S. P. Owocki
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View article: A generalized semi-analytic model for the combined outflow from a cluster of stars with strong stellar winds
A generalized semi-analytic model for the combined outflow from a cluster of stars with strong stellar winds Open
We derive semi-analytic solutions for the thermally driven cumulative outflow from a dense stellar cluster that consists of a large number of stars with strong stellar winds, under the key assumption that their mass and energy deposition c…
View article: Wind and Eruptive Mass Loss near the Eddington Limit
Wind and Eruptive Mass Loss near the Eddington Limit Open
Luminous, hot, massive stars can lose mass both through quasi-steady winds driven by line-scattering of the star’s continuum luminosity, and through transient eruptions identified as Luminous Blue Variables (LBVs). This paper compares and …
View article: A generalized semi-analytic model for the combined outflow from a cluster of stars with strong stellar winds
A generalized semi-analytic model for the combined outflow from a cluster of stars with strong stellar winds Open
We derive semi-analytic solutions for the thermally driven cumulative outflow from a dense stellar cluster that consists of a large number of stars with strong stellar winds, under the key assumption that their mass and energy deposition c…
View article: Discovery of the binary nature of the magnetospheric B-type star <i>ρ</i> Oph A
Discovery of the binary nature of the magnetospheric B-type star <i>ρ</i> Oph A Open
Context . The nearby B-type star ρ Oph A was recently identified as a rapidly rotating magnetic B-type star with variable radio and X-ray emission consistent with a magnetospheric origin. Aims . We aim to refine constraints on ρ Oph A’s ma…
View article: The effect of collisional cooling of energetic electrons on radio emission from the centrifugal magnetospheres of magnetic hot stars
The effect of collisional cooling of energetic electrons on radio emission from the centrifugal magnetospheres of magnetic hot stars Open
This paper extends our previous study of the gyro-emission by energetic electrons in the magnetospheres of rapidly rotating, magnetic massive stars, through a quantitative analysis of the role of cooling by Coulomb collisions with thermal …
View article: On the spatial distribution of electron energy loss due to gyro-cooling in hot star magnetospheres
On the spatial distribution of electron energy loss due to gyro-cooling in hot star magnetospheres Open
Hot magnetic stars often exhibit incoherent circularly polarized radio emission thought to arise from gyro-synchrotron emission by energetic electrons trapped in the circumstellar magnetosphere. Theoretical scalings for electron accelerati…
View article: MOBSTER -- VII. Using light curves to infer magnetic and rotational properties of stars with centrifugal magnetospheres
MOBSTER -- VII. Using light curves to infer magnetic and rotational properties of stars with centrifugal magnetospheres Open
Early-type B stars with strong magnetic fields and rapid rotation form centrifugal magnetospheres (CMs), as the relatively weak stellar wind becomes magnetically confined and centrifugally supported above the Kepler co-rotation radius. CM …
View article: 3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field
3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field Open
We present results from new self-consistent 3D magnetohydrodynamics (MHD) simulations of the magnetospheres from massive stars with a dipole magnetic axis that has a non-zero obliquity angle (β) to the star’s rotation axis. As an initial d…
View article: 3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field
3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field Open
We present results from new self-consistent 3D MHD simulations of the magnetospheres from massive stars with a dipole magnetic axis that has a non-zero obliquity angle ($β$) to the star's rotation axis. As an initial direct application, we…
View article: Winds and magnetospheres of stars and planets: similarities and differences
Winds and magnetospheres of stars and planets: similarities and differences Open
Both stars and planets can lose mass through an expansive wind outflow, often constrained or channeled by magnetic fields that form a surrounding magnetosphere. The very strong winds of massive stars are understood to be driven by line-sca…
View article: Magnetically confined wind shock
Magnetically confined wind shock Open
Many stars across all classes possess strong enough magnetic fields to influence dynamical flow of material off the stellar surface. For the case of massive stars (O and B types), about 10\% of them harbour strong, globally ordered (mostly…
View article: Obliquely Rotating Massive Star Magnetospheres
Obliquely Rotating Massive Star Magnetospheres Open
We present results from 3D MHD simulations of the magnetospheres from massive stars with a dipole magnetic axis that has an arbitrary obliquity angle ( β ) to the stars rotation axis. As an initial direct application, we examine the global…
View article: Method and new tabulations for flux-weighted line-opacity and radiation line-force in supersonic media: Tables
Method and new tabulations for flux-weighted line-opacity and radiation line-force in supersonic media: Tables Open
The table presented gives the line strength distribution parameters \alpha, \bar{Q}, Q_0 and Thompson scattering mass absorption coefficient \kappa_e. Each of these parameters is given as a function of mass density \rho and temperature T…
View article: Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars
Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars Open
Magnetic B-stars often exhibit circularly polarized radio emission thought to arise from gyrosynchrotron emission by energetic electrons trapped in the circumstellar magnetosphere. Recent empirical analyses show that the onset and strength…
View article: Getting started: How a supersonic stellar wind is initiated from a hydrostatic surface
Getting started: How a supersonic stellar wind is initiated from a hydrostatic surface Open
Most of a star's mass is bound in a hydrostatic equilibrium in which pressure balances gravity. But if at some near-surface layer additional outward forces overcome gravity, this can transition to a supersonic, outflowing wind, with the so…
View article: MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars
MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars Open
Numerous magnetic hot stars exhibit gyrosynchrotron radio emission. The source electrons were previously thought to be accelerated to relativistic velocities in the current sheet formed in the middle magnetosphere by the wind opening magne…
View article: Electron scattering emission in the light curves of stars with centrifugal magnetospheres
Electron scattering emission in the light curves of stars with centrifugal magnetospheres Open
Strongly magnetic, rapidly rotating B-type stars with relatively weak winds form centrifugal magnetospheres (CMs), as the stellar wind becomes magnetically confined above the Kepler co-rotation radius. Approximating the magnetic field as a…
View article: Ultraviolet Spectropolarimetry with Polstar: Clumping and Mass-loss Rate Corrections
Ultraviolet Spectropolarimetry with Polstar: Clumping and Mass-loss Rate Corrections Open
The most massive stars are thought to lose a significant fraction of their mass in a steady wind during the main-sequence and blue supergiant phases. This in turn sets the stage for their further evolution and eventual supernova, with cons…
View article: Can Magnetospheric Scattering Explain Inferred Emission in Photometric Light Curves of σ Ori E and Magnetic Stars Observed with TESS?
Can Magnetospheric Scattering Explain Inferred Emission in Photometric Light Curves of σ Ori E and Magnetic Stars Observed with TESS? Open
σ Ori E is a prototypical magnetic B star with a rapid 1.2 day rotation period. Two dips in brightness can be seen in its photometric light curve, which was well fit by the Rigidly Rotating Magnetosphere (RRM) model. This model shows that …
View article: H-alpha Emission as a Diagnostic of Plasma Transport Mechanics in Centrifugal Magnetospheres
H-alpha Emission as a Diagnostic of Plasma Transport Mechanics in Centrifugal Magnetospheres Open
Approximately one quarter of magnetic early (B5-B0) B-type type stars display Balmer line emission originating in centrifugal magnetospheres (CMs). Indeed, the CMs of these stars are uniquely detectable in all available magnetospheric diag…
View article: Winds and magnetospheres from stars and planets: similarities and differences
Winds and magnetospheres from stars and planets: similarities and differences Open
Both stars and planets can lose mass through an expansive wind outflow, often constrained or channeled by magnetic fields that form a surrounding magnetosphere. The very strong winds of massive stars are understood to be driven by line-sca…
View article: Detection of an extremely strong magnetic field in the double-degenerate binary merger product HD 144941
Detection of an extremely strong magnetic field in the double-degenerate binary merger product HD 144941 Open
HD 144941 is an extreme He (EHe) star, a rare class of subdwarf OB star formed from the merger of two white dwarf (WD) stars. Uniquely amongst EHe stars, its light curve has been reported to be modulated entirely by rotation, suggesting th…
View article: Simulating the formation of η Carinae’s surrounding nebula through unstable triple evolution and stellar merger-induced eruption
Simulating the formation of η Carinae’s surrounding nebula through unstable triple evolution and stellar merger-induced eruption Open
η Carinae is an extraordinary massive star famous for its 19th century Great Eruption and the surrounding Homunculus nebula ejected in that event. The cause of this eruption has been the centre of a long-standing mystery. Recent observatio…
View article: Modelling Eta Carinae's Great Eruption and its surrounding nebula
Modelling Eta Carinae's Great Eruption and its surrounding nebula Open
$\eta$ Carinae is an extraordinary massive star famous for its 19th century Great Eruption and the surrounding Homunculus nebula ejected in that event. The cause of this eruption has been the centre of a long-standing mystery. Recent obser…
View article: Getting started: How a supersonic stellar wind is initiated from a hydrostatic surface
Getting started: How a supersonic stellar wind is initiated from a hydrostatic surface Open
Most of a star’s mass is bound in a hydrostatic equilibrium in which pressure balances gravity. But if at some near-surface layer additional outward forces overcome gravity, this can transition to a supersonic, outflowing wind, with the so…
View article: The magnetic early B-type stars – IV. Breakout or leakage? H α emission as a diagnostic of plasma transport in centrifugal magnetospheres
The magnetic early B-type stars – IV. Breakout or leakage? H α emission as a diagnostic of plasma transport in centrifugal magnetospheres Open
Rapidly rotating early-type stars with strong magnetic fields frequently show H α emission originating in centrifugal magnetospheres (CMs), circumstellar structures in which centrifugal support due to magnetically enforced corotation of th…
View article: Line-drag damping of Alfvén waves in radiatively driven winds of magnetic massive stars
Line-drag damping of Alfvén waves in radiatively driven winds of magnetic massive stars Open
Line-driven stellar winds from massive (OB) stars are subject to a strong line-deshadowing instability. Recently, spectropolarimetric surveys have collected ample evidence that a subset of Galactic massive stars hosts strong surface magnet…
View article: How the breakout-limited mass in B-star centrifugal magnetospheres controls their circumstellar H α emission
How the breakout-limited mass in B-star centrifugal magnetospheres controls their circumstellar H α emission Open
Strongly magnetic B-type stars with moderately rapid rotation form ‘centrifugal magnetospheres’ (CMs) from the magnetic trapping of stellar wind material in a region above the Kepler co-rotation radius. A long-standing question is whether …
View article: The effects of surface fossil magnetic fields on massive star evolution – II. Implementation of magnetic braking in mesa and implications for the evolution of surface rotation in OB stars
The effects of surface fossil magnetic fields on massive star evolution – II. Implementation of magnetic braking in mesa and implications for the evolution of surface rotation in OB stars Open
The time evolution of angular momentum and surface rotation of massive stars are strongly influenced by fossil magnetic fields via magnetic braking. We present a new module containing a simple, comprehensive implementation of such a field …
View article: PolStar -- An Explorer-Class FUV Spectropolarimetry Mission to Map the Environments of Massive Stars
PolStar -- An Explorer-Class FUV Spectropolarimetry Mission to Map the Environments of Massive Stars Open
PolStar is an Explorer-class far ultraviolet (FUV) spectropolarimetry mission designed to target massive stars and their environments. PolStar will take advantage of resonance lines only available in the FUV to measure for the first time t…