Mass Loss Dynamics in Evolved Stellar Systems
Summary
Evolved stars, such as asymptotic giant branch (AGB) stars, red supergiants and hypergiants, undergo intense mass loss through stellar winds that shape their subsequent evolution and contribute to the chemical enrichment of galaxies. This mass loss is driven by a combination of large‐scale pulsations, turbulent convection and the formation of dust grains in extended atmospheres. Pulsations levitate gas to cooler regions where dust condenses, and radiation pressure on these grains accelerates an outflow. The resulting circumstellar envelopes display a remarkable variety of morphologies, from spherical shells to filamentary arcs and clumpy ejecta. Episodic mass ejections, often linked to changes in stellar luminosity or convective activity, give rise to discrete structures whose kinematics trace the history of outflow events. Understanding these processes requires both high‐resolution observations, often at millimetre and submillimetre wavelengths, and multidimensional radiation‐hydrodynamical models that capture the interplay between gas dynamics, dust chemistry and radiative forces. Insights into mass‐loss rates and wind geometry have profound implications for predicting final stellar masses, the formation of planetary nebulae and the input of gas and dust into the interstellar medium.
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Mass Loss Dynamics in Evolved Stellar Systems publication trend
The graph below shows the total number of articles in mass loss dynamics in evolved stellar systems across all publications each year (not limited to Nature Index journals).
Technical terms
Mass‐loss rate: The amount of mass a star ejects per unit time, typically expressed in solar masses per year (M⊙ yr⁻¹).
Circumstellar envelope: The shell of gas and dust surrounding an evolved star, formed by accumulated mass ejections over time.
Dust‐driven wind: A stellar outflow propelled by radiation pressure on dust grains that form in the extended atmosphere.
Convection cell: A turbulent region in the stellar interior or atmosphere where hot material rises and cool material sinks, driving large‐scale surface patterns.
Pulsation: Periodic expansion and contraction of a star’s outer layers, which can lift gas to cooler regions conducive to dust formation.
Episodic mass ejection: Discrete, often irregular events in which a star releases substantial amounts of material, creating clumps or arcs in its envelope.
Radiation pressure: The force exerted by photons on matter, capable of accelerating dust grains and driving stellar winds.
References
- ALMA Reveals Hidden Morphologies in the Molecular Envelope of VY Canis Majoris. The Astrophysical Journal Letters (2023).
- Global 3D radiation-hydrodynamical models of AGB stars with dust-driven winds. Astronomy & Astrophysics (2023).
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