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

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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

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

Credits : T. Berger Lockheed; Movie credits – M. Carlsson ; Dave Jess/QUB

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

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

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Alignment of the SST data with SDO