Solar space-born instruments and detectors for X-ray observations of the solar corona. Szymon Gburek Space Research Centre Polish Academy of Sciences,

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Presentation transcript:

Solar space-born instruments and detectors for X-ray observations of the solar corona. Szymon Gburek Space Research Centre Polish Academy of Sciences, SRC-PAS Solar Physics Division Wrocław, Kopernika 11 MPGD 2013/RD51, 1 – 6 July, 2013, Zaragoza, Spain

OUTLINE About the group (SRC-PAS) Solar X-ray observation SRC-PAS solar experiments

SPACE RESEARCH CENTER POLISH ACADEMY OF SCIENCES WARSAW SOLAR PHYSICS DIVISION WROCLAW

English SOLAR PHYSICS DIVISION, SRC PAS – WROCLAW the website

WHY STUDY THE SUN IN X-RAYS Solar corona is well seen in short wavelength radiation – studies of coronal heating problem Studies of triggering, evolution and spectroscopy of solar flares - the most energetic events in the Solar System. Determining coronal plasma physical parameters T, EM Improving models of solar chemical composition – element abundances Tstin plasma ionisation equlibrium Space weather

Past and present solar soft X-ray imaging SRC-PAS early experiments Sounding rocket experiment XRT telescope on Hinode satellite

Overwiev of solar activity as seen by GOES satellites 1 – 8 Angstrom wavelength range

GOES 12, Mass 2T, Mid 1970's – present, Orbit geostationary 35,790 km 1m

Solar spectra – theory – generated with CHIANTI code Big flare Active Sun Quiet Sun

Quiet 15 September 2009 Active 14 November 2012 Large solar flare 13 May 2013 Solar limb

RECENT SRC-PAS EXPERIMENTS RESIKSphinXRF-15I

20 cm Solid state detectors Si – PIN diodes Energy range ~ keV Resolution ~0.4 keV SphinX: Solar Photometer in X-rays CORONAS – Photon satellite February – November 2009

SphinX detectors and optics X-RAYS D1 D2 D3 Seven orders of magnitude of solar X-ray flux covered AMPTEK Si PIN-DIODES XR-100CR X-RAYS Al entrance filters Be detector windows

SphinX/GOES-10 X-ray measurements in 2009 SphinX GOES-10

RF-15I photometer/imager, INTERBALL – Tail spacecraft August 1995 – December cm energy range keV proportional detectors Gas Ar+10%CO 2, 350 Torr 2 - 3, 3 - 5, keV scintillation detector NaI(Tl) crystal 10-15, 15-30, 30-60, , keV

RF-15I instrument, top view, no cover. Imager assembly photometer assembly

10 cm RF-15I detectors Calibration source

2 – 3 keV 3 – 5 keV 5 – 8 keV 10 – 15 keV 15 – 30 keV keV Time UT, 2 February 1997 Counts per second RF-15I example of data

Figure 3: Left: RF15-I soft X-ray Photometer-Imager flown on INTERBALL-Tail mission. Center: Imager assembly of RF15-I, Right image obtained from RF15- I (grid is 50×50 arcsec). Gas equal xenon - argon mixture with 5 % CO 2. Resolution ~ 10 m Å. The wavelength coverage, 3.3 Å Å, includes emission lines of Si, S, Cl, Ar, and K Four wavelength channels Printed in Zaragoza 02 July 2013 RESIK Bragg-cristal spectrometer CORONAS-F satellite August 2000 – May 2003

RESIK detectors 10 cm

RESIK example spectra

Further SRC-PAS satellite projects Development of the next solar X-ray Bragg – crystal spectrometer Development of a solar X-ray polarimeter

Thank you More in the posters and another talk tomorrow!!!