation per second• 256MB mass memory• Whole instrument control• 4 channels readout independently• Onboard software updating• Onboard processing (including star trackers)• Onboard data compression
www.tesis.lebedev.ru
Top Related