Super-Eddington stellar winds: unifying radiative-enthalpy vs. flux-driven models

Abstract

We derive semi-analytic solutions for optically thick, super-Eddington stellar winds, induced by an assumed steady energy addition $\Delta \dot{E}$ concentrated around a near-surface heating radius $R$ in a massive star of central luminosity $L_{\ast }$. We show that obtaining steady wind solutions requires both that the resulting total luminosity $L_o=L_{\ast }+\Delta \dot{E}$ exceed the Eddington luminosity, ${\Gamma }_o\equiv L_o/L_{Edd}>1$, and that the induced mass loss rate be such that the "photon-tiring" parameter $m\equiv \dot{M}GM/R{L}_o\le 1-1/{\Gamma }_o$, ensuring the luminosity is sufficient to overcome the gravitational potential $GM/R$. Our analysis unifies previous super-Eddington wind models that either: (1) assumed a direct radiative flux-driving without accounting for the advection of radiative enthalpy that can become important in such an optically thick flow; or (2) assumed that such super-Eddington outflows are adiabatic, neglecting the effects of the diffusive radiative flux. We show that these distinct models become applicable in the asymptotic limits of small vs. large values of $m{\Gamma }_o$, respectively. By solving the coupled differential equations for radiative diffusion and wind momentum, we obtain general solutions that effectively bridge the behaviours of these limiting models. Two key scaling results are for the terminal wind speed to escape speed, which is found to vary as $v_{\infty }^2/v_{esc}^2={\Gamma }_o/(1+m{\Gamma }_o)-1$, and for the final observed luminosity $L_{obs}$, which for all allowed steady-solutions with $m<1-1/{\Gamma }_o$, exceeds the Eddington luminosity, $L_{obs}>L_{Edd}$. Our super-Eddington wind solutions have potential applicability for modeling phases of eruptive mass loss from massive stars, classical novae, and the remnants of stellar mergers.

arXiv comment13 pages, 11 figures, accepted for MNRAS

References in corpus (23)

• Common Envelope Evolution: Where we stand and how we can move forward
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars
• A giant outburst two years before the core-collapse of a massive star
• On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
• Wave-Driven Mass Loss in the Last Year of Stellar Evolution: Setting the Stage for the Most Luminous Core-Collapse Supernovae
• The Unprecedented 2012 Outburst of SN 2009ip: A Luminous Blue Variable Becomes a True Supernova
• SN 2006jc: A Wolf-Rayet Star Exploding in a Dense He-Rich Circumstellar Medium
• Caltech Core-Collapse Project (CCCP) observations of type IIn supernovae: typical properties and implications for their progenitor stars
• An outburst from a massive star 40 days before a supernova explosion
• A Porosity-Length Formalism for Photon-Tiring-Limited Mass Loss from Stars Above the Eddington Limit
• Luminous Blue Variables and superluminous supernovae from binary mergers
• Local Radiation Hydrodynamic Simulations of Massive Star Envelopes at the Iron Opacity Peak
• Super-Eddington Stellar Winds Driven by Near-Surface Energy Deposition
• Detection of an outburst one year prior to the explosion of SN 2011ht
• Super-Eddington Atmospheres that Don't Blow Away
• Two-Dimensional Simulations of Pulsational Pair-Instability Supernovae
• The Astrophysical Implications of Dust Formation During The Eruptions of Hot, Massive Stars
• A consistent solution for the velocity field and mass-loss rate of massive stars
• SN 2009ip at late times - an interacting transient at +2 years
• The Unusual Temporal and Spectral Evolution of SN2011ht. II. Peculiar Type IIn or Impostor?
• On the behaviour of stellar winds that exceed the photon-tiring limit
• The dynamics of radiation driven, optically thick winds
• G-Mode Excitation During the Pre-explosive Simmering of Type Ia Supernovae

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• Critical Metallicity of Cool Supergiant Formation. I. Effects on Stellar Mass Loss and Feedback
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• Mass Ejection Driven by Sudden Energy Deposition in Stellar Envelopes
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