Science Lessons Learned from TESIS and their Relevance to SWAP
V. Slemzin, LPI
PROBA 2 SWT, La Roche, 14 June 2010
TESIS scientific team (LPI):S. Kuzin, S. Bogachev, S. Shestov, V. Slemzin, A. Ulyanov, A. Reva
CORONAS-Photon was launched on January 31, 2009
The projected time of the mission was 2 years
The flight was terminated after 9 months in November 2009 because of problems with the satellite power system. TESIS
Array of TESIS instruments
CHANNELS (7)
MgXIIMgXII
8.42 A8.42 A
Telescope 1Telescope 1
132 A132 A
FeXX-XXIIIFeXX-XXIII
Telescope 2Telescope 2
171/304 A171/304 A
FeIX-X / He IIFeIX-X / He II
CORONO-CORONO-GRAPHGRAPH
304A304A
SPECTRO-HELIOSPECTRO-HELIO
GRAPHGRAPH
SphinX SphinX photometer photometer SRC PANSRC PAN
SpectralRange, A
8.41-8.42
131-132
171-178 295-315
295-315
285-335
1-12
Fieldof View
45’ Disk: 10
Corona: 2-5 Rsun
2.5° ~2° -
AngularResolution
3” 1.7” 20” X: 1.7”Y: 40”
-
SpectralResolution
0.0002 A/pixel
70 20 20 0.01 A/pixel ~0.05
Exposition,sec
0.01-600 0.01-0.001
TESIS: parameters of EUV telescopes
Wavelength band 132 A (telescope I)
171 / 304 A (telescope II) Focal length……………. 1600 mm Mirror Aperture…...100 mm diameter Field of view ……………………... 1° Angular resolution……1.7 arc sec/pix Max. cadence…………1 sec (partial frame)
10 sec (full frame)
Typical cadence………..2 – 5 min Detector……….… backside CCD
2048 × 2048 pixels
CORONAS-Photon orbit
01.01.2010 01.07.2010 01.01.20110,4
0,6
0,8
1,0
no
n-o
bsc
ure
d v
iew
, % o
f the
orb
it
CORONAS-Photon
PROBA 2
Horb =550-570 km, α = 820
Eclipse time for one 95 min orbit
TESIS resuls1. Eruption of giant prominences in 304 A
TESIS HeII 304 A 23/04-2009
2. Dynamics of active regions in 171 A
3. Short-time dynamics
Nanoflares in 171 A
Cadence 3 s, exposure 0.5 s
Dynamics of spicules in 304 A
4. Eruption of a giant prominence in 304 A and U-shaped magnetic feature
12 May 2009
4. Quasi-static inner corona in 171 A
Overexposure (10 s instead of 0.1s)
Low straylight (one-mirror telescope)
Coronal dynamics during one solar rotation1-27 September 2009
N W S E N
TESIS lessons The scientific program was not fulfilled because the mission was
terminated in November 2009 due to failure of the satellite power system. Total volume of information: 700 Gb, 150000 images.
In 2009 the solar activity was unexpectedly low. Two high temperature channels did not provide valuable data (Mg, 132 A)
At very low solar activity there are many specific phenomena as global and small scale: eruption of giant prominences, a lot of bright EUV points, rich magnetic structure of the inner corona, reconnection of closed structures with open interplanetary lines.
The 171 A band is very informative to study the inner corona (T ~ 1-2 MK) in global and local scales.
Perspectives: EUV imaging with resolution < 1” and cadence of 1 s (“Arka” project)
Level 1 TESIS data are available at http://www.tesis.lebedev.ru/en/data_access.html
The inner corona in SWAP
1x10s 100x10s equatorial scan
100x10s
N W S E N
1x10s
SWAP – LASCO C2