magnetic field measurements in and above a limb active region philip judge hao, ncar and montana...
TRANSCRIPT
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Magnetic field measurements in and above a limb active region
Philip Judge
HAO, NCAR and Montana State
University
Roberto Casini
Thomas Schad
Lucia Kleint
Sarah Jaeggli
Rebeca Centeno
coronal structure is imprinted in the chromosphere
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The Quest: measure the magnetic free energy over active regions
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Method: use He I lines formed at the coronal base
what? surely you are joking?
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A quirk of nature. Sometimes we need a bit of luck.
4
He triplets can be populated only inthe cool plasmaimmediately adjacent tothe corona, unlesshigh energy photons/electrons in deeper layers can prevail.
In 1D models this meansthe uppermost scaleheight of the chromo-sphere.
Low beta
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Yes, use He I lines formed at the coronal base
But 1D models? Surely you are STILL joking?
Ah… not so fast…
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here is the well-knownlimb “He shell”
Unique “gap”, line forms ~ 1.5-2Mm
I I ISi He
gap = absence of emission (opt thin vs Eddington Barbier)
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..and a lot of hard work ..and a lot of hard work:
Lin, Jaeggli (PhD 2011, U. Hawaii) ..
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..and a lot more hard work:inversion codes for He 1083
HAZELAsensio Ramos, Trujillo Bueno, et al. 2008
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Particular observations:
FIRS 1083nm channel
22 Sep 2011, 20 minute sequence
NOAA 11302 at E limb
6 hours after X1.4 class flare.
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Context
Boringspacecraft intensity data Boring
ground-basedintensity data
mildyusefulspace-basedmagneticdata
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Boringintensity data -
becausethese are“effects”not“causes”
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Stereo B (L=265 deg)
Usefulintensity data
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Interesting dataHigh sensitivity He I polarimetry
FIRS data and processing
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High sensitivity demands special care in both data acquisition and processing. - use AO for residual seeing reduction - flat fields - deep integrations - polarization calibration - use 1 of 4 slits (spectral purity) - use PCA to remove residual fringes
- diverse PCA training set of spectra needed
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opticalfringe
removal
Casini, Judge, Schad2012 ApJ
2D PCA
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FIRS monochromatic imagesfrom 20min scan (75 steps, slit || limb)
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seeing-induced crosstalk at the limb
Spurious polarizationsignals at several %level at/above limb
Not completely understood
rows at/ above limb are crosstalk
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Seeing (DST G band)
Frames 17:00-17:09, rms (limb) 0.3”
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Seeing (DST Ca II camera)
Frames 17:00-17:09, rms (limb) 0.3”
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1083 nm region IQUV spectra (x=λ, y=position along slit)
Redshifted v>>0 post-flare loop data within coronal plasma: REAL
He I Polarization at coronalbase in active region, v~0
residual fringes
Polarized spectra
t (t)
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Disk data: Milne- Eddington inversions
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on disk inversions of “plumes”
ME:
SLAB:
(binned 2x2 pixels)
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off-limb inversions: optically thin slabs
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Observed and inverted profiles along a plume
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Inversion maps
Caveat: seeing- induced noise, crosstalk and other systematic errors seriously affect limb/off-limb data.
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results: surface fields
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results: plumes
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FIRS Si vs He inversions: curious
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Conclusions: He I 1083 high s/n spectropolarimetry
• challenging (small B, polarization, non-ideal setup)• (our limb data do not address free energy problem)• in spite of difficulties:
• we achieved 0.03%* sensitivity with FIRS • demonstrated credible inversions
• though not an ideal dataset• inversions “make sense” (ME vs slab vs thin)• first measurement of B above limb in post flare loops
• He I should be a prime line for Solar C• Imaging IR spectropolarimeter (coronagraph) needed
• Judge, Heliophysics decadal survey• BBSO NST• ATST?
*residual noise, rms, sensitivity, not accuracy
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You failed!
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Failed indeed… but this is not easy…and remember….
2012
2014 - vector fields at the coronal base?
2013
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Maybe! T. Schad, Ph. D. Thesis, U. Arizona: The Right Stuff