Workshop „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, RHESSI and SPIRIT...

WorkshopWorkshop „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, RHESSI and SPIRIT Instruments”RHESSI and SPIRIT Instruments”, , 6 – 8 December 20056 – 8 December 2005, , WrocławWrocław

Spectroscopy DepartmentSpectroscopy DepartmentLebedev Physical InstituteLebedev Physical InstituteMoscowMoscow

Principle Investigator: Dr. Yu.D. KotovTel/fax (007-095)-3240616E-mail: [email protected]

Space Research Program

RUSSIAN SATELLITE PROJECTRUSSIAN SATELLITE PROJECT"CORONAS-PHOTON""CORONAS-PHOTON"

FOR THE STUDY OF SOLAR FLARE FOR THE STUDY OF SOLAR FLARE HARD RADIATIONSHARD RADIATIONS

Russian Aviation and Space AgencyRussian Academy of Science

Principal Organization: Moscow Engineering Physics Institute

Launch date: end of 2007, from Plesetsk (Russia)

Launch date: end of 2007, from Plesetsk (Russia)



CORONAS-PHOTON mission is the third satellite of the Russian CORONAS program on the Solar activity observations. The main goal of the CORONAS-PHOTON mission is the study of the Solar flare hard electromagnetic radiation in the wide energy range from Extreme UV up to high energy gamma - radiation (~2000MeV).

It is adopted as a part of the Russian Federal Program of Fundamental Space Researches. The project is a part of International Living With the Star (ILWS) program.

Goal of the project: Investigation of the process of energy accumulation and its

transformation to the energy of accelerated particles during solar flares, study of the acceleration mechanisms, propagation and interaction of the fast particles in the solar atmosphere.



Direct solar flare radiation

Study of the temporal dynamic of hard electromagnetic radiation from full disk in a wide energy range from EUV to 2000MeV;

Study of spatial and temporal dynamics of hot plasma regions in Solar atmosphere by observation of X- ray/XUV radiation;

XUV full Sun spectroscopy;Nuclear gamma-lines spectroscopy of Solar activity regions;Detection of solar neutrons with energies higher 20MeV;Measurement of linear polarization and rapid variability of hard X-ray emission during the flares;

•Monitoring of the Solar extreme ultra-violet (EUV), soft and hard X-ray emissions;

Main objectives of the mission



CORONAS-PHOTON mission scientific Payload:

1. High energy radiation spectrometer NATALYA Gamma-rays spectroscopy 0.3 – 2000MeV;Neutrons 20 – 300MeV

2. Low energy gamma-ray spectrometer RT - 2 Phoswich mode: 15 – 150keV; Spectrometric mode: 100 – 2000keV

3. Hard X-ray polarimeter PENGUIN-M (X-ray radiation 1 – 10keV; X-ray polarization 20 – 150keV; X-ray & gamma-ray spectroscopy 0.15 – 5MeV)

4. Fast X-ray monitor FXM (Hard X-ray with sub-msec temporal resolution 20 – 500keV )

5. Solar flare and cosmic gamma-burst spectrometer KONUS-RF (Hard X-ray & gamma-ray spectroscopy with high temporal resolution (0.0112)MeV )

6. XUV TeleScope/ Imaging Spectrometer TESIS

7. Multi-channel Extreme ultra-violet and Soft X-ray monitor PHOKA (Timing of the full disk radiation in 7 spectral windows from 10nm to visual band )

8. Energetic particle analyzer ELECTRON-M-PESCA (e : 0.2 – 2MeV p : 1.0 – 150MeV α : 1.5 – 50MeV/nucleon Nuclei (Z <26) 2.0 – 50MeV/nucleon )

9. Energetic particle telescope STEP-F (e : 0.15 – 10MeV p : 4.0 – 62MeV α : 15.5 – 245.5MeV )



Orbit and LauncherOrbit and Launcher Circular 500 km; Period 95 min (60 min Sun/orbit)Circular 500 km; Period 95 min (60 min Sun/orbit) Orbit inclination 82°5 ; 2 weeks/ 3 months full Sun orbitsOrbit inclination 82°5 ; 2 weeks/ 3 months full Sun orbits

Launcher: Cyclon-3MLauncher: Cyclon-3M Launching date 2007Launching date 2007

Lifetime 3 –5 yearsLifetime 3 –5 years

Weight satellite: 1900 kg;Weight satellite: 1900 kg; scientific payload: 540 kg scientific payload: 540 kg



Overview of TESIS instrumentsOverview of TESIS instruments

The main emitting ions and wavelengthsThe main emitting ions and wavelengths

Ion Wavelength, Å T, ºKHeII 304,8 5*104

SiXI 304.3 1.6*106

FeVIII-FeXX 132; 1. & 12*106 MgXII 8.418; 8.423 (1-2)*107

Spectroheliograms 280 to 330 (0.05- 12)*106

The goal of the experiment “TESIS” is to study the structure and the dynamics of the solar atmosphere over a broad range of heights

and temperatures using full sun XUV spectroscopic imaging.Lebedev Physical Institute of the Russian Academy of Sciences



Main parameters of TESIS channelsMain parameters of TESIS channels

Name of channel

Parameter

FeXX (XUV

telescope)

HeII (XUV

telescope-coronagraph)

WF (XUVwide field

telescope-coronagraph)

Mg XII (spectro-

heliometer)

XUV spectro-heliometer

SphinX Solar

Photometer in X-rays

Spectral band, Å 131-133 295-315 8.418-8.423 280-335 1- 10 keV Field of view Full disk: 60 60 in the

field of 2.5 Corona up to 5

radii - 2.5 Full disk: 60

1.6 (cross to dispertion)

Spatial resolution, arcsec

1,7 4.4 2 3 (cross to dispertion)

256 channel

Spectral resolution

/~70 /~20 /~20 2*10-4 Å/pix 2*10-2 Å/pix Full Sun

Exposure time/ temporal resolution, sec

0.01 – 600 / up to 0.5 100 Hz-1000 Hz

Principal optical element

Off-axis paraboloid, Multi-layer coating

Ritchey-Chrétien 2 mirror system,

Multi-layer coating

Bragg spherical crystal quartz

Diffraction grating with 3600

l/mm

Detector backside CCD42-40 AIMO by E2V (2Kx2K size , 13.5x13.5 um), with Peltier cooler, similar to CCDs used in Secchi of Stereo



Artificial moon

Entrance filter

Detector

132A 304A

Shutter

Multilayer mirror

Pointing and focusing mechanism

Optical layout of the XUV telescopes of TESIS instrument



Wide field EUV Telescope:



synthetic quartz 2d=8.501 A 80x120 mm

MgXII spectrogeliograph



Typical image given by the spectroheliograph



Deep spectroheliogram to show a large extension of 304 emissions



SphinX Solar Photometer in X-ray

PI – Janusz Sylwester SRC PAS



Main features of the TESIS experiment

Full disk spectroscopic imaging: 4 EUV channels 1 MgXII channels Simultaneous observations in all spectral channels Temporal resolution up to 0.5 sec XUV observations of the corona, up to 5 solar radius Full Sun spectroheliograms in 280- 330 A Ritchey-Chrétien Wide FOV 304 telescope SphinX Solar Photometer in X-rays

Study of the upper Earth atmosphere Observation of space debris



On board computing and data collection features

• 50MIPS DSP

• 128MB data RAM

• Up to 4 Ch. Simultaneously + SphinX

• 8 sec readout time (2Kx2K image)

• Update on board S/W

• Loose less data compression algorithm (c.r. 2-4)

• JPEG like data compression algorithm (c.r. 10-???)

• 500 MB/day data rate



Coronas-Photon doing electrical tests at MEPhI Sept 2005

TESISTESIS

Workshop „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, RHESSI and SPIRIT...

Documents

Transcript of Workshop „X-ray Spectroscopy and Plasma Diagnostics from the RESIK, RHESSI and SPIRIT...