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The evolution of AGB stars with convective overshoot
Astrophysics · Submitted 11 Jul 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that overshoot at the He-flash convection zone as well as at the base of the envelope convection enhance the efficiency of the third dredge-up.
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The abstract, sentence by sentence
The influence of extended convective mixing (overshoot) on asymptotic giant branch stellar evolution is investigated in detail. The extended mixing is treated time-dependently, and the efficiency declines exponentially with the geometric distance from the convective boundary. It has been considered at all convective boundaries, including the He-flash convection zone in the intershell region which forms during the thermal pulses. Both the structural and the chemical evolution are affected by the inclusion of overshoot. The main results include a very efficient third dredge-up which leads to the formation of carbon stars of low mass and luminosity. A C13 pocket which may serve as a neutron source for the s-process can form after the third dredge-up has reached into the C12 rich intershell. Overshoot applied to the pulse-driven convective zone during the He-flash leads to a deeper penetration of the bottom of this convective zone into the C/O core below the He-burning shell. This in turn causes He4 to be less abundant in the intershell while C12 and O16 are more abundant compared to calculations without overshoot. We show that overshoot at the He-flash convection zone as well as at the base of the envelope convection enhance the efficiency of the third dredge-up. Characteristic properties of the structural and chemical evolution of AGB stars are presented.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The influence of extended convective mixing (overshoot) on asymptotic giant branch stellar evolution is investigated in detail. | contribution 0.94 | 0.81 | 0.05 | asserted 0.72 |
| s1 | The extended mixing is treated time-dependently, and the efficiency declines exponentially with the geometric distance from the convective boundary. | method 0.98 | 0.72 | 0.05 | asserted 1.00 |
| s2 | It has been considered at all convective boundaries, including the He-flash convection zone in the intershell region which forms during the thermal pulses. | method 0.77 | 0.55 | 0.04 | asserted 1.00 |
| s3 | Both the structural and the chemical evolution are affected by the inclusion of overshoot. | result 0.99 | 0.77 | 0.15 | asserted 1.00 |
| s4 | The main results include a very efficient third dredge-up which leads to the formation of carbon stars of low mass and luminosity. | result 1.00 | 0.89 | 0.46 | asserted 1.00 |
| s5 | A C13 pocket which may serve as a neutron source for the s-process can form after the third dredge-up has reached into the C12 rich intershell. | result 0.79 | 0.74 | 0.10 | hedged possibility 1.00 |
| s6 | Overshoot applied to the pulse-driven convective zone during the He-flash leads to a deeper penetration of the bottom of this convective zone into the C/O core below the He-burning shell. | result 0.96 | 0.81 | 0.09 | asserted 1.00 |
| s7 | This in turn causes He4 to be less abundant in the intershell while C12 and O16 are more abundant compared to calculations without overshoot. | result 0.96 | 0.85 | 0.10 | asserted 1.00 |
| s8 | We show that overshoot at the He-flash convection zone as well as at the base of the envelope convection enhance the efficiency of the third dredge-up. | result 1.00 | 0.92 | 0.42 | asserted 1.00 |
| s9 | Characteristic properties of the structural and chemical evolution of AGB stars are presented. | contribution 0.64 | 0.72 | 0.05 | asserted 0.84 |
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The paper
Original abstract
The influence of extended convective mixing (overshoot) on asymptotic giant branch stellar evolution is investigated in detail. The extended mixing is treated time-dependently, and the efficiency declines exponentially with the geometric distance from the convective boundary. It has been considered at all convective boundaries, including the He-flash convection zone in the intershell region which forms during the thermal pulses. Both the structural and the chemical evolution are affected by the inclusion of overshoot. The main results include a very efficient third dredge-up which leads to the formation of carbon stars of low mass and luminosity. A C13 pocket which may serve as a neutron source for the s-process can form after the third dredge-up has reached into the C12 rich intershell. Overshoot applied to the pulse-driven convective zone during the He-flash leads to a deeper penetration of the bottom of this convective zone into the C/O core below the He-burning shell. This in turn causes He4 to be less abundant in the intershell while C12 and O16 are more abundant compared to calculations without overshoot. We show that overshoot at the He-flash convection zone as well as at the base of the envelope convection enhance the efficiency of the third dredge-up. Characteristic properties of the structural and chemical evolution of AGB stars are presented.
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References
How later papers used it
49 later papers cite it
23 later papers by other authors are listed below: 22 used its method or tool and 1 used its data or values.
Uses its method or tool 22 of 31 papers with this label
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For convective overshooting we use exponential prescription, see [ref] , and [ref] for implementation.
Toward a Comprehensive Grid of Cepheid Models with MESA. III. Evolutionary and Pulsation Relations for Models with Core and Envelope Overshooting (2026) · Modeling tools – stellar evolution · 1.00
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Overshooting follows the exponential prescription [ref] , with the efficiency characterized with the and parameters at the MS core and at the lower boundary of the convective envelope on the RGB, respectively.
Toward a Comprehensive Grid of Cepheid Models with MESA. IV. Modest Effects of Rotation on Blue Loops (2026) · Evolutionary calculations · 1.00
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We used the exponential overshooting scheme from [ref] to model CBM above the convective hydrogen-burning core, with efficiency parameters $f_ov=0.010$ and $f_0=0.005$, which result in an $f_CBM = 0.005$[To determine the diffusion coefficient of the overshooting region, the overshooting scheme takes the value of the convective diffusion coefficient at a distance of $f_0H_P$, with $H_P = -P(dr/dP)$ the pressure scale height, into the convective region.
The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors (2026) · Stellar structure and evolution models · 1.00
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In our “core only” treatment of overshooting, we apply step overshooting across the hydrogen core with $f=0.345$ and $f_0=0.01$ [ref] , and exponential overshooting across the helium core with $f=0.01$ and $f_0=0.005$ [ref] [ref] [ref] .
The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants (2026) · Modeling Red Supergiants with · 0.80
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Treated overshoot mixing beyond the convective zone with a diffusion approach using an exponentially decaying diffusion coefficient based on this paper's approach.
Formation of WNL stars for the MW and LMC based on the k-omega model (2024) · 1.00 · paraphrased: the licence does not allow quoting
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We implement exponential diffusive overshoot [ref] at the Hydrogen core with a strength set to increase gradually with mass, following the expression proposed by [ref] : [equation] where $M_*$ is the mass along the isochrone, $M_full_off=1.10 M_⊙$, $M_full_on=1.80 M_⊙$, which provides a smooth transition between 0 and $f_ov$.
Isochrone fitting to the open cluster M67 in the era of Gaia and improved model physics (2024) · Overshooting · 0.99
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We define the boundary of convective regions following the Schwarzschild criterion [ref] and apply overshooting in both the envelope and core following the exponential scheme described by [ref] , with the corresponding efficiency parameters $f_ov, env$ and $f_ov, core$, respectively.
Flow-Based Generative Emulation of Grids of Stellar Evolutionary Models (2024) · MESA Grid of Dwarf Star Models · 1.00
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We use [ref] diffusive technique to represent the convective overshooting, using $f_1$ = 0.005 and $f_0$ = 0.001 for each convective core and shell.
Accretion and Recovery in Giant Eruptions of Massive Stars (2025) · The Numerical Simulation · 1.00
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Employed this paper's exponential overshoot scheme in its mesa calculations.
Seismology and diffusion of ultramassive white dwarf magnetic fields (2025) · 1.00 · paraphrased: the licence does not allow quoting
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Calculated extra mixing at boundaries of convection zones according to this paper.
Hydrodynamic models of pulsation period evolution in R Hydrae (2024) · 0.99 · paraphrased: the licence does not allow quoting
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Calculated the diffusion coefficient for overshooting of the convective envelope and pulse-driven convective zone with the scheme proposed by this paper.
The Impact of the Third Dredge-up and Mass Loss in Shaping the Initial-Final Mass Relation of White Dwarfs (2024) · 1.00 · paraphrased: the licence does not allow quoting
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We use exponential prescription for overshooting, as introduced in [ref] , see also [ref] , with $f=0.02$.
Toward a Comprehensive Grid of Cepheid Models with MESA I. Uncertainties of the Evolutionary Tracks of Intermediate-Mass Stars (2024) · Convective core overshooting · 1.00
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Included convective core overshoot using the exponential decay with a diffusion coefficient described by this paper.
Uniform characterisation of an ensemble of main-sequence benchmark stars: effect of Gaia-based data on grid search models (2024) · 1.00 · paraphrased: the licence does not allow quoting
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Explained convective overshooting in the core with this paper's theory.
Probing Red Giant Interiors with G-Dominated Mixed Modes I: The Cases of KIC 9145955, KIC 9970396, KIC 9882316 and KIC 11968334 (2026) · 0.94 · paraphrased: the licence does not allow quoting
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Adopted this paper's exponential diffusive scheme for overshooting during the main sequence.
Shaping the horizontal branch: The role of envelope mass in the evolution of stripped core-helium-burning stars (2026) · 0.86 · paraphrased: the licence does not allow quoting
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The overshoot is realized by exponentially decaying the convective diffusion coefficient from the convective boundary according to [ref] (see also [ref] for detail).
Binary Interaction Can Yield a Diversity of Circumstellar Media around Type II Supernova Progenitors (2023) · Mixing · 1.00
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Accounted for convective core overshooting by applying this paper's exponential overshooting.
On the evolutionary nature of puffed-up stripped star binaries and their occurrence in stellar populations (2023) · 0.97 · paraphrased: the licence does not allow quoting
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Used this paper's exponential prescription for overshooting from the convective core during the main sequence and from the convective envelope on the RGB.
Pulsation periods reveal tension between theoretical and empirical radii for classical Cepheids in eclipsing binary systems (2026) · 1.00 · paraphrased: the licence does not allow quoting
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We adopt the [ref] criterion to determine the boundary of the convective regions an exponential overshoot prescription [ref] with parameters $f = 0.016$ and $f_0 = 0.008$ at the top of the core and $f = 0.0174$, $f_0 = 0.0087$ at the bottom of the hydrogen-burning shell.
Collisions of red giants in galactic nuclei (2023) · Stellar model · 1.00
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We also include an exponential scheme to treat convective overshooting [ref] with parameters $f= 0.01$ and $f_0 = 0.005$.
Rotational Dynamics in Pulsational Pair-Instability Supernovae: Implications for Mass-Loss and Transient Events (2025) · PPISNe progenitor evolution with · 1.00
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Our standard and new winds models adopt a diffusive overshoot prescription which extends mixing into the radiative zone via the exponential-decay formalism in [ref] (see their equation 2).
Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSE (2026) · Convective Boundary Mixing · 1.00
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Presented illustrative models with convective overshoot of 10% of one pressure scale height above the convective core, citing this paper.
The Stability of Massive Main Sequence Stars as a Function of Metallicity (2012) · 0.81 · paraphrased: the licence does not allow quoting
Uses its data or values 1 of 3 papers with this label
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Took the overshooting parameter f_ov as 0.016 from this paper.
Distribution and evolution of Li abundance in red clump stars can be explained by the internal gravity waves (2024) · 0.97 · paraphrased: the licence does not allow quoting
How the literature uses it
17 arXiv papers cite this in 24 sentences
Papers citing it · 9 sentences without a confident label
Uses its method or tool 11 papers
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We used the exponential overshooting scheme from [ref] to model CBM above the convective hydrogen-burning core, with efficiency parameters $f_ov=0.010$ and $f_0=0.005$, which result in an $f_CBM = 0.005$[To determine the diffusion coefficient of the overshooting region, the overshooting scheme takes the value of the convective diffusion coefficient at a distance of $f_0H_P$, with $H_P = -P(dr/dP)$ the pressure scale height, into the convective region.
The effect of near-core mixing on rejuvenation and the asteroseismic properties of massive accretors · Stellar structure and evolution models · 1.00
-
In our “core only” treatment of overshooting, we apply step overshooting across the hydrogen core with $f=0.345$ and $f_0=0.01$ [ref] , and exponential overshooting across the helium core with $f=0.01$ and $f_0=0.005$ [ref] [ref] [ref] .
The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants · Modeling Red Supergiants with · 0.80
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We treat overshooting as a diffusive process with an exponentially decaying diffusion coefficient [ref] .
Formation of Extremely Low-mass White Dwarf Binaries Undergoing Enhanced Angular Momentum Loss · Model Inputs and Methods · 0.97
Uses its data or values 1 paper
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The extent of the overshoot region is controlled by the free parameter $f_ov$, for which we adopt the recommended value of $0.016$ [ref] .
Formation of Extremely Low-mass White Dwarf Binaries Undergoing Enhanced Angular Momentum Loss · Model Inputs and Methods · 0.90
Cites it as background 1 paper
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Another factor that will affect the structure and composition of the RSG, and thus the pre-SN emission, is overshooting at the convective-radiative boundaries [ref] .
The Effect of Mass Loss and Convective Overshooting on the Pre-Collapse Structure, Composition, and Neutrino Emission of Red Supergiants · Introduction · 0.91
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