Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars
نویسندگان
چکیده
منابع مشابه
Mass loss and evolution of hot massive stars
We discuss the role of mass loss for the evolution of the most massive stars, highlighting the role of the predicted bi-stability jump that might be relevant for the evolution of rotational velocities during or just after the main sequence. This mechanism is also proposed as an explanation for the mass-loss variations seen in the winds from Luminous Blue Variables (LBVs). These might be relevan...
متن کاملMass loss predictions for hot stars
I present the results of radiation-driven mass-loss predictions for hot stars of all mass. Mass loss is an important aspect for the evolution of massive stars, the rotational properties of the progenitors of gamma-ray bursts, and is essential in assessing whether the most massive stars explode as pair-instability supernovae, or avoid them due to mass loss. As a result, the rate of mass loss is ...
متن کاملThe coupling between pulsation and mass loss in massive stars
To what extent can pulsational instabilities resolve the mass-loss problem of massive stars? How important is pulsation in structuring and modulating the winds of these stars? What role does pulsation play in redistributing angular momentum in massive stars? Although I cannot offer answers to these questions, I hope at the very least to explain how they come to be asked.
متن کاملInstability & Mass Loss near the Eddington Limit
We review the physics of continuum-driven mass loss and the role it plays in η Carinae and other LBVs. Unlike line-driven mass loss, which is inherently limited by self-shadowing, continuum driving can in principle lead to mass-loss rates up to the “photon-tiring” limit, for which the energy to lift the outflow becomes equal to the stellar luminosity. We discuss how luminous atmospheres give ri...
متن کاملEvolution of massive stars with rotation and mass loss
Rotation appears as a dominant effect in massive star evolution. It largely affects all the model outputs: inner structure, tracks, lifetimes, isochrones, surface compositions, blue to red supergiant ratios, etc. At lower metallicities, the effects of rotational mixing are larger; also, more stars may reach critical velocity, even if the initial distribution of rotational velocities is the same.
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2020
ISSN: 0035-8711,1365-2966
DOI: 10.1093/mnras/staa474