Astrophysical: Radiative transfer

  • Publication
    Spectropolarimetric diagnostics of unresolved magnetic fields in the quiet solar photosphere
    A few years before the Hinode space telescope was launched, an investigation based on the Hanle effect in atomic and molecular lines indicated that the bulk of...
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    Spectropolarimetric multi line analysis of stellar magnetic fields
    Aims: In this paper we study the feasibility of inferring the magnetic field from polarized multi line spectra using two methods: The pseudo line approach and...
  • Publication
    Spectropolarimetric synthesis of forbidden lines in magnetohydrodynamic models of coronal bright points
    Context. The inference of the magnetic field vector from spectropolarimetric observations is crucial for understanding the physical processes governing the...
  • Publication
    Spectropolarimetry of solar faculae - High spatial resolution results
    A new method to measure the magnetic field strength of small-scale solar magnetic concentrations is presented. It is based on the center of gravity method...
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    Stokes Profiles Inversion Techniques
    Inversion techniques of the radiative transfer equation for polarized light are presented as one of the best current procedures to infer the vector magnetic...
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    Stratification with Optical Depth of the 5 Minute Oscillation through the Solar Photosphere
    An analysis of the 5 minute oscillation in the solar photosphere has been carried out using an inversion of the radiative transfer equation applied to a time...
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    Stray-light effects on the solar intensity distribution
    A description of the stray-light problem based on a radiative transfer approach is presented. The 2D convolution that describes the effect of the stray-light is...
  • Publication
    Structural algorithms to solve radiative transfer problems
    Not Available
  • Publication
    Structure and components of an LTE stellar atmosphere model
    We summarize in this paper the principles for the algorithmic representation of the structure of a stellar atmosphere. The physical analysis of the problem...