Editorial Technical Support:
D. H. Diaz
M. A. Gomez
Editorial management and production:
SOLGRAF Editora firstname.lastname@example.org
Dennis Jack , Peter H. Hauschildt and Ed Baron
We will present an overview of the general-purpose stellar and planetary atmosphere code PHOENIX. With PHOENIX one can calculate model atmospheres and spectra of stars all across the HR-diagram including main sequence stars, giants, white dwarfs, stars with winds, TTauri stars, novae, supernovae, brown dwarfs and extrasolar giant planets. To be able to compute models of such different types of astrophysical objects many different types of physical processes need to be included in model atmosphere codes like PHOENIX. Most of the work with PHOENIX has been done by assuming the model atmospheres of the astrophysical objects to be one di- mensional. Recent progress in computer science now allows for the development of a 3D stellar and planetary atmosphere code. We will present the recent achievements in the development of our 3D radiative transfer framework. We are able to solve the radiative transfer for given atmospheric structures of a stellar or planetary object in different geometries like Cartesian, spherical and cylindrical coordinate systems. We will also present the most recent extension of a time-dependent treatment of the radiative transfer equation in detail.
computational physics and chemistry, radiative transfer, numerical methods.
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 HAUSCHILDT, BARMAN, BARON & ALLARD. 2003. Temperature Correction Methods, Stellar Atmosphere Modeling. ASP Confer- ence Proceedings, Vol. 288: 227.
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 ALLARD, NF, ALLARD F, HAUSCHILDT, KIELKOPF & MACHIN. 2003. A new model for brown dwarf spectra including accurate uni- fied line shape theory for the Na I and K I resonance line profiles. A&A, 411: L473–L476.
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 JACK, HAUSCHILDT & BARON. 2012. Near-infrared light curves of type Ia supernovae. A&A, 538: A132.
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