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

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.

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


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


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


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)


MgXII IMAGING SPECTROHELIOMETERtemperature response 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


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


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


SOLAR EUV CORONOGRAPH 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)


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• 6.4x107 operation per second• 256MB mass memory• Whole instrument control• 4 channels readout independently• Onboard software updating• Onboard processing (including star trackers)• Onboard data compression


THANK FOR YOUR ATTENTION


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

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