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DTSTAMP:20190719T085744Z
LOCATION:HG E 1.1
DTSTART;TZID=Europe/Stockholm:20190612T170000
DTEND;TZID=Europe/Stockholm:20190612T173000
UID:submissions.pasc-conference.org_PASC19_sess162_msa200@linklings.com
SUMMARY:Aspects of Multi-Dimensional Radiation Transfer in Stellar Atmosph
 eres
DESCRIPTION:Minisymposium\nComputer Science and Applied Mathematics, Physi
 cs\n\nAspects of Multi-Dimensional Radiation Transfer in Stellar Atmospher
 es\n\nSteiner\n\nRadiative transfer (RT) computations are the bread and bu
 tter of astrophysical research. One can arguably divide RT tasks into thre
 e categories. First, RT occurs as part of the energy equation in numerical
  simulations of stellar atmosphere. In this case, details of the spectrum 
 are less important than the energy transported by radiation. Yet, effects 
 of the entirety of spectral lines may need to be taken into account. Since
  RT is carried out in each time step across the entire computational domai
 n, it must be done highly efficiently. Second, the production of virtual s
 pectroscopic and polarimetric observations from numerical models asks for 
 precise RT calculation of single spectral lines or broad band filters. Dep
 arture from local thermal equilibrium, or departure from exact coherence b
 etween absorbed and emitted photons (partial redistribution), or magnetic 
 fields, etc. must possibly be incorporated into the RT. This can amount to
  a massive computational task for the production of two-dimensional intens
 ity maps from even one single snapshot of a three-dimensional simulation. 
 Third, there is computationally intensive RT needed for inversion procedur
 es. By inversion we mean the derivation of the atmospheric structure from 
 RT analysis of single or multiple spectral lines and/or Stokes profiles.
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