Add to ORKGAbstract. We developed a numerical method for a solution of the radia-tive transfer equation in axial symmetry. The transfer problem is solved using the \extended " short characteristic method in individual planes in-tersecting the star. This geometry allows us to include the deformation of the star due to a rotation and an asymmetry of the stellar wind. We also include the velocity eld to the solution of the problem to enable studies of hot Be stars with a stellar wind. 1
Aims.This paper describes a code which is capable of modeling axisymmetric stellar winds. Me...
The discretization of the multi-dimensional radiative transfer equation results in a very large line...
The 3D radiative transfer equation is written in O(#nu#/c) in the comoving frame and solved by a sho...
We present a method for solving the radiative transfer equation in axial symmetry both in static cas...
We present our multidimensional radiative transfer code. The problem is solved in the axial symmetry...
We come back to the analytical solution of the standard transfer problem in a stellar atmosphere. It...
The theory of radiation driven wind including stellar rotation is re-examined. After a suitable chan...
This paper contains the calculation of the tangential component of the velocity for a model of galax...
Context. State of the art quantitative spectroscopy utilizes synthetic spectra to extract informatio...
The radiative heat transfer equation in a participating medium is a Fredholm integral equation of th...
Abstract. The observational effects of rotation on outflows in OB stars are reviewed. Direct evidenc...
In this paper the methods developed in earlier papers are extended to solving the problem of radiati...
Context. Knowledge about hot, massive stars is usually inferred from quantitative spectroscopy. To a...
. The discretization of the multi--dimensional radiative transfer equation results in a very large l...
The purpose of this paper is to improve the modelization of the rotational mixing which occurs in st...
Aims.This paper describes a code which is capable of modeling axisymmetric stellar winds. Me...
The discretization of the multi-dimensional radiative transfer equation results in a very large line...
The 3D radiative transfer equation is written in O(#nu#/c) in the comoving frame and solved by a sho...
We present a method for solving the radiative transfer equation in axial symmetry both in static cas...
We present our multidimensional radiative transfer code. The problem is solved in the axial symmetry...
We come back to the analytical solution of the standard transfer problem in a stellar atmosphere. It...
The theory of radiation driven wind including stellar rotation is re-examined. After a suitable chan...
This paper contains the calculation of the tangential component of the velocity for a model of galax...
Context. State of the art quantitative spectroscopy utilizes synthetic spectra to extract informatio...
The radiative heat transfer equation in a participating medium is a Fredholm integral equation of th...
Abstract. The observational effects of rotation on outflows in OB stars are reviewed. Direct evidenc...
In this paper the methods developed in earlier papers are extended to solving the problem of radiati...
Context. Knowledge about hot, massive stars is usually inferred from quantitative spectroscopy. To a...
. The discretization of the multi--dimensional radiative transfer equation results in a very large l...
The purpose of this paper is to improve the modelization of the rotational mixing which occurs in st...
Aims.This paper describes a code which is capable of modeling axisymmetric stellar winds. Me...
The discretization of the multi-dimensional radiative transfer equation results in a very large line...
The 3D radiative transfer equation is written in O(#nu#/c) in the comoving frame and solved by a sho...