Physics, Formation and Evolution of Rotating Stars

By Andre Maeder. 2009

470 citations recorded by the source corpus.

Stellar Equilibrium With and Without Rotation.- The Mechanical Equilibrium of Stars.- The Mechanical Equilibrium of Rotating Stars.- The Energetic Equilibrium of Stars.- The Energy Conservation and Radiative Equilibrium in Rotating Stars.- Stellar Convection.- Overshoot, Semiconvection, Thermohaline Convection, Rotation and Solberg-Hoiland Criterion.- Physical Properties of Stellar Matter.- The Equation of State.- The Opacities.- Nuclear Reactions and Neutrino Processes.- Hydrodynamical Instabilities and Transport Processes.- Transport Processes: Diffusion and Advection.- Meridional Circulation.- Rotation-Driven Instabilities.- Magnetic Field Instabilities and Transport Processes.- Physics of Mass Loss by Stellar Winds.- Acoustic and Gravity Waves. Helio- and Asteroseismology.- Radial Pulsations of Stars.- Nonradial Stellar Oscillations.- Transport by Gravity Waves.- Star Formation.- Pre-stellar Phase.- The Protostellar Phase and Accretion Disks.- The Pre-main Sequence Phase and the Birthlines.- Rotation in Star Formation.- The Formation of Massive Stars.- The Formation of First Stars in the Universe: Pop. III and Pop. II.5 Stars.- Main-Sequence and Post-MS Evolution.- Solutions of the Equations and Simple Models.- Evolution in the H-Burning Phases.- Evolution in the He Burning and AGB Phases of Low and Intermediate Mass Stars with Rotation.- Massive Star Evolution with Mass Loss and Rotation.- Advanced Evolutionary Stages and Pre-supernovae.- Evolution of Z = 0 and Very Low Z Stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fc58720c772a48a3b38a4c2926c1f0fb04ef184e

How researchers see this paper

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In Astronomy and Astrophysics

1. N. Langer
2. Selma de Mink
3. Aaron Dotter
4. G. Meynet
5. Robert G. Izzard
6. B. Paxton
7. S. Ekström
8. R. Hirschi

In Instrumentation

1. N. Langer
2. Selma de Mink
3. D. Stello
4. A. Miglio
5. R. Hirschi
6. Robert G. Izzard
7. Aaron Dotter
8. B. Mosser

Citations in the corpus

• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “The stability of such radiationdominated envelopes has been discussed in the past, and is still a matter of debate (see, e.g., Langer 1997; BisnovatyiKogan & Dorodnitsyn 1999; Maeder 2009; Suárez-Madrigal et al. 2013).”
• THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “Compelling evidence for spin-up of massive mainsequence stars as a result of binary interaction comes from the Be/X-ray binaries, the most frequent type of high mass X-ray binaries (Liu et al. 2006). This class, first recognized by Maraschi et al. (1976), consists of a neutron star in an eccentric o”
• THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽ M/M☉ ⩽ 8.0 (2013, background): “Convective, Overshoot and Thermohaline Mixing The mixing processes near the stellar core will have an appreciable effect on the duration and width of the main-sequence (MS) phase in the HR diagram (Maeder 2009).”
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit (2010, background): “All the main effects of rotation are included in the calculations: centrifugal support, mass-loss enhancement and especially mixing in radiative zones (Maeder 2009), although predictions for both non-rotating and rotating models are considered here.”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, background): “A book by Maeder (2009) on the physics, formation, and evolution of rotating stars presents a very detailed description of the effects of rotation on stellar evolution.”
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation (2019, background): “As stars are centrally condensed and rotational frequencies close to critical are typically reached only in the outermost layers, Ψ is well approximated by the potential of a point mass in rapidly rotating layers (e.g., Maeder 2009).”
• Rotation periods of 12 000 main-sequence Kepler stars: Dependence on stellar spectral type and comparison with v sin i observations (2013, background): “Measuring stellar rotation as a function of age and mass is essential to studies of stellar evolution (Maeder 2009) and stellar dynamos (Böhm-Vitense 2007; Reiners & Mohanty 2012).”
• The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “With the development of both observational and theoretical techniques is has been possible to move from the pioneer-⋆ for example, Maeder 2009; Langer 2012).”
• Spin down of the core rotation in red giants (2012, background): “…indications of the internal angular momentum are given by surface-abundance anomalies resulting from the action of internal transport processes and from the redistribution of angular momentum and10 chemical elements (Zahn 1992; Talon & Charbonnel 2008; Maeder 2009; Canto Martins et al. 2011).”
• WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “Using the Roche model from Maeder (2009), this deformation can be expressed as R?,eq/R?,pol = 1 + (1/2) (ω?”
• Populations of rotating stars (2013, methodology): “As described by Meynet & Maeder (2000) and Ekström et al.”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, unknown): “9 and 10; see, e. g. Maeder 2009 and references therein).”
• Angular Momentum Transport in Stellar Interiors (2018, background): “…Mathis, Rogers Secular 1D stellar modeling has shown that the combined action of hydrodynamical turbulent transport and of the advection by the meridional circulation can explain some properties of massive stars (e.g. Meynet & Maeder 2000), such as surface abundances (e.g., Hunter et al. 2008).”
• Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants (2012, background): “Rotation is an important process that can have a significant impact on the evolution and properties of stars (e.g. Maeder 2009).”
• Thermohaline instability and rotation-induced mixing - III. Grid of stellar models and asymptotic asteroseismic quantities from the pre-main sequence up to the AGB for low- and intermediate-mass stars of various metallicities (2012, methodology): “We first recall the impact of metallicity as already reported in the literature (e.g. Schaller et al. 1992; Schaerer et al. 1993; Charbonnel 1994; Heger & Langer 2000; Maeder 2009).”