An Improved Line-Strength Parameterization in Hot-Star Winds

Gayley, K. G.

doi:10.1086/176492

Cited by 139 publications

(186 citation statements)

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“…However, numerical tests showed that this phenomenon can be neglected for most considered levels (see also Lamers & Morton 1976). Moreover, there would not be any radiatively driven wind if the opposite is true since radiatively driven stellar wind is enabled by high transition rates P i j (Gayley 1995). On the other hand, at first sight it is not clear whether this assumption is also fulfilled in the case of strong wind-shocks.…”

Section: Discussionmentioning

confidence: 99%

“…Clearly, such a complicated situation cannot be adequately described by models with a temperatureindependent radiative force, or with a radiative force artificially depending on wind temperature via the thermal velocity as has been done, e.g., by KKII. Note that the artificial dependence on the thermal velocity may be removed using an alternative description of the radiative force by Gayley (1995).…”

Section: Introductionmentioning

confidence: 99%

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NLTE models of line-driven stellar winds

Krtička

Kubát

2004

A&A

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Abstract. New numerical models of line-driven stellar winds of late O stars are presented. Statistical equilibrium (NLTE) equations of the most abundant elements are solved. Properly obtained occupation numbers are used to calculate consistent radiative force and radiative heating terms. Wind density, velocity and temperature are calculated as a solution of model hydrodynamical equations. Contrary to other published models we account for a multicomponent wind nature and do not simplify the calculation of the radiative force (e.g. using force multipliers). We discuss the convergence behaviour of our models. The ability of our models to predict correct values of mass-loss rates and terminal velocities of selected late O stars (mainly giants and supergiants) is demonstrated. The systematic difference between predicted and observed terminal velocities reported in the literature has been removed. Moreover, we found good agreement between the theoretical wind momentum-luminosity relationship and the observed one for Cyg OB2 supergiants.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

NLTE models of line-driven stellar winds

Krtička

Kubát

2004

A&A

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“…1, is that the X-ray differential emission measure (DEM) is very sensitive to changes in the mass-loss rate, as parametrized via theQ introduced by Gayley (1995) to characterize the overall opacity available for line driving in the Castor, Abbott & Klein (1975) wind formalism. …”

Section: Rfhd Analysismentioning

confidence: 99%

Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

et al. 2010

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Abstract. We present Rigid Field Hydrodynamic simulations of the magnetosphere of σ Ori E. We find that the X-ray emission from the star's magnetically confined wind shocks is very sensitive to the assumed mass-loss rate. To compare the simulations against the measured X-ray emission, we first disentangle the star from its recently discovered late-type companion using Chandra HRC-I observations. This then allows us to place an upper limit on the mass-loss rate of the primary, which we find to be significantly smaller than previously imagined.

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“…where the notation follows Owocki (2004), and in particularQ is a measure of the total line opacity in the wind, in units of the electron scattering opacity κ e (see Gayley 1995). The term in parentheses is the reciprocal of the Sobolev optical depth; through the appearance of the spatial velocity gradient dv/dr, it represents the degree to which the wind is able to Doppler-shift the lines out of their own shadow.…”

Section: Line-driven Windsmentioning

confidence: 99%

Modeling the winds and magnetospheres of active OB stars

Townsend

2010

Proc. IAU

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Abstract. After briefly reviewing the theory behind the radiative line-driven winds of OB stars, I examine the processes that can generate structure in them; these include both intrinsic instabilities, and surface perturbations such as pulsation and rotation. I then delve into wind channeling and confinement by magnetic fields as a mechanism for forming longer-lived circumstellar structures. With a narrative that largely follows the historical progression of the field, I introduce the key insights and results that link the first detection of a magnetosphere, over three decades ago, to the recent direct measurement of magnetic braking in a number of active OB stars.

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An Improved Line-Strength Parameterization in Hot-Star Winds

Cited by 139 publications

References 0 publications

NLTE models of line-driven stellar winds

NLTE models of line-driven stellar winds

Rigid Field Hydrodynamic simulations of the magnetosphere of σ Orionis E

Modeling the winds and magnetospheres of active OB stars

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