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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, 51-622 Wrocław, Kopernika 11
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
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 2009
Janusz Sylwester
SphinX: Solar Photometer in X-rays, PI:
Mass ~2500 kg,
8.2 GB/day
SRC-PAS
Launched
30 Jan. 2009 at 13:30 UT
from Plesetsk
Cosmodrome
Pointing
Semi-Three axis stabilised
TESIS with
http://www.tesis.lebedev.ru/
SphinX
http://www.cbk.pan.wroc.pl/body/publikacje/2008/SphinX.pdf
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
The orbit
96 min
550km ,
82.5 deg.
Polar orbit
Life ~7
years
CORONAS-F
Encountered
SAA
~1000 cts/s
&
Polar ovals
~100 cts/s
4 times/96 min
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
SphinX
Polish concept, design & manufacture
Measures the X-ray
fluence of the Sun 0.85 –
15 keV with
unprecedented
– Time resolution
~0.00001 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 2009
Janusz Sylwester
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 2009
Janusz Sylwester
Measurement channels
Photometric
FFU
φ: 5 mm
A: 20.4mm2
8 μs
Up to
25 000 cts/s
φ: 4 mm
A: 0.50 mm2
25 μs
Up to
20 000 cts/s
φ: 4 mm
A: 0.0052 mm2
25 μs
Up to
20 000 cts/s
φ: 4 mm
A: 13.0 mm2
25 μs
Up to
20 000 cts/s
FWHM: 490 eV
FWHM: 290 eV
FWHM: 290 eV
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 2009
Janusz Sylwester
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 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 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 2009
Janusz Sylwester
GOES X class range  to be extended down
10-6
W/m2
10-7
A = 10-8 W/m2
10-8
Solar X-ray flux remains at background levels:
i.e. Max Millenium message
10-9
S = 10-9 W/m2
10-10
SAA
S/C night
10-11
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Q = 10-10 W/m2
SphinX detection
threshold
Janusz Sylwester
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 = 10-10 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 2009
Janusz Sylwester
Solar activity: longer-term
only around 80 flares,detected by GOES, among them C2.7 on 6 July
2009 and triple B on March 26, 2009
SphinX D2 record cts/s
GOES detection threshold
The Lowest observed level
Since Launch:
Long
S/C
day
GOES  80 events, SphinX  550 events
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
Determination of absolute levels of
X-ray solar luminosity E > 1 keV
D1- DGI 1s
E1 /E2
D1
D2
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
X-ray fluence at E > 1 keV
Instrument
heating
Histogram of
T values
D2 rate
D1 rate
Temperature
D1 rate
1.6 1.8 2.0 MK
Emission Measure
Thermodynamic Measure
Example: for data set No. 50
Te
1.71 MK [ 1.69, 1.72 ]
EM 6.2 [ 5.7 , 6.7] 1047 cm-3
Flux [1 - 15 keV] 1.4 10-8 W/m2
Flux GOES [1 – 8 Å] 4.2 10-10 W/m2
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
TESIS images (courtesy Sergey Bogaczev FIAN)
2009 02 20 18:28:42 304 Å
2009 02 20 18:27:42 171 Å
~80 000 K
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
~1 MK
Janusz Sylwester
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 2009
Janusz Sylwester
http://www.cbk.pan.wroc.pl/sphinxnews/?page_id=25
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
Example catalogue page
D1
D2
bcg
XXXIV Zjazd PTA Kraków , Solar Session, 15 September 2009
Janusz Sylwester
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 2009
Janusz Sylwester
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 2009
Janusz Sylwester
Compilation of SphinX flare
catalogue
SOLAR CORONAL LOOPS WORKSHOP IV ,
Wednesday, July 1, 2009
Janusz Sylwester:
Activity - SphinX
Flare statistics – based on SphinX catalogue
interpretation (provisional)
Flare amplitude vs
the occurence times
of events
GOES detection Threshold
Increasing trend is
noticeable
SOLAR CORONAL LOOPS WORKSHOP IV ,
Wednesday, July 1, 2009
Janusz Sylwester:
Activity - SphinX
30 April 2009 10:42 A3.1 flare
EIT SOHO 195 Å
XRT Hinode
SOLAR CORONAL LOOPS WORKSHOP IV ,
Wednesday, July 1, 2009
Janusz Sylwester:
Activity - SphinX
Spectra
maximum
decay
E2
E1
Flare evolution on T-EM diagram
see poster B. Sylwester et al.
T
EM
ThM = T * sqrt(EM)
Diagnostic Diagram
Jakimiec, J.; Sylwester, B.; Sylwester, J.; Serio, S.; Peres, G.; Reale, F.
1992A&A...253..269
From HXIS
A
eH
C L
Palermo-Harvard Code
Peres et al., 1982
A
eH
C L
Jakimiec, J.; Sylwester, B.; Sylwester, J.;
Mewe, R.; Peres, G., 1986AdSpR...6..237J
SS RTV: 2 Log T – ½ Log EM = ½ Log(L/2A) - 6.145
Diagnostic diagram based on GOES
Sylwester, J.; Sylwester, B.; Phillips, K. J. H.; Kepa, A.
06 June 2009 B2.6 flare
TESIS 171 Å
XRT Hinode
SOLAR CORONAL LOOPS WORKSHOP IV ,
Wednesday, July 1, 2009
Janusz Sylwester:
Activity - SphinX
Spectra
maximum
decay
E2
E1
SOLAR CORONAL LOOPS WORKSHOP IV ,
Wednesday, July 1, 2009
Janusz Sylwester:
Activity - SphinX
Flare evolution on T-EM diagram
see poster B. Sylwester et al.
T
EM
ThM = T * sqrt(EM)
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, 2009
Janusz Sylwester:
Activity - SphinX