Astrofísicas: Transferencia radiativa

  • Publicación
    Optical Tomography of a Sunspot. I. Comparison between Two Inversion Techniques
    A quantitative comparison between the Milne-Eddington (ME) inversion technique implemented by Skumanich & Lites and the SIR (Stokes Inversion based on Response...
  • Publicación
    Physical properties of a sunspot chromosphere with umbral flashes
    We present new high-resolution spectro-polarimetric Ca IIλ8542 observations of umbral flashes in sunspots. At nearly 0.18 arcsec, and spanning about one hour of...
  • Charla
    Physical properties of asteroid surfaces 1: Introduction to asteroid UV-VIS-NIR spectrometry
    Series: XXVIII Canary Islands Winter School of Astrophysics: Solar System Exploration Topic: Physical Properties of Asteroid Surfaces Lecture 1: Introduction to...
  • Charla
    Physical properties of asteroid surfaces 2: Novel spectrometric modeling
    Series: XXVIII Canary Islands Winter School of Astrophysics: Solar System Exploration Topic: Physical Properties of Asteroid Surfaces Lecture 2: Novel...
  • Publicación
    Physical Properties of the Solar Magnetic Photosphere under the MISMA Hypothesis. I. Description of the Inversion Procedure
    The paper describes an automatic inversion code to recover microstructured magnetic atmospheres (MISMAs) by fitting Stokes profiles. These solar model...
  • Publicación
    Physical Properties of the Solar Magnetic Photosphere under the MISMA Hypothesis. II. Network and Internetwork Fields at the Disk Center
    This paper is the second in a series that models photospheric magnetic structures in terms of atmospheres having optically thin fluctuations of magnetic field...
  • Charla
    Planetary Atmospheres 2: Radiative Transfer, Composition, and Clouds
    Series: XXVIII Canary Islands Winter School of Astrophysics: Solar System Exploration Topic: Planetary Atmospheres. Lecture 2: Radiative transfer, composition...
  • Publicación
    Polarized resonance line transfer in a spherically symmetric medium with angle-dependent partial frequency redistribution
    In a stellar atmosphere, the resonance line polarization arises from scattering of limb-darkened radiation field by atoms. This spectral line polarization gets...
  • Publicación
    PORTA: A three-dimensional multilevel radiative transfer code for modeling the intensity and polarization of spectral lines with massively parallel computers
    The interpretation of the intensity and polarization of the spectral line radiation produced in the atmosphere of the Sun and of other stars requires solving a...