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Past political opportunities : Intercosmos 1967 no launch payments http://www.cbk.pan.wroc.pl/body/publikacje/2005/PTA_Solar_htm.html. Plesetsk Orbital missions 3 launches 1994 Coronas-I 1995 Interball-Tail 2001 Coronas-F. Kapustin Yar Sounding rockets 7 launches 1970 1971 1977

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Slide1 l.jpg
Past politicalopportunities: Intercosmos1967no launchpaymentshttp://www.cbk.pan.wroc.pl/body/publikacje/2005/PTA_Solar_htm.html

Plesetsk

Orbital

missions

3 launches

1994

Coronas-I

1995

Interball-Tail

2001

Coronas-F

Kapustin Yar

Sounding rockets

7 launches

1970

1971

1977

1979

1980

1981

1983

1984



Sphinx soft x ray spectrophotometer l.jpg

The Team: PI Janusz Sylwester

SphinX soft X-ray spectrophotometer

  • Mirek Kowalinski : Project Manager

  • Jarek Bakała: Project Constructor

  • Szymon Gburek: Project Scientist

  • Marek Siarkowski, Barbara Sylwester,

  • Zbigniew Kordylewski, Piotr Podgórski,

  • Witold Trzebiński, Stefan Płocieniak, Anna Kępa

  • FIAN: Dr. Sergey Kuzin, TESIS PI

  • MEPhI: YuryKotov, CORONAS-Photon PM

  • AI CzAS: Dr. Franta Farnik

  • Prof. Fabio Reale, INAFA, Palermo University

    Prof. Ken Phillips, UCL, London

http://www.cbk.pan.wroc.pl/body/publikacje/2008/SphinX.pdf


Coronas f launch orbit pointing l.jpg
CORONAS-F launch, orbit & pointing

31 July 2001,

polar orbit, 95min,

~500 km

semi-Sun-synchronous

SS-14 Cyclone

x

10,

CORONAS-F

http://coronas.izmiran.rssi.ru/F/instruments


Slide5 l.jpg

Satellite CORONAS-PHOTON

TESIS

SphinX

STEP-F

KONUS-RF-anti

pressure vessel

PHOKA

RT-2/GA

RT-2/S

KONUS-RF

N-2M

RT-2/G

PINGUIN

Magnetometer

Launch is fixed to the last week of 2008 !



Tesis assembly of instruments for xuv imaging spectroscopy of the sun l.jpg
TESIS assembly of instrumentsfor XUV imaging spectroscopy of the Sun

It is advanced version of the SPIRIT instrument

http://www.tesis.lebedev.ru/


Sphinx tesis l.jpg
SphinX & TESIS

TESIS

SphinX


Instruments for charge particle measurements l.jpg
Instruments for charge particle measurements

3-axis magnetometer


Sphinx construction l.jpg
SphinX construction

  • EUV filters (doublyaluminizedMylar)

  • Photometer

    • Collimators(+-2.5 deg)

    • Threeapertures

    • D1, D2, D3

  • Shutter

    • Stepper motor

  • FFU

    • Filters

    • Targets

    • D4

  • Electronics

    • Front endAmptek

    • Digital „our”

  • Controller

    • Software

    • reprogramming

  • Heatsink

  • Alignment mirror


Measurement channels l.jpg
Measurement channels

P h o t o m e t r i c

FFU

D2

D1

D3

D4

φ: 5 mm

A: 13.0 mm2

8 μs

Up to

60 000 cts/s

FWHM: 490 eV

φ: 4 mm

A: 0.26 mm2

25 μs

Up to

20 000 cts/s

FWHM: 290 eV

φ: 4 mm

A: 0.0052 mm2

25 μs

Up to

20 000 cts/s

FWHM: 290 eV

φ: 4 mm

A: 13.0 mm2

25 μs

Up to

20 000 cts/s

FWHM: 290 eV

$4000

Detectors (four units): 256/1024energy bins

Amptek, Peltier cooled (-50 deg) Si PIN diodes.

Detectors’ support plate thermally

connected to external heat radiator

via heat sink pipe.

Photon arrival time measured towithin 2μs(in Time Stamping Mode)

Much better energy resolution than gas detectors

2.5 %against16%, low thermal noise

http://www.carroll-ramsey.com/detect.htm


Expected total count rates l.jpg
Expected total count rates

Courtesy; Marek Siarkowski


Sphinx calibration bessy synchrotron l.jpg
SphinX calibration BESSY synchrotron

Berlin February 26th 2008

March 2nd 2008

D3

RAS Meeting 9 May 2008 Janusz Sylwester, Poland: Ongoing and future solar X-ray experimenting


How it looks from the tests l.jpg
How it looks from the tests

The BESSY synchrotron input spectrum (red) with overplotted response of SphinX D2 detector (black). Nominal effective areas have been used. The agreement is better than 5% in the energy band where SphinX detectors

are the most sensitive.

BESSY

Berlin

Synchrotron:

- All detector linearity: perfect (0.1% ) over 0.8-14.5 keV; dynamic range 104.

- absolute response known to better than 5% against reference synchrotron source.

- pile-up matrices known as measured fromX-ray 4 crystal monochromator spectra

obtained at 8 energies between 1.5 and 8 keV


The measurement environment bcgd few cts s up to 10 3 cts s saa l.jpg
The measurement environment, bcgd: ~few cts/s up to 103 cts/s (SAA)

SAA Night RB RB Night Flare

CORONAS-F

  • Important pahases

  • S/C X-ray day

  • S/C optical day

  • S/C optical night

  • S/C X-ray night

  • Terminator crossing

Previous CORONAS-F

orbit


Time stamping mode d1 d2 or d3 rates 10 3 s l.jpg
Time stamping mode D1, D2 or D3 rates < 103/s

  • Time stampingmodefrom: D1, D2, D3, D4

    • 2 Bytes for processor time of thedetectorevent start

    • 1 byte for theamplitude

    • Allows to determinethedifferencebetweenevents to within 2 μs ~2/1000 accuracy

    • Absolute timing to within 0.001s against UT

      Expectedrates

      D1= 103events/s (event: Amplitude 1byte, time 2 bytes)-3 KB/s

      D2= 10 events/s, D3= 10 events/s, D4= 10 events/s

      Total: 3Kbytes/s – canlast for ~10000s (3 h) eachdump – maycover 100% cyclewithcompression


Slide18 l.jpg

Waiting time analysis – is the process at low count rate Poissonian?Wheatland, The Astrophysical Journal, Volume 679, Issue 2, pp. 1621-1628, 2008

  • Radioactivesourcesgive an idealexample of thestatistics

  • To whatdegreethearrivaltimes of photonsfromthe „quiet” coronahave „no memory” i.etheyhavetheexponentialwaiting time distribution? (Modelsfor flare statistics assume or predict that flares are independent events- howeverthisis under question)

  • Theprimarytask for theinitial part of themissionwheretheactivityisexpected to be low.


Sphinx convolved spectra a coronal l.jpg
SphinX convolved spectra (Acoronal)

O, Ne,Fe

Shape depends on T

Si

Ca

Ar

Fe

S

Ni

Fe

Ni

25 MK

pure continuum

10 MK

5 MK


Predicted behaviour of activity during active phase of coronas photon l.jpg
Predicted behaviour of activity during active phase of Coronas-Photon

http://science.nasa.gov/headlines/y2006/10may_longrange.htm


Recent goes rhessi l.jpg
Recent GOES & RHESSI


Energy calibration l.jpg
Energy Calibration

  • D1,D2,D3 solar induced fluorescence spectra of pure elements

    • During flares ~> M1

    • Until 10^6 cts collected for each detector

    • Approximately each month

    • If v. quiet condition then on the command from the ground for 10 min


Terminator transit profile of earth atmospecric absorption l.jpg
Terminator transit: Profile of Earth atmospecric absorption

  • X-ray terminator crossing algorithm operational on board

    • Predict the entry/exit to within few seconds

    • Spectra 256 energy bins each 0.1 sec give at least 1 km resolution in the vertical Earth absorption profile

    • Time stamping or spectral mode depending on the flare flag


Slide24 l.jpg
SphinX firstshttp://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The_SphinX_Instrument_on_CORONAS-PHOTON

  • SphinX will measure absolute element abundances using line features due to neon, magnesium, silicon, sulphur, argon, calcium, iron and nickel in various levels of solar activity (quiet Sun, active regions and flares). It should therefore be in a strong position to give a definitive answer to the continuing debate about the dependence of coronal abundances of elements on their first ionization potential, the so-called FIP effect.

  • SphinX will obtain the first absolutely calibrated solar X-ray spectra in the 0.8--15 keV range. In particular this will help us to understand the RHESSI continuum observations in this difficult range.

  • SphinX will also study quiet coronal heating processes via photon arrival time--distance analysis (the arrival time of an X-ray photon will be measured to a couple of microseconds); X-ray oscillations in the <1 to 500 s period range; and transient ionization in flares.


Instrument satus l.jpg
Instrument satus

  • Flight model at the Moscow „factory” undergoing final electro-magnetic & teelmetry compatibility tests

  • On November 30, TESIS ( a mother instrument for SphinX) is coming for a final maintenance tests to FIAN (MK+WT) will reload the flight programme

  • The Coronas-Photon launch is expected before the end of 2008 a X-mas present?

  • Ground sector of software v1 ready (Czech contribution under guidance od Szymon)

    • 2 mirror servers (Wrocław, Ondrejov)

    • Automatic data access to FIAN SphinX data stream (~12 hours maximum delay if 2 dumps/24h)

    • Automatic reduction to Level2

    • Data publishing to the public access area (90% data will go there decision taken by the duty scientist)

    • Automatic flare event catalogue creation start,max, end, class, Tmax, Emmax, rise phase dur L, H, EMmax-Tmax delay

    • Auxiliary data available: GOES, RHESSI, SOXS


The ffu unit filter fluorescence unit l.jpg
The FFU unit (filter-fluorescence unit)

Filter-Fluorescence Unit (FFU) layout

This unit will be active all the time: time stamping < 1000 cts/s or spectra (256 bins)


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