EDP Sciences
Free access
Volume 498, Number 3, May II 2009
Page(s) 987 - 992
Section Numerical methods and codes
DOI http://dx.doi.org/10.1051/0004-6361/200911681
Published online 19 March 2009
A&A 498, 987-992 (2009)
DOI: 10.1051/0004-6361/200911681

A 3D radiative transfer framework

V. Homologous flows
E. Baron1, 2, 3, P. H. Hauschildt1, and B. Chen2

1  Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany
    e-mail: yeti@hs.uni-hamburg.de
2  Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W Brooks, Rm 100, Norman, OK 73019-2061 USA
    e-mail: baron@ou.edu
3  Computational Research Division, Lawrence Berkeley National Laboratory, MS 50F-1650, 1 Cyclotron Rd, Berkeley, CA 94720 USA

Received 19 January 2009 / Accepted 6 March 2009

Context. Observations and theoretical calculations have shown the importance of non-spherically symmetric structures in supernovae. Thus, the interpretation of observed supernova spectra requires the ability to solve the transfer equation in 3-D moving atmospheres.
Aims. We present an implementation of the solution of the radiative transfer equation in 3-D homologously expanding atmospheres in spherical coordinates. The implementation is exact to all orders in v/c.
Methods. We use the methods that we have developed in previous papers in this series as well as a new affine method that makes use of the fact that photons travel on straight lines. The affine method greatly facilitates delineating the characteristics and can be used in the case of strong-gravitational and arbitrary-velocity fields.
Results. We compare our results in 3-D for spherically symmetric test problems with high velocity fields (up to 87% of the speed of light) and find excellent agreement, when the number of momentum space angles is high. Our well-tested 1-D results are based on methods where the momentum directions vary along the characteristic (co-moving momentum directions). Thus, we are able to verify both the analytic framework and its numerical implementation. Additionally, we have been able to test the parallelization over characteristics. Using 5122 momentum angles we ran the code on 16 384 Opteron processors and achieved excellent scaling.
Conclusions. It is now possible to calculate synthetic spectra from realistic 3D hydro simulations. This should open an era of progress in hydro modeling, similar to that that occurred in the 1980s when 1-D models were confronted with synthetic spectra.

Key words: radiative transfer -- relativity -- stars: supernovae: general

© ESO 2009