Physics, Formation and Evolution of Rotating Stars

By S. Stahler. 2009

361 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c582c361d85d9b5857d555ae2e5e41f2ee92663f

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In Astronomy and Astrophysics

1. Selma de Mink
2. N. Langer
3. D. Stello
4. A. Miglio
5. W. Chaplin
6. Aaron Dotter
7. G. Meynet
8. R. Hirschi

In Instrumentation

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

Citations in the corpus

• 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): “On the main sequence, the evolution of the internal angular momentum profile is accounted for using the complete formalism developed by Zahn (1992), Maeder & Zahn (1998), and Mathis & Zahn (2004), which takes into account advection by meridional circulation and diffusion by shear turbulence (see Pal”
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation (2019, methodology): “The averages in Equation (35) are performed over each isobar (Meynet & Maeder 1997). Until now, MESA used the method of Endal & Sofia (1976), which considers deviations of the Roche potential from spherical symmetry (Kopal 1959), to compute the fP and fT factors.”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, methodology): “Prescriptions derived by Zahn (1992), Maeder (2003), and Mathis et al. (2004) can differ by as much as two orders of magnitude.”
• 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).”
• THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, methodology): “We treat the enhancement of stellar winds due to rotation as in Maeder & Meynet (2000a). As justified by Georgy et al. (2011), we assume mass loss through stellar winds to be spherical when computing the associated angular momentum loss.”
• Grids of stellar models with rotation - III. Models from 0.8 to 120 Msun at a metallicity Z = 0.002 (2013, methodology): “radius at the break-up velocity (see Maeder & Meynet 2000). (Mokiem et al. 2006). Thus present models may be more representative of the stars at the high end of the velocity distribution rather than of the average rotators. Further computations will be performed to complete the present grid in order”
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit (2010, background): “Current mass-loss rates match solar-metallicity theoretical predictions (Vink et al. 2001) to within 0.2 dex. ages (Sung & Bessell 2004), while Crowther et al. (2006) estimated 1.3 ± 0.3 Myr for NGC 3603 from a comparison between massive O stars and theoretical isochrones (Lejeune & Schaerer 2001).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, background): “For lowerTeff, the library is completed with spectral fluxes for M, L, and T dwarfs from Allard et al. (2000), M giants from Fluks et al. (1994), and finally C star spectra from Loidl et al. (2001).”
• Classical Be stars (2013, background): “2 of Maeder 2009, for the derivation of this factor).”
• Spin down of the core rotation in red giants (2012, background): “(9) and (10), one can derive that the core kernel reduces to about 1/2, in agreement with the Ledoux coefficient of g modes (Ledoux 1951).”
• Grids of stellar models with rotation - I. Models from 0.8 to 120 M⊙ at solar metallicity (Z = 0.014) (2011, methodology): “The formulation of the radial amplitudeU(r) was determined by Zahn (1992) and Maeder & Zahn (1998) to be”
• The PLATO 2.0 mission (2013, background): “One of the main sources of uncertainty affecting age determination is the presence and efficiency of transport mechanisms in radiative zones [227, 391].”