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

@article{Shaviv2000TheNO,
  title={The Nature of the Radiative Hydrodynamic Instabilities in Radiatively Supported Thomson Atmospheres},
  author={Nir J. Shaviv},
  journal={The Astrophysical Journal},
  year={2000},
  volume={549},
  pages={1093 - 1110}
}
  • N. Shaviv
  • Published 20 October 2000
  • Physics, Environmental Science
  • The Astrophysical Journal
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 depending on the boundary conditions. Two different types of absolute radiation-hydrodynamic instabilities of acoustic waves are found to take place even in the electron scattering-dominated limit. Both instabilities grow over dynamical timescales and both operate on nonradial modes. One is stationary… 

Figures and Tables from this paper

Eddington Limit and Radiative Transfer in Highly Inhomogeneous Atmospheres

Radiation-dominated accretion disks are likely to be subject to the "photon bubble" instability, which may lead to strong density inhomogeneities on scales much shorter than the disk scale height.

Radiation hydrodynamic instability in a plane-parallel, super-Eddington atmosphere: A mechanism for clump formation

In order to understand the physical processes underlying clump formation in outflow from supercritical accretion flow, we performed two-dimensional radiation hydrodynamic (RHD) simulations. We focus

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

Relativistic, Viscous, Radiation Hydrodynamic Simulations of Geometrically Thin Disks. I. Thermal and Other Instabilities

We present results from two-dimensional, general relativistic, viscous, radiation hydrodynamic numerical simulations of Shakura–Sunyaev thin disks accreting onto stellar-mass Schwarzschild black

The Effects of Photon Bubble Instability in Radiation-dominated Accretion Disks

We examine the effects of photon bubble instability in radiation-dominated accretion disks such as those found around black holes in active galactic nuclei and X-ray binary star systems. Two- and

DIRECT NUMERICAL SIMULATION OF RADIATION PRESSURE-DRIVEN TURBULENCE AND WINDS IN STAR CLUSTERS AND GALACTIC DISKS

The pressure exerted by the radiation of young stars may be an important feedback mechanism that drives turbulence and winds in forming star clusters and the disks of starburst galaxies. However,

Instabilities in massive stars

A defining property of massive stars is the dominant, dynamical role played by radiation throughout the stellar interior, atmosphere, and wind. Associated with this radiation hydrodynamics are

ON CONTINUUM-DRIVEN WINDS FROM ROTATING STARS

We study the dynamics of continuum-driven winds from rotating stars and develop an approximate analytical model. We then discuss the evolution of stellar angular momentum, and show that just above

Super-Eddington stellar winds driven by near-surface energy deposition

We develop analytic and numerical models of the properties of super-Eddington stellar winds, motivated by phases in stellar evolution when super-Eddington energy deposition (via, e.g., unstable

The theory of steady‐state super‐Eddington winds and its application to novae

We present a model for steady state winds of systems with super-Eddington luminosities. These radiatively driven winds are expected to be optically thick and clumpy as they arise from an instability

References

SHOWING 1-10 OF 31 REFERENCES

Instabilities in line-driven stellar winds. IV - Linear perturbations in three dimensions

Nonradial wave propagation in line-driven stellar winds is analyzed including both finite disk effects and the line-drag effect of scattered line radiation. Within the local (WKB) analysis the

Instabilities in line-driven stellar winds. I - Dependence on perturbation wavelength

We investigate the stability of absorption-line-driven flows (e.g., as in the winds from hot stars) against small-amplitude velocity perturbations. Our work represents a generalization of previous

On the nature of strange modes in massive stars

This dissertation aims to provide a history of web exceptionalism from 1989 to 2002, a period chosen in order to explore its roots as well as specific cases up to and including the year in which descriptions of “Web 2.0” began to circulate.

Photofluid instabilities of hot stellar envelopes

The instability of radiation-driven stellar winds

The stability of a radiation-driven stellar wind is examined by applying a completely linearized stability analysis to a physically realistic wind model. Three types of instability are found. Both

Photon bubbles - Overstability in a magnetized atmosphere

The formation of 'photon bubbles' in a convectively stable scattering atmosphere supported against gravity entirely by radiation pressure is studied by means of linear stability theory. A simple

Instabilities in line-driven stellar winds. II - Effect of scattering

An earlier analysis (Owocki and Rybicki) of the linear instability of line-driven stellar winds is extended to take proper account of the dynamical effect of scattered radiation. The principal

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.

Variable and Nonspherical Stellar Winds in Luminous Hot Stars: IAU Colloquium 169

The winds of hot stars are generally understood to be driven by the absorption of momentum from the intense stellar radiation field by line transitions in the ultraviolet and farultraviolet regions