solar prominence properties derived from the uv-euv sumer spectral atlas
DESCRIPTION
Solar Prominence Properties derived from the UV-EUV SUMER spectral atlas. S. Parenti, J.-C. Vial, P. Lemaire IAS, Univeristé Paris Sud. The atlas: motivation. To carefully determine the complex physical character istics of the prominence. - PowerPoint PPT PresentationTRANSCRIPT
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Solar Prominence Properties derived from the UV-EUV
SUMER spectral atlas
Solar Prominence Properties derived from the UV-EUV
SUMER spectral atlas
S. Parenti, J.-C. Vial, P. Lemaire
IAS, Univeristé Paris Sud
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The atlas: motivationThe atlas: motivation
To carefully determine the complex physical characteristics of the prominence.
• We use SUMER (high spatial and spectral resolutions) to build an UV-EUV spectral Atlas.
• A large spectral coverage in UV-EUV gives the coverage of a large range of temperatures (Chromosphere – Prominence Corona TR – Corona)
• Spectroscopic informations:o, FWHM dynamics
line Intensity N,T, Emission Measure, AX
First complete First complete atlasatlas between 800 a between 800 andnd 1250 1250 ÅÅ
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The dataThe data• Prominence and QS 10/’99 (MEDOC #4)• Spectral range: 800 - 1250 Å (det A)• Observation time 5:30h• Spectral windows of 40 Å ( 20 in the kbr)
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Ly
1 1
Ly
8
Ly
1 9
Ly
1 3
N I
I
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Data processingData processing
• Determine the stray light contribution• Wavelength calibration for each spectral
window, for the QS and prominence independently.
• Multi-Gaussian line fitting of about 600 lines in each dataset.
• Line identification and radiometric calibration.• About 30 new lines identified (mostly from ions
at low ionization stage) between the QS and the prominence
I, o, FWHM
S. Parenti, J-C Vial, P. Lemaire, Sol. Phys, 220, 61, 2004
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S. P
arenti, et al., 2004
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The final productThe final product
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The Differentiel Emission MeasureThe Differentiel Emission Measure
• Selection of observed lines intensities• CHIANTI (v 4.2) atomic database
(Mazzotta et al. Ion fraction; coronal abundances)
• Inversion technique to estimate DEM(T)• QS ; PRM1
dTTDEMTGIobs )()( dTdTdhNdTTDEM e2)(
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The DEM: resultsThe DEM: results
Prominence A_1Quiet Sun
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Non Thermal VelocitiesNon Thermal Velocities
2
MkT2 solarv
FWHMFWHMFWHM instsolarmeas
222
2ln22FWHMcv
• Lines from allowed transitions, well isolated and intense
• T is for the maximum ionization fraction. For the neutrals: Chae et al. 1998
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Non Thermal Velocities: results
Non Thermal Velocities: results
Chae et al., A
pJ, 505, 957, 1998
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Future workFuture work
• We have produced the first complete UV-EUV prominence atlas in the range 800 Å - 1250 Å
• Still 350 Å to be processed• We derived DEMs and NTVs for both QS and
prominence
physical interpretation• More physical properties to be derived..
Thank you Philippe!!!!Thank you Philippe!!!!
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DEM in the prominence
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Data processing