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Intra-Network Magnetism and Solar Irradiance Variations

This research project explores the contribution of intra-network magnetism to the variations in solar irradiance and its implications. It includes measurements of the filling factor and magnetic fields, as well as analysis of observed signals and probability density functions. The results suggest that the role of intra-network magnetism cannot be neglected in understanding solar irradiance variations.

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Intra-Network Magnetism and Solar Irradiance Variations

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  1. The contribution of the intra-network magnetism to the solar irradiance variations Sánchez Almeida, Domingo, Bonet Navarro, Dominguez Cerdeña, Cabello, Marquez

  2. Total irradiance variations Two component model

  3. 0.5 0.02 0 0.02 0.2 0.01 0.7 0.0007 0.2 0.01 0.9 0.0002 30% variations of the IN fill factor may produce irradiance variations of some 0.07%,comparable to the observed values, It is not obvious that the role of the IN can be neglected

  4. ISSI team inspired research project • Measure with the SST (Swedish Solar Tower, La Palma) the filling factor aand the center-to-limb variation of the intensity I. • Estimate of filling factor abased on spectro- polarimetric measurements of the IN magnetic fields. • Got time from July 8 to July 22 (V. Domingo, I. Cabello, J.A. Bonet, I. Marquez, I.Dominguez Cerneña & SA). • Decent data up to m= 0.38. Image restoration allows 0.1” resolution. • G-band + CaK for region identification. A blue continuum and a red continuum for color temperature estimate. • Estimate the probability density function (PDF) of the magnetic field strength based on Hanle and Zeeman observed signals. (Dominguez Cerdeña & SA) • B > 1200 G is expected to be bright.

  5. SST, June 2005 G-band raw image m=0.98 Interior of a super-granulation cell

  6. SST, June 2005 G-band raw image m=0.38 Interior of a super-granulation cell

  7. evident barely visible Restored image, m=0.98

  8. PDF(B): probability of finding a field strength B in the quiet Sun. Vögler (2003), 50 G Vögler (2003), 200 G Z=0, disk center Dominguez Cerdeña, SA, & Kneer (2005), an empirical PDF satisfying observational constraints set by • Zeeman signals of Fe I 6301A, Fe I 6302A, Fe I 15648A, Fe I 15652 • Hanle signals of Sr I 4607 A

  9. The tail of strong kG fields can be bright in continuum (hot wall effect, Spruit 1977) Even though not all kG will be bright, BP are expected to cover a few percent of the solar surface.

  10. ... to be continued

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