Add to ORKGWe present the initial results from our GALEX program designed to obtain ultraviolet (UV) spectra of...
We present first results on the quantitative spectroscopic analysis of the photospheric-phase of typ...
We present a set of nonlocal thermodynamic equilibrium steady-state calculations of radiative transf...
We present detailed NLTE spectral synthesis models of the Type II supernova 2005cs, which occurred i...
Massive stars live fast and die young. They shine furiously for a few million years, during which ti...
I have modeled the spectra of Type Ia supernovae with a detailed, non-local thermodynamic equilibriu...
We have calculated fast direct spectral model fits to two early-time spectra of the Type II plateau ...
Radiation transport codes are often used in astrophysics to construct spectral models. In this work,...
Massive stars live fast and die young. They shine furiously for a few million years, during which ti...
The explosive deaths of stars, known as a supernovae (SNe), have been critical to our understanding ...
International audienceNebular phase spectra of core-collapse supernovae (SNe) provide critical and u...
Utilizing non-local thermodynamic equilibrium time-dependent radiative-transfer calculations, we inv...
The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important both in...
International audienceWe present a set of nonlocal thermodynamic equilibrium steady-state calculatio...
International audienceWe present a set of nonlocal thermodynamic equilibrium steady-state calculatio...
We present the initial results from our GALEX program designed to obtain ultraviolet (UV) spectra of...
We present first results on the quantitative spectroscopic analysis of the photospheric-phase of typ...
We present a set of nonlocal thermodynamic equilibrium steady-state calculations of radiative transf...
We present detailed NLTE spectral synthesis models of the Type II supernova 2005cs, which occurred i...
Massive stars live fast and die young. They shine furiously for a few million years, during which ti...
I have modeled the spectra of Type Ia supernovae with a detailed, non-local thermodynamic equilibriu...
We have calculated fast direct spectral model fits to two early-time spectra of the Type II plateau ...
Radiation transport codes are often used in astrophysics to construct spectral models. In this work,...
Massive stars live fast and die young. They shine furiously for a few million years, during which ti...
The explosive deaths of stars, known as a supernovae (SNe), have been critical to our understanding ...
International audienceNebular phase spectra of core-collapse supernovae (SNe) provide critical and u...
Utilizing non-local thermodynamic equilibrium time-dependent radiative-transfer calculations, we inv...
The evolution of massive stars, as well as their endpoints as supernovae (SNe), is important both in...
International audienceWe present a set of nonlocal thermodynamic equilibrium steady-state calculatio...
International audienceWe present a set of nonlocal thermodynamic equilibrium steady-state calculatio...
We present the initial results from our GALEX program designed to obtain ultraviolet (UV) spectra of...
We present first results on the quantitative spectroscopic analysis of the photospheric-phase of typ...
We present a set of nonlocal thermodynamic equilibrium steady-state calculations of radiative transf...