The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important
both in astrophysics and cosmology. While tremendous progress towards an understanding …

We have developed a time-dependent non local-thermodynamic-equilibrium radiative
transfer code (CMFGEN) to model supernovae (SNe). With this code we are making …

We incorporate non-thermal excitation and ionization processes arising from non-thermal
electrons that result from γ-ray energy deposition into our radiative transfer code cmfgen …

We describe the difficulties in modeling the spectra and light curves of supernovae (SNe),
and highlight how they differ from modeling stellar atmospheres. SNe evolve in time, and …

Massive stars and supernovae are not only remarkable objects on their own but they are
closely related to many other topics in Astrophysics, such as nucleosynthesis, star formation …

Abstract The code CMFGEN (Hillier & Miller 1998) solves the radiative transfer equation in
the co-moving frame subject to statistical and radiative equilibrium, assuming an expanding …

Massive stars live fast and die young. They shine furiously for a few million years, during
which time they synthesize most of the heavy elements in the universe in their cores. They …

We have developed a radiative transfer code, cmfgen, which allows us to model the spectra
of massive stars and supernovae. Using cmfgen we can derive fundamental parameters …

Supernovae are a rich source of information. By studying their light curves and spectra we
gain insights into stellar evolution, the nature of the progenitor star, surface abundances at …

We present numerical simulations of supernova light curves as compared to two well-
observed supernovae, SN 1999em and SN 1999gi. In this theoretical study, model …