Add to ORKGAbstract. We present a moving periodic box technique to study the outer-wind evolution of instability-generated structure in hot-star winds. This has considerable computational and conceptual advantages 1
We report initial results of two-dimensional simulations of the nonlinear evolution of the line-dri...
Radiatively driven winds are a key component in a number of astrophysical settings, most notably the...
We investigate the flow's structure properties due to the mass transfer in binaries with a cool star...
The line-driven instability of hot-star winds is understood to lead to extensive clumped structure i...
We investigate stochastic structure in hot-star winds. The structure (i.e. inhomogeneities such as c...
We present an efficient technique to study the 1D evolution of instability-generated structure in wi...
Clumps in hot star winds can originate from shock compression due to the line driven insta-bility. O...
We investigate the effects of stellar limb-darkening and photospheric perturbations for the onset of...
The inner parsec of our Galaxy contains tens of Wolf–Rayet stars whose powerful outflows are constan...
It is now well established that stellar winds of hot stars are fragmentary and that the X-ray emissi...
Context. Clumping in the radiation-driven winds of hot, massive stars arises naturally due to the st...
The feedback form pre-main sequence and young stars influences their vicinity. The stars are formed ...
A numerical hydrodynamics code is used to investigate two aspects of the winds of hot stars. The fir...
The hottest and most massive stars (spectral types O, B, Wolf-Rayet) have strong stellar winds that ...
Low- and intermediate mass stars move up the asymptotic giant branch (AGB) as they reach the end of ...
We report initial results of two-dimensional simulations of the nonlinear evolution of the line-dri...
Radiatively driven winds are a key component in a number of astrophysical settings, most notably the...
We investigate the flow's structure properties due to the mass transfer in binaries with a cool star...
The line-driven instability of hot-star winds is understood to lead to extensive clumped structure i...
We investigate stochastic structure in hot-star winds. The structure (i.e. inhomogeneities such as c...
We present an efficient technique to study the 1D evolution of instability-generated structure in wi...
Clumps in hot star winds can originate from shock compression due to the line driven insta-bility. O...
We investigate the effects of stellar limb-darkening and photospheric perturbations for the onset of...
The inner parsec of our Galaxy contains tens of Wolf–Rayet stars whose powerful outflows are constan...
It is now well established that stellar winds of hot stars are fragmentary and that the X-ray emissi...
Context. Clumping in the radiation-driven winds of hot, massive stars arises naturally due to the st...
The feedback form pre-main sequence and young stars influences their vicinity. The stars are formed ...
A numerical hydrodynamics code is used to investigate two aspects of the winds of hot stars. The fir...
The hottest and most massive stars (spectral types O, B, Wolf-Rayet) have strong stellar winds that ...
Low- and intermediate mass stars move up the asymptotic giant branch (AGB) as they reach the end of ...
We report initial results of two-dimensional simulations of the nonlinear evolution of the line-dri...
Radiatively driven winds are a key component in a number of astrophysical settings, most notably the...
We investigate the flow's structure properties due to the mass transfer in binaries with a cool star...