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Obserwacje strumienia promieniowania rentgenowskiego Słońca „jako gwiazdy” w okresie głębokiego minimum aktywności Recent solar activity as observed with X-ray spectrophotometer SphinX aboard the CORONAS-PHOTON Janusz Sylwester for the SphinX team Solar Physics Division, Space Research Centre Polish Academy of Sciences, Wrocław, Kopernika 11 XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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The SphinX Team SRC PAS Wrocław
Mirek Kowalinski, Szymon Gburek, Marek Siarkowski, Jarek Bakala, Zbigniew Kordylewski, Piotr Podgorski, Barbara Sylwester, Anna Kepa, Witold Trzebiński P.N. Lebedev Physical Institute, Moscow Sergey Kuzin-TESIS PI, Andrei Pertsov, Sergey Bogaczev Astronomical Institute, Ondrejov Frantisek Farnik Astronomical Observatory, Palermo Fabio Reale, Alfonso Collura University College, London Ken Phillips XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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SphinX: Solar Photometer in X-rays, PI: SRC-PAS
Mass ~2500 kg, 8.2 GB/day Launched 30 Jan at 13:30 UT from Plesetsk Cosmodrome CORONAS PHOTON Pointing Semi-Three axis stabilised TESIS with SphinX XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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The orbit 96 min 550km , 82.5 deg. Polar orbit Life ~7 years
Encountered SAA ~1000 cts/s & Polar ovals ~100 cts/s 4 times/96 min CORONAS-F XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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SphinX Polish concept, design & manufacture
Measures the X-ray fluence of the Sun 0.85 – 15 keV with unprecedented Time resolution ~ s Sensitivity 100 x better than GOES XRM – the standard for 30+years Energy resolution 3x RHESSI (NASA) XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Total cost of the project ~ 1 mln PLN KBN T12 grant
The construction EUV filters (doubly aluminized Mylar) Photometer Collimators (+-2.5 deg) Three apertures D1, D2, D3 Shutter Stepper motor FFU Filters Targets D4 Electronics Front end Amptek Digital „our” Controller Software reprogramming Heat sink Alignment mirror Total cost of the project ~ 1 mln PLN KBN T12 grant XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Measurement channels D1 D2 D3 D4 P h o t o m e t r i c FFU φ: 5 mm
A: 20.4mm2 8 μs Up to cts/s FWHM: 490 eV φ: 4 mm A: 0.50 mm2 25 μs Up to cts/s FWHM: 290 eV φ: 4 mm A: mm2 25 μs Up to cts/s FWHM: 290 eV φ: 4 mm A: 13.0 mm2 25 μs Up to cts/s FWHM: 290 eV Detectors (four units): 256/1024 energy bins Amptek, Peltier cooled (-50 deg C below the support T) Si PIN diodes. Detectors’ support plate passively cooled through the heat sink pipe to the external radiator Photon arrival time measured to within 2μs (in Time Stamping Mode) XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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How performance 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 detectors’ linearity: perfect (0.1% ) over keV; & dynamic range 104. - absolute response known to better than 5% against reference synchrotron source. - pile-up matrices known as measured from X-ray 4 crystal monochromator spectra obtained at 8 energies between 1.5 and 8 keV XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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GOES X class range to be extended down
10-6 W/m2 10-7 10-8 10-9 10-10 10-11 SphinX detection threshold A = 10-8 W/m2 S = 10-9 W/m2 Q = W/m2 SAA S/C night Solar X-ray flux remains at background levels: i.e. Max Millenium message XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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New X-ray classes We are introducing new „classes” of X-ray solar variability, below GOES A1.0 A = 10-8 W/m2 (present lowest) S = 10-9 W/m2 Q = W/m2 SphinX in its D1 channel is capable to observe events 100 x less intense than GOES Most of variability since the launch is observed to happen below the GOES delectability threshold XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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GOES detection threshold
Solar activity: longer-term only around 80 flares,detected by GOES, among them C2.7 on 6 July and triple B on March 26, 2009 SphinX D2 record cts/s GOES detection threshold Long S/C day The Lowest observed level Since Launch: GOES 80 events, SphinX 550 events XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Determination of absolute levels of X-ray solar luminosity E > 1 keV
D1- DGI 1s D1 D2 XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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X-ray fluence at E > 1 keV
Histogram of T values D1 rate D2 rate Instrument heating Temperature D1 rate MK Emission Measure Example: for data set No. 50 Te 1.71 MK [ 1.69, 1.72 ] EM 6.2 [ 5.7 , 6.7] cm-3 Flux [ keV] W/m2 Flux GOES [1 – 8 Å] W/m2 Thermodynamic Measure XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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TESIS images (courtesy Sergey Bogaczev FIAN)
:28: Å :27: Å ~ K ~1 MK XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Longer exposure: ~18 hours
Counts below 3 keV ~ 1 mln Counts above 3 keV ~ 3000 Ratio: 0.003 Any coronal heating model should „obey” this measurement from now on XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Example catalogue page
D1 D2 bcg XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Summary Two components on the lightcurves:
Quasi steady X-ray intensities enhanced when AR are present The lowest quasi-steady state level, when no AR are present, is also observed in D2, this level is still fluctuating on a 5 min time scale study is in progress. Flares are seen on-top of this basal variability. Flare „enhancements” are being detected from amplitudes above ~ 0.05 dex. Both short and LDE types of events are present „without the sunspots” The Sun is the weakest X-ray star within 7 parsecs (Schmitt et al., 1995, ApJ, 450, 392) with our new estimated luminosity at LX = 1.3 × 1018 W 100 x less α Cen A., 47 x less previous estimates (Judge et al., 2003, ApJ, 593, 534) Luminosity in the 1—300 Å is 8.0 × 1025 erg s-1, a value which is of interest for heating the Earth’s atmosphere, much below present estimates Thermal energy content of the solar corona is 2 × 1030 erg XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Please have a look at the poster
The End Please have a look at the poster Barbara Sylwester, Janusz Sylwester, Marek Siarkowski Zakład Fizyki Słońca CBK PAN Wrocław: "Interpretacja widm uzyskanych za pomocą polskiego spektrofotometru SphinX" XXXIV Zjazd PTA Kraków , Solar Session, 15 September Janusz Sylwester
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Compilation of SphinX flare catalogue
SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX
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Flare statistics – based on SphinX catalogue interpretation (provisional)
Increasing trend is noticeable Flare amplitude vs the occurence times of events GOES detection Threshold SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX
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30 April 2009 10:42 A3.1 flare XRT Hinode EIT SOHO 195 Å
SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX
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Spectra maximum decay E2 E1
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Flare evolution on T-EM diagram see poster B. Sylwester et al.
ThM = T * sqrt(EM)
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SS RTV: 2 Log T – ½ Log EM = ½ Log(L/2A) - 6.145
Diagnostic Diagram Jakimiec, J.; Sylwester, B.; Sylwester, J.; Serio, S.; Peres, G.; Reale, F. 1992A&A From HXIS eH eH A A C L C L Palermo-Harvard Code Peres et al., 1982 Jakimiec, J.; Sylwester, B.; Sylwester, J.; Mewe, R.; Peres, G., 1986AdSpR J SS RTV: 2 Log T – ½ Log EM = ½ Log(L/2A)
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Diagnostic diagram based on GOES
Sylwester, J.; Sylwester, B.; Phillips, K. J. H.; Kepa, A. Warning
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Differential 120”x120” image: flare-preflare
06 June B2.6 flare TESIS 171 Å XRT Hinode SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX Differential 120”x120” image: flare-preflare
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Spectra E2 E1 maximum decay
SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX
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Flare evolution on T-EM diagram see poster B. Sylwester et al.
ThM = T * sqrt(EM)
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Conclusions SphinX will provide flare flags to Coronas (testing algorithms in orbit) Sphinx measurements allow To See solar X-ray variability from the bottom level up to X20 To Determine absolute fluxes above 1 keV, each few s (also GOES in standard bands) To Study photon arrival times statistics (needs some more work on the instrument operation) To Study small flare statistics Will supplement RHESSI spectra towards lower energies Will provide the most exhaustive flare catalogue SOLAR CORONAL LOOPS WORKSHOP IV , Wednesday, July 1, Janusz Sylwester: Activity - SphinX
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