Radiative transfer simulations
Our research revolves around the theoretical description of atmospheres along with their corresponding radiation fields. In order to compute both with increasing level of detail and resolution, we are developing the PHOENIX code.
Scientists who would like to use our models can download individual ones or full grids either from our local archive or from our collaborators in Göttingen. Those with a worthwhile idea that requires more specialized data should feel free contact us, of course.
What is PHOENIX?
PHOENIX is a general-purpose state-of-the-art radiative transfer code. Its purpose is to calculate atmospheres and spectra of stars all across the HR-diagram. Across its 30 years of continuous development, it has been expanded to describe a multitude of objects, ranging from main sequence stars and irradiated planets across TTauri stars and disks up to expanding shells of novae and supernovae. Out of necessity, the code is highly trimmed for efficiency, with enormous attention devoted to massively parallel computing performance.
What does it do?
The code can be run in two vastly different flavours.
The 1D mode is designed to compute a fully consistent, vertical atmospheric slice, involving the hydrostatic stratification, gas chemistry, radiative transfer and temperature correction and can take into account a range of potentially important effects, such as NLTE, time-dependence, winds, and clouds. The highly optimized and short runtime of the 1D mode lends itself to produce large scale model grids or high resolution models.
The 3D mode blows up the details of the 1D mode by two additional dimension, which can be employed to compute either a lowly resolved full star in a box or a highly resolved, box within a star. Both configurations lend themselves to import detailed hydrodynamic simulations as hydro-structures for the follow-up chemistry and radiative transfer computation. Given current lack in computational power, no feedback-loop between a hydrodynamic code and PHOENIX has been implemented, yet, which prevents a proper relaxation of 3D models for now. The 3D mode nonetheless provides research opportunities that 1D runs fail, as for instance the study of star spots, irraditated global circulation atmospheres or transmission / reflection spectra.
We apologize to all developers we might have missed in the list below, in particular to Eddies former students. We intend to get this list up to date. Please get in touch with us!
Current development version (v18) collaborators
Earlier version (v15 or earlier) collaborators
Assistant research professor at Belgrade Astronomical Observatory
Where can I get the models?
We maintain a local archive for downloading with all available model data including ancient historial stuff and experimental pre-release material.
Of course, you might always get in touch with us if you have a worthwhile project in mind that the vanilla model grids are unable to cover.