S. Owocki

Publications388
h-index49
Citations8,281
Highly Influential Citations563
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Dynamical Simulations of Magnetically Channeled Line-driven Stellar Winds. I. Isothermal, Nonrotating, Radially Driven Flow
We present numerical magnetohydrodynamic (MHD) simulations of the effect of stellar dipole magnetic fields on line-driven wind outflows from hot, luminous stars. Unlike previous fixed-field analyses,… Expand
Be-star rotation: how close to critical?
We argue that, in general, observational studies of Be-star rotation have paid insufficient attention to the effects of equatorial gravity darkening. We present new line-profile calculations that… Expand
Hydrodynamical Simulations of Corotating Interaction Regions and Discrete Absorption Components in Rotating O-Star Winds
We present two-dimensional hydrodynamical simulations of corotating stream structure in the wind from a rotating O star, together with resulting synthetic line profiles showing discrete absorption… Expand
On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
We suggest that the mass lost during the evolution of very massive stars may be dominated by optically thick, continuum-driven outbursts or explosions, instead of by steady line-driven winds. In… Expand
Time-dependent models of radiatively driven stellar winds. I - Nonlinear evolution of instabilities for a pure absorption model
Numerical radiation-hydrodynamics simulations of the nonlinear evolution of instabilities in radiatively driven stellar winds have been performed. The results show a strong tendency for the unstable… Expand
CHANDRA HETGS MULTIPHASE SPECTROSCOPY OF THE YOUNG MAGNETIC O STAR theta^1 ORIONIS C
We report on four Chandra grating observations of the oblique magnetic rotator � 1 Ori C (O5.5 V), covering a wide range of viewing angles with respect to the star’s 1060 G dipole magnetic field. We… Expand
The outer evolution of instability-generated structure in radiatively driven stellar winds
We investigate stochastic structure in hot-star winds. The structure (i.e. inhomogeneities such as clumps and shocks) is generated by the instability of the line driving mechanism in the inner wind.… Expand
Dynamical simulations of magnetically channelled line-driven stellar winds - III. Angular momentum loss and rotational spin-down
We examine the angular momentum loss and associated rotational spin-down for magnetic hot stars with a line-driven stellar wind and a rotation-aligned dipole magnetic field. Our analysis here is… Expand
A POROSITY-LENGTH FORMALISM FOR PHOTON-TIRING-LIMITED MASS LOSS FROM STARS ABOVE THE EDDINGTON LIMIT
We examine radiatively driven mass loss from stars near and above the Eddington limit. Building on the standard CAK theory of driving by scattering in an ensemble of lines with a power-law… Expand
A magnetic confinement versus rotation classification of massive-star magnetospheres
Building on results from the Magnetism in Massive Stars (MiMeS) project, this paper shows how a two-parameter classification of massive-star magnetospheres in terms of the magnetic wind confinement… Expand
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