Luminous Blue Variables & Mass Loss near the Eddington Limit

  title={Luminous Blue Variables \& Mass Loss near the Eddington Limit},
  author={Stanley P. Owocki and A. J. van Marle},
  journal={Proceedings of the International Astronomical Union},
  pages={71 - 82}
  • S. OwockiA. J. Marle
  • Published 1 December 2007
  • Physics
  • Proceedings of the International Astronomical Union
Abstract During the course of their evolution, massive stars lose a substantial fraction of their initial mass, both through steady winds and through relatively brief eruptions during their Luminous Blue Variable (LBV) phase. This talk reviews the dynamical driving of this mass loss, contrasting the line-driving of steady winds to the potential role of continuum driving for eruptions during LBV episodes when the star exceeds the Eddington limit. A key theme is to emphasize the inherent limits… 
3 Citations

Numerical simulations of continuum-driven winds of super-Eddington stars

We present the results of numerical simulations of continuum-driven winds of stars that exceed the Eddington limit and compare these against predictions from earlier analytical solutions. Our models



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

Mass and Kinetic Energy of the Homunculus Nebula around η Carinae

We examine thermal infrared images of η Car at wavelengths from 4.8 to 25 μm obtained with the MIRAC3 camera system at the Magellan Observatory, and we conclude that η Car's circumstellar Homunculus

The Porous Atmosphere of η Carinae

  • N. Shaviv
  • Physics
    The Astrophysical journal
  • 2000
It is shown that by using the classical stellar atmosphere and wind theory, it is impossible to construct a consistent wind model in which a sufficiently small amount of mass is shed to drive a thick wind with a mass-loss rate substantially higher than the observed one.

Line Forces in Keplerian Circumstellar Disks and Precession of Nearly Circular Orbits

We examine the effects of optically thick line forces on orbiting circumstellar disks, such as occur around Be stars. For radially streaming radiation (e.g., as from a point source), line forces are

Dissecting the Homunculus nebula around Eta Carinae with spatially resolved near-infrared spectroscopy

Near-infrared emission lines are unique diagnostics of the geometry, structure, kinematics, and excitation of the circumstellar ejecta of η Carinae, and give clues to the nature of its wind. The

The Nature of the Radiative Hydrodynamic Instabilities in Radiatively Supported Thomson Atmospheres

Atmospheres having a significant radiative support are shown to be intrinsically unstable at luminosities above a critical fraction Γcrit ≈ 0.5-0.85 of the Eddington limit, with the exact value

The Arches Cluster Mass Function

We have analyzed H- and Ks-band images of the Arches cluster obtained using the NIRC2 instrument on Keck with the laser guide star adaptive optics (LGS AO) system. With the help of the LGS AO system,

The Eddington Luminosity Limit for Multiphased Media

We consider the effective Eddington luminosity in a locally inhomogeneous medium by averaging out the coarse, small-scale behavior. We show that the ratio between the emitted flux and the average

Statistical Confirmation of a Stellar Upper Mass Limit

We derive the expectation value for the maximum stellar mass (mmax) in an ensemble of N stars, as a function of the initial mass function (IMF) upper mass cutoff (mup) and N. We statistically