☆ 3.8 Review

The Structure and Evolution of Stars: Introductory Remarks

GALAXIES (2023)

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Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure

Adam S. Jermyn et al.

Summary: We have updated the capabilities of the MESA software by implementing automatic differentiation, improving the treatment of convection, enhancing the equation of state, and updating various aspects of stellar modeling. We have also introduced new methods to increase the efficiency of calculating opacities and radiative levitation, and to evolve the late stages of massive stars. Additionally, we have made improvements to the software infrastructure of MESA to enhance source code development and community engagement.

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES (2023)

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Article Astronomy & Astrophysics

A calibration point for stellar evolution from massive star asteroseismology

Siemen Burssens et al.

Summary: Massive stars are progenitors of supernovae, neutron stars, and black holes. This study deduces the convective core mass and demonstrates non-rigid radial rotation in a supernova progenitor, HD 192575, using various methods including asteroseismology and space-based photometry. The results provide important insights into the rotation and mixing processes inside massive stars.

NATURE ASTRONOMY (2023)

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Review Astronomy & Astrophysics

Opacities and Atomic Diffusion

Georges Alecian et al.

Summary: Opacity is crucial for stellar modeling and influences the structure and energy flow of stars. It is determined by the interaction between radiation and matter, which is influenced by the microscopic interactions of photons and atoms. Atomic diffusion, a slow process, can significantly impact stellar structure and chemical composition measurements.

GALAXIES (2023)

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Review Astronomy & Astrophysics

Magnetism in High-Mass Stars

Zsolt Keszthelyi

Summary: Magnetism is a common property of astrophysical plasmas, but stellar magnetism in high-mass stars is still not fully understood. This review discusses recent observational and modeling efforts to expand our knowledge of magnetic properties in high-mass stars. Various mechanisms, such as magneto-convection, mass-loss quenching, internal angular momentum transport, and magnetic braking, have significant implications for stellar evolution and populations. Therefore, resolving open questions related to magnetism in high-mass stars is an urgent issue.

GALAXIES (2023)

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A Review of the Mixing Length Theory of Convection in 1D Stellar Modeling

Meridith Joyce et al.

Summary: This article reviews the application of the one-dimensional Mixing Length Theory (MLT) model in stellar interiors and low-mass stellar evolution. The history of MLT is summarized, and a derivation of MLT in the context of 1D stellar structure equations is presented. The physical regimes in which MLT is relevant are discussed. Attempts to improve and extend the formalism, including to higher dimensions, are reviewed.

GALAXIES (2023)

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Review Astronomy & Astrophysics

Convective Boundary Mixing in Main-Sequence Stars: Theory and Empirical Constraints

Evan H. Anders et al.

Summary: This review discusses the convective boundaries and mixing in solar-type stars and intermediate- and high-mass stars. It covers the implementation of 1D CBM prescriptions, the fluid dynamical processes of convective overshoot, entrainment, and convective penetration, and observational inferences regarding mixing in stellar cores. The paper concludes with a discussion of future research directions.

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3D hydrodynamic simulations of massive main-sequence stars – I. Dynamics and mixing of convection and internal gravity waves

Falk Herwig et al.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY (2023)

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Calibrating angular momentum transport in intermediate-mass stars from gravity-mode asteroseismology

J. S. G. Mombarg

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Multidimensional Simulations of Core Convection

Daniel Lecoanet et al.

Summary: This article discusses the influence and simulation methods of core convection in main sequence intermediate- and high-mass stars, and summarizes the latest simulation results. Simulations provide important insights into the processes associated with core convection. However, simulating core convection faces many challenges, such as a wide range of temporal and spatial scales and potentially contradictory results from different methods. To address these issues, future research needs to consider the impact of stellar luminosity, dimensionality, and turbulence intensity on the results, and conduct code comparison projects.

GALAXIES (2023)

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Dynamics in a stellar convective layer and at its boundary: Comparison of five 3D hydrodynamics codes

R. Andrassy et al.

Summary: Our ability to predict the structure and evolution of stars is limited by complex hydrodynamic processes. However, our simulations show that hydrodynamic simulations of flows in stellar interiors are reliable.

ASTRONOMY & ASTROPHYSICS (2022)

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Asteroseismology of β Cephei stars: The stellar inferences tested in hare and hound exercises

S. J. A. J. Salmon et al.

Summary: This study investigates the importance of asteroseismology for beta Cephei stars by simulating and validating seismic models. The results show that a set of identified oscillation frequencies can accurately infer stellar parameters, and the importance of observational constraints is also verified.

ASTRONOMY & ASTROPHYSICS (2022)

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Stellar Convective Penetration: Parameterized Theory and Dynamical Simulations

Evan H. Anders et al.

Summary: Most stars have convection zones, but the behavior of convective boundaries is not well understood. In this study, researchers conducted 3D numerical simulations and discovered the existence of penetration zones. By defining the penetration parameter P and constructing an energy-based theoretical model, they successfully described the simulations. This study is important for understanding convective phenomena in stars.

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Predictions for Gravity-mode Periods and Surface Abundances in Intermediate-mass Dwarfs from Shear Mixing and Radiative Levitation

Joey S. G. Mombarg et al.

Summary: Recent study presented new MESA stellar models with improvements in computing efficiency and shear mixing in radiative envelopes, which allows for mode trapping in chemical mixing profiles. Predictions also show correlations between N/C and C/O abundance ratios with stellar age, observable with precision around 0.1 dex with accurate age estimates.

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Stochastic Low-frequency Variability in Three-dimensional Radiation Hydrodynamical Models of Massive Star Envelopes

William C. Schultz et al.

Summary: Increasing stellar mass leads to higher stellar luminosity, causing radiation pressure to dominate in the stellar envelope. Additional instabilities can occur in OB stars, manifesting as low-frequency variability in lightcurves. 3D simulations validate these observations and show similar characteristics to real stars.

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Asteroseismic inference of the near-core magnetic field strength in the main sequence B star HD 43317

Daniel Lecoanet et al.

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Asteroseismology Across the Hertzsprung-Russell Diagram

Donald W. Kurtz

Summary: Asteroseismology is a mature field that has made significant advancements in the past decade. Space photometry and ground-based surveys have provided high-precision data, leading to a better understanding of stellar physics and improving models of stellar structure and evolution.

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Convective Penetration in Early-type Stars

Adam S. Jermyn et al.

Summary: Observations indicate that convective cores of stars ingest material from the overlying radiative zone. The mechanism causing this mixing is uncertain. By using a theory of convective penetration, it is found that convective penetration can explain the core masses of stars and matches observed trends in mass and age. The results suggest that most convective boundary mixing in early-type main-sequence stars arises from convective penetration.

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On the Diversity of Mixing and Helium Core Masses of B-type Dwarfs from Gravity-mode Asteroseismology

May G. Pedersen

Summary: The internal mixing profiles of oscillating stars observed by the Kepler space telescope have been studied to investigate their distinguishability and to predict the expected helium core masses at the end of the main-sequence evolution. The results show ambiguous differentiation in the mixing profiles and emphasize the significant influence of envelope mixing estimation on the helium core masses.

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Method and new tabulations for flux-weighted line opacity and radiation line force in supersonic media☆

L. G. Poniatowski et al.

Summary: This paper presents a comprehensive and fast method for computing the radiation line force using tables of spectral-line-strength distribution parameters, which can be applied in arbitrary (multi-D, time-dependent) simulations, including those that account for the line-deshadowing instability, to compute the appropriate opacities.

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First 3D radiation-hydrodynamic simulations of Wolf-Rayet winds

N. Moens et al.

Summary: Understanding the outflow of WR stars is crucial for studying stellar evolution, the impact of massive stars on their environments, and the distribution of black hole masses.

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Backtracing the internal rotation history of the β Cep star HD 129929

S. J. A. J. Salmon et al.

Summary: HD 129929 is a massive slowly rotating giant star with differential rotation between the core and surface. The surface rotation speed is estimated to be around 2km/s. The models based on hydrodynamic processes are consistent with the asteroseismic measurements, while the models considering the Tayler magnetic instability do not match the observations.

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Magnetic signatures on mixed-mode frequencies II. Period spacings as a probe of the internal magnetism of red giants

L. Bugnet

Summary: In this study, we investigate the effect of magnetic fields on the internal dynamics of evolved stars using asteroseismic data. We propose a new method to account for magnetic signatures in the estimation of period spacings. Our results show that the presence of magnetic fields leads to biased estimates of period spacings and careful analysis of multiple estimates and frequency patterns may result in the first detection of internal magnetic fields in red giants.

ASTRONOMY & ASTROPHYSICS (2022)

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Magnetic fields of 30 to 100 kG in the cores of red giant stars

Gang Li et al.

Summary: The presence of magnetic fields in the cores of red giant stars has been detected through the observation of changes in oscillation mode frequencies. This discovery is significant for understanding the properties of magnetic fields in stellar interiors.

NATURE (2022)

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Article Astronomy & Astrophysics

Photometric detection of internal gravity waves in upper main-sequence stars: III. Comparison of amplitude spectrum fitting and Gaussian process regression using CELERITE2

Dominic M. Bowman et al.

Summary: Recent studies have shown that massive stars commonly exhibit stochastic low-frequency variability, which is believed to be caused by internal gravity waves or dynamic turbulence. This study aims to compare the properties of this variability and confirm its correlation with a star's location in the HR diagram using different statistical methods. The results suggest that Gaussian process regression is an efficient and novel methodology for characterizing stochastic low-frequency variability in massive stars.

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Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport

May G. Pedersen

Summary: This study compiles the asteroseismic measurements of internal rotation for 52 slowly pulsating B stars, revealing the core rotation frequencies decrease with age and indicating evidence of angular momentum transport occurring on the main sequence.

ASTROPHYSICAL JOURNAL (2022)

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Probing the interior physics of stars through asteroseismology

C. Aerts

Summary: High-precision brightness measurements collected over years using telescopes in space have enabled astronomers to study the physics of stellar interiors through nonradial oscillations. The field of asteroseismology has provided new insights into how stars rotate and evolve chemically. Data-driven space asteroseismology has significantly improved computer models of star evolution, which are crucial for various research fields in space science and have potential applications in the search for extraterrestrial life and studies of supernova progenitors.

REVIEWS OF MODERN PHYSICS (2021)

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Wind-envelope interaction as the origin of the slow cyclic brightness variations of luminous blue variables

L. Grassitelli et al.

Summary: This study explores the impact of stellar wind mass-loss on envelope structure in massive stars near the Eddington limit, suggesting that when the wind mass-loss rate crosses a certain threshold, it leads to restructuring of the stellar envelope and induces drastic radius and temperature changes. The resulting cycle lacks a stationary equilibrium configuration and broadly reproduces the observational phenomenology of S Doradus variability.

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Convective core sizes in rotating massive stars: I. Constraints from solar metallicity OB field stars

S. Martinet et al.

Summary: Spectroscopic studies of Galactic O and B stars suggest that the convective core sizes in stars more massive than about 8 solar masses at the end of the main sequence phase may be larger than predicted by stellar models. By combining stellar evolution models with spectroscopic parameters, the study examines the convective core size in massive stars and finds tensions among different methods for stars more massive than 15 solar masses.

ASTRONOMY & ASTROPHYSICS (2021)

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Article Astronomy & Astrophysics

Convective core entrainment in 1D main-sequence stellar models

L. J. A. Scott et al.

Summary: The study on the application of the entrainment law in 1D models reveals that the impact of mass and time on boundary penetrability varies, with the chemical gradient having a greater influence on time.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY (2021)

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Constraining stellar evolution theory with asteroseismology of γ Doradus stars using deep learning: Stellar masses, ages, and core-boundary mixing

J. S. G. Mombarg et al.

Summary: The neural network approach developed in this study allows for the derivation of important stellar properties for evolution, such as mass, age, and extent of core-boundary mixing. It also paves the way for inferring mixing profiles throughout the radiative envelope for large samples of gamma Doradus stars in the future.

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Stochastic light variations in hot stars from wind instability: finding photometric signatures and testing against the TESS data

J. Krticka et al.

Summary: The study reveals characteristic photometric signatures of line-driven wind instability, including a knee in the power spectrum of magnitude fluctuations and a negative skewness in the distribution of fluctuations. These features persist even when combining light curves from independent wind sectors.

ASTRONOMY & ASTROPHYSICS (2021)

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Article Astronomy & Astrophysics

Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants

L. Bugnet et al.

Summary: The research suggests that evolved solar-like stars may contain a significant magnetic field in their core, leading to asymmetries in mixed-mode frequency multiplets. The impact of the magnetic field on the interior of stars can be detected in seismic data, but only for small field amplitudes that do not affect the modes significantly.

ASTRONOMY & ASTROPHYSICS (2021)

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Probing the temperature gradient in the core boundary layer of stars with gravito-inertial modes: The case of KIC 7760680

M. Michielsen et al.

Summary: This study investigated the thermal and chemical structure in the near-core region of stars with a convective core using gravito-inertial modes, focusing on the B-type star KIC 7760680 rotating at a quarter of its critical rotation velocity. The results suggest that period spacings of modes with consecutive radial order offer a better diagnostic for asteroseismic modelling of stars with high-order gravito-inertial modes, with simpler models without convective boundary mixing being statistically preferred for KIC 7760680.

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The effects of surface fossil magnetic fields on massive star evolution - III. The case of τ Sco

Z. Keszthelyi et al.

Summary: tau Sco is a magnetic B-type star with surprising characteristics such as slow rotation and nitrogen excess. To reconcile its properties with single-star models, an increase in the efficiency of rotational mixing and magnetic braking is necessary.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY (2021)

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Internal mixing of rotating stars inferred from dipole gravity modes

May G. Pedersen et al.

Summary: Observations of 26 rotating stars with masses between 3 and 10 solar masses reveal a wide range of internal mixing levels, with models incorporating radially stratified mixing profiles showing the best asteroseismic performance. This study provides observational guidance for three-dimensional hydrodynamical simulations of transport processes in the deep interiors of stars, based on gravity modes probing the stars' deep interiors near the convective core. The internal mixing levels in the analyzed stars are unexpectedly varied and are best reproduced with models incorporating radially stratified mixing profiles.

NATURE ASTRONOMY (2021)

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One size does not fit all: Evidence for a range of mixing efficiencies in stellar evolution calculations

C. Johnston

Summary: Internal chemical mixing in intermediate- and high-mass stars is a major uncertainty in stellar evolution models. This study demonstrates that stellar models regularly underestimate the masses of convective stellar cores. In order to accurately reproduce high-precision observations, stellar models require a more efficient mixing mechanism that produces more massive cores throughout the main sequence.

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On the Origin of Stochastic, Low-Frequency Photometric Variability in Massive Stars

Matteo Cantiello et al.

Summary: High-precision photometric observations have revealed that stochastic low-frequency photometric variability in early-type stars is likely caused by subsurface convection. The presence of subsurface convection is closely related to the timescale and amplitude of this variability, as well as to the amplitude of macroturbulence. The explanation relying on convective core driven internal gravity waves encounters difficulties and seems unlikely to explain the observed trends.

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The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars

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