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

@article{Quataert2015SuperEddingtonSW,
title={Super-Eddington stellar winds driven by near-surface energy deposition},
author={Eliot Quataert and Rodrigo Fern{\'a}ndez and Daniel Kasen and Hannah Klion and Bill Paxton},
journal={Monthly Notices of the Royal Astronomical Society},
year={2015},
volume={458},
pages={1214-1233}
}
• Published 21 September 2015
• Physics
• Monthly Notices of the Royal Astronomical Society
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 fusion, wave heating, or a binary companion) heats a region near the stellar surface. This appears to occur in luminous blue variables (LBVs), Type IIn supernovae progenitors, classical novae, and X-ray bursts. We show that when the wind kinetic power exceeds Eddington, the photons are trapped and behave…

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## References

SHOWING 1-10 OF 55 REFERENCES

• Physics
• 2008
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
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
• Physics
• 2009
Observations of transient phenomena in the Universe reveal a spectrum of mass-ejection properties associated with massive stars, covering from Type II/Ib/Ic core-collapse supernovae (SNe) to giant
• Physics, Geology
• 2013
Supernovae (SNe) powered by interaction with circumstellar material provide evidence for intense stellar mass loss during the final years before core collapse. We have argued that during and after
• Physics, Geology
• 2012
During the late stages of stellar evolution in massive stars (C fusion and later), the fusion luminosity in the core of the star exceeds the star’s Eddington luminosity. This can drive vigorous
• Physics
• 2015
We perform three-dimensional radiation hydrodynamic simulations of the structure and dynamics of the radiation-dominated envelopes of massive stars at the location of the iron opacity peak.
• Physics
• 2008
Following the unstable ignition of carbon, but prior to explosion, a white dwarf (WD) in a Type Ia supernova (SN Ia) undergoes a simmering phase. During this time, a central convective region grows
• Physics
• 2014
Both observations and numerical simulations are discordant with predictions of conventional stellar evolution codes for the latest stages of a massive star's life before core collapse. The most
• Physics, Environmental Science
• 2007
We describe the results of 3D numerical simulations of oxygen shell burning and hydrogen core burning in a 23 M☉ stellar model. A detailed comparison is made to stellar mixing-length theory (MLT) for
• 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.