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patrick-howell

Imaging: intensity and magnetic measurements - PowerPoint PPT Presentation

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Imaging: intensity and magnetic measurements
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  1. Imaging: intensity and magnetic measurements Feature definition: by magnetograms, by filtergrams or else…. Empirical models ISSI team – Session 2 – 4-6 July 2005

  2. Still deepening….. Modelling irradiance variations through full-disk PSPT images and semi-empirical atmospheric models Ilaria Ermolli 1 Francesco Berrilli 2, Mauro Centrone 1, Serena Criscuoli 2, Fabrizio Giorgi 1, Valentina Penza 1, Corrado Perna 1 1 INAF Osservatorio Astronomico di Roma 2 Università degli Studi di Roma “Tor Vergata” ISSI team – Session 1 - 11-15 october 2004

  3. Test the capability of the models to reproduce the emergent intensity Mod E Ermolli et al. 2003, A&A, 412, 857 Mod H Mod F Penza et al. 2004, A&A, 413, 1115

  4. Test the capability of the models to reproduce the emergent intensity

  5. Test the capability of the models to reproduce the emergent intensity

  6. Test the capability of the models to reproduce the emergent intensity: main results Mod E reproduces the network CLV Computed/Measured 0.05% difference until m=0.3 Mod P and Mod H do not reproduce the measured facular CLV Mod F reproduces the facular CLV with a difference less than 1% until m=0.3 Mod P and Mod H produce negative continuum facular contrast at the m=1 , not measured Slight model modifications to optimize details of this comparison Small C variation in time (2000> 2003-04) Dependence on the feature id: Mag > CaII K > B-R > Chapman meth

  7. Count magnetic “ingredients” of solar variability

  8. Count magnetic “ingredients” of solar variability 5 components -> 86% of TSI variance

  9. Rome PSPT images 2555 days VIRGO (total) RISE- SATIRE models 4 components -> 98%of TSI variance June- July 2004

  10. Reconstruction of the disk integrated spectrum (VIRGO TSI): Main results Magnetic “ingredients” of solar variability Spot (umbra, penumbra), faculae, network -> 86% of TSI variance Spot (umbra, penumbra), faculae, quiet sun -> 98% of TSI variance Their respective weight Whether variation of the coverage factors alone and/or emergent intensity Study limitations of decomposing the Sun into structures The use of a set of 1D models simplifies the approach, but needs a correct determination of the coverage factors, that are strongly dependent on the feature identification procedures. Feature id more important than spatial scale and seeing effects