Reconstruction of the EUV spectral irradiance Atomic data and model atmosphere structures Margit Haberreiter Veronique Delouille, Benjamin Mampeay, Micha.

Reconstruction of the EUV spectral irradiance

Atomic data and model atmosphere

structures

Margit HaberreiterVeronique Delouille, Benjamin Mampeay, Micha Schoell, Rami Qahwaji, Ilaria Ermolli

SOLID First Annual Meeting Margit HaberreiterOct 14 – 18, 2013, Orléans

Reconstruction of EUV variations


i: concentric rings rij: class (feature)

Ij:(ri,λ): Intensity for each feature and position on the solar disk

50 1001 10

7

1 106

1 105

1 104

1 103

0.01

0.1

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SPRM 1SPRM 2SPRM 3SPRM 4SPRM 5

Wavelength (nm)

Irra

dian

ce (

erg

cm-2

s-1

nm

-1)


I(λ,μ,φ,t)

nlevel, nel,nion,…

(x,y,z,t)

I(λ,μ,φ,t)

Iterative

process

EUV reconstruction - Semi-empirical modeling

Solar Modeling (SolMod) code• Multi level atoms

– 373 ions, from H to Ni with ioncharge 25– ~14’000+ atomic levels– ~170’000+ spectral lines – Statistical equation is solved to get the level populations

• Chromosphere and transition region – Fontenla et al. ,2009 atmosphere structures -> to be

updated– for ioncharge 2: – full NLTE (Fontenla et al., 2009)

• Corona– Coronal structures (Haberreiter, 2011, SoPh)– ioncharge >2 – optically thin, i.e. collisions and spontaneous emission

(updated to latest Chianti v7.1.9)– Line of sight integration accounts for opacity– Spherical symmetry

Model Atmospheres of Chromosphere and Transition region

Synthetic EUV Spectra


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SPRM 1SPRM 2SPRM 3SPRM 4SPRM 5

Wavelength (nm)

Irra

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cm-2

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nm

-1)

Quiet Corona (QS1)Quiet Coronal Network (QS2)Active Coronal Network (AR1)Hot loops (AR2)Super hot loops (AR3)

Contribution of chromosphere, transition region and corona


SolMod Contrast at EIT passbands


Contrast of SOLMOD spectra for the EIT 171 and 195 passbands

Determination of the intensity centers for each class


Filling factors from SOHO/EIT


Image segmentation of SOHO/ EIT images carried out by ROB(D3.2)

SolMod Reconstruction versus SOHO/SEM


SolMod Reconstruction versus SOHO/SEM


Missing some variability

AR2 and AR3 are represented by the brightest model (AR3)

Reasons: Background radiation from chromosphere and transition region needs to be added

In process for D4.4: using the PSPT filling factors

Also analysis from Rami using the MDI analysis

Pre-study: Determine the center intensity of each class


Missing some variability:

Some inter-class variation might be missing

-> inherent to the approach

Status of Deliverables under PMOD/WRCs’s responsibility

• D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum

• D4.3 Improvement of the atomic data set employed in the spectral synthesis

• D4.4 Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images

• D8.2: Database to disseminate the irradiance time series and segmentation maps

D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum

• Main problems indicated with the line formation of EUV/UV spectral lines

• Lyman-α ✔

• He II 304 nm in progress

• He II continuum

(“improvement” not explicitly specified in the proposal)

D4.2: 1. Lyman-α line formation

Schöll, Haberreiter, Schmutz, Shapiro, submitted to A&A

AD: Ambipolar Diffussion

Without ADWith AD








D4.2: 2. He continuum and He II 304 Å

Haberreiter, 2011, Solar Physics

D4.2 Improved atmosphere structures for the

synthesis of the EUV/UV spectrum


• Improvement atmosphere structure for modeling the Lyman α line

• Decreased temperature in the chromosphere will lead to a decrease in the He II 304 spectral line

• He II 30.4 nm calculations are on their way for end of November

D4.3 Improvement of the atomic data set employed in the spectral synthesis


• Two main points to be addressed:

1. Update of atomic data of already implemented spectral lines to Chianti 7.1.9

2. Implementation of highly ionized ions

3. Update from Giulio on important lines for the (optically think UV that were not yet implemented in Chianti 7.1.9

D4.3: 1. Update of atomic data of implemented spectral lines to Chianti

7.1.9

• Update of the atomic data set from Chianti 5.2 to Chianti 7.1.9

D4.3: 1. Update of atomic data of implemented spectral lines to Chianti 7.1.9

• Update of the atomic data set from Chianti 5.2 to Chianti 7.1.9

D4.3: 1. Update of atomic data of implemented spectral lines to

Chianti 7.1.9


• For D4.3:

• Compare the calculation of the additional optically thin lines carried out with SOLMOD versus CHIANTI

Status Update WP8 / SOLID Database

http://projects.pmodwrc.ch/solid-visualization/makeover/

Deliverables within first year of SOLID (1)

No Title Lead Benficiary

Month Status

D4.2 Improved atmosphere structures for the synthesis of the EUV/UV spectrum

PMOD/WRC

6 -> 12 (✔) Ly αIn

progress (He II)

D4.3 Improvement of the atomic data set employed in the spectral synthesis

PMOD/WRC

12 (✔)

D4.4 Reconstruction and validation of EUV/UV Spectral irradiance based on SOHO/EIT, PSPT/Ca II images

PMOD/WRC

12 In progress

D8.1 Project Webpage PMOD/WRC

12 ✔

Future Steps

• Use PROBA2/SWAP and PSPT filling factors for reconstruction of the EUV/UV and visible

• Use the MDI analysis by Rami for the reconstruction of the UV and visible

• Use Picard/SODISM data for reconstruction of the UV and visible

Towards the Recommended SSI time series

• SSI from semi-empirical modeling

• We need to discuss an approach how to determine the error propagation:

• the contrast of activity features

• filling factor


D4.2: 2. He continuum and He II 304 Å

Haberreiter (2011), Solar Physics, 274, 473

Reconstruction of the EUV spectral irradiance Atomic data and model atmosphere structures Margit Haberreiter Veronique Delouille, Benjamin Mampeay, Micha.

Documents

orlans slide

class solid

approach slide

corona solid

sohosem solid

sohoeit solid

solar disk slide

mdi analysis slide