Coronal Image Processing The Accurate Depiction of Structure in Qualitative Images of the White Light Corona Huw Morgan, Shadia Habbal, Richard Woo.

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Presentation transcript:

Coronal Image Processing The Accurate Depiction of Structure in Qualitative Images of the White Light Corona Huw Morgan, Shadia Habbal, Richard Woo

Outline Finding an unbiased radial graded filter using a model pB corona Apply to pB observations Compare results with standard LASCO images (made using division by a long term minimum method) Processing of white light images

Synthetic Solar Minimum Corona pB at polepB at equator Current sheet width w is constant so RADIAL corona pB at equator pB at pole LOG pB

Simple Radial Graded Filter (RGF) Processed intensity Original intensity Intensity averaged over all latitudes at r WHY NOT RADIAL ???? r height  latitude

Std. deviation  Average Std. dev. Average WHY NOT RADIAL? Large change in relative contrast between high and low intensity regions with height RGF neglects the change in contrast so processed corona is distorted MODEL DATA Sol. min Sol. max

Normalizing Radial Graded Filter (NRGF) ProcessedOriginalAverage Std. dev. RGF equator RGF pole NRGF pole NRGF equator

Application to pB observations - Solar Minimum January MLSO MKIII & MKIV coronameters R s LASCO (SOHO) C2 coronagraph R s ‘Standard’ LASCO & MKIIINRGF

Application to pB observations - Solar Maximum (June ) ‘Standard’ LASCO & MKIIINRGF

LASCO ‘standard’ images or the NRGF - which gives the true picture? Latitudinal profiles at 3 heights LOG Standard NRGF Solar minSolar max

Application to white light (WL)... Easy to apply NRGF to pB observations since pB does not contain F corona and stray light. Why bother with WL? LASCO makes ~30 WL obs./day, compared with ~2 pB. LASCO WL observations have 12” resolution (1024x1024 pix). LASCO pB have half this resolution. How we do it... Calculate WL-pB for many days surrounding observation, and average. Subtract this average from desired observation This method provides excellent qualitative images of coronal structure after final processing with NRGF White light processed pB Minimum Maximum

Application to WL - comparison with LASCO standard images

Application to WL - CME

Conclusions The NRGF is a correct method for removing radial gradient from coronal images Division by a long term minimum almost invariably leads to a misleading depiction of structure A new method for processing white light images provides good results with LASCO C2 observations (C3 needs more work - due to polarization of F corona?) Using the NRGF, we can avoid saturating the image to see structure, and finer detail can be seen at all heights in the corona.