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Spicule Family Tree
Type I
Type II
Macrospicules
Discovered in 2007 / Ca II H line
200 - 300 km width
typically 60 -120 km/s
reduced opacity /fade from view !
Lifetime approx. 1 min
No periodicity
Observational
Signature
Formatio
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Discovered in 1877 - Hα - ‘classical’
Temp. 5,000-10,000 K
Densities 3 x 10-10 kg/m3
300 - 1500 km width ; 5 min periodicity
typically 25 -30 km/s ; 10 arcsec height
Discovered in 1975 - EUV
up to 300 km/s rise
50 - 70 arcsec height
lifetimes 20-40 min
15,000 - 30,000 km width
Wavesp-mode leakage
Unclearreconnection ?
waves ?
Magnetic ReconnectionErupting loop
Spiked Jet
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Co-observing: SST (CRISP) and
SDO
SST/CRISP
• Advance - CRisp Imaging Spectro-Polarimeter (2008)
• Dual Fabry-Pérot interferometer (FPI)
•1-m Swedish Solar Telescope (La Palma)
•Line sampling between 510 - 860 nm: 36 fps
•Chromosphere and Photosphere analysis in: Red Beam (nb + wb) Blue BeamCa II 8542 Å (Infra-red triplet) G-BandH-alpha 6563 Å Ca II HNa D 5896 ÅMg b 5172 ÅFe I 6301 & 6302 Å
•60 x 60 arcsec FOV
•0.06 arcsec / pixel - after image restoration
Scharmer et al., 2003a; 2006, 2008
SST/CRISP Data
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Credits : T. Berger Lockheed; Movie credits – M. Carlsson ; Dave Jess/QUB
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Image Credit : DOTImage Credit : DOT
SUNSPOTS
Dark spots on Sun (Galileo)cooler than surroundings ~3700K. Last for several days(large ones for weeks)Sites of strong magnetic field(~3000G)Dark central umbra (strong B)Filamentary penumbra.(inhibit convection)Arise in pairs with oppositePolarityPart of the solar cycleTypical temperature of 4,000 – 4,500 Faculae typical sizes of 10,000 – 100,000 km
SUNSPOTS
Dark spots on Sun (Galileo)cooler than surroundings ~3700K. Last for several days(large ones for weeks)Sites of strong magnetic field(~3000G)Dark central umbra (strong B)Filamentary penumbra.(inhibit convection)Arise in pairs with oppositePolarityPart of the solar cycleTypical temperature of 4,000 – 4,500 Faculae typical sizes of 10,000 – 100,000 km
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Image credit: G. Scharmer, ISP/SST
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SST/CRISP data reduction: MOMFBD
van der Voort et al., 2005
• Raw data -> Gain Corrected (flat fielding + dark current correction)
• Offset calibration : Aligning Crisp-R and Crisp-T with WB pinholes to subpixel accuracy.
• MOMFBD
• LRE/HRE Calibration: Prefilter correction
•Destretching + alignment + derotation
Reduction
Steps
MOMFB
D • A known relation exists between the wavefronts of a set of images
• Each camera (Object i) is simultaneously imaged in a number of focus diversity channels (sufficiently close in wavelength), indicated with an index k i.e. a wavelength sampling.
• By exposing multiple cameras (Objects i) a set of images can be obtained for which the degradation of the images due to atmospheric distortions is identical.
• The solution to the MOMFBD problem is to minimize the maximum likelihood error metric that measures the difference between the data frames and model data frames
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XRT
SOTSST
SDOCo-alignment across multiple instruments
ω is the angle between solar north and the optical table. φ is the azimuth. θ is the elevation.TC is the table constant.β is the tilt angle between first mirror in the telescope and solar north, i.e. a constant
14
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Alignment of the SST data with SDO