Presupernova Evolution of Rotating Massive Stars. II. Evolution of the Surface Properties

By Alexander Heger, N. Langer. 2000

330 citations recorded by the source corpus.

We investigate the evolution of the surface properties of models for rotating massive stars, i.e., their luminosities, effective temperatures, surface rotational velocities, and surface abundances of all isotopes, from the zero-age main sequence to the supernova stage. Our results are based on the grid of stellar models by Heger, Langer, & Woosley, which covers solar metallicity stars in the initial-mass range 8-25 M☉. Results are parameterized by initial mass, initial rotational velocity and major uncertainties in the treatment of the rotational mixing inside massive stars. Rotationally induced mixing processes widen the main sequence and increase the core hydrogen-burning lifetime, similar to the effects of convective overshooting. It can also significantly increase the luminosity during and after core hydrogen burning, and strongly affects the evolution of the effective temperature. Our models predict surface rotational velocities for various evolutionary stages, in particular for blue supergiants, red supergiants, and for the immediate presupernova stage. We discuss the changes of the surface abundances due to rotationally induced mixing for main sequence and post-main-sequence stars. We single out two characteristics by which the effect of rotational mixing can be distinguished from that of massive close binary mass transfer, the only alternative process leading to nonstandard chemical surface abundances in massive stars. A comparison with observed abundance anomalies in various types of massive stars supports the concept of rotational mixing in massive stars and indicates that it is responsible for most of the observed abundance anomalies.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/856a9180a637a44d8ba32362ac3c9ccfaf7bbea4

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. N. Langer
2. Michela Mapelli
3. Selma de Mink
4. Stan Woosley
5. S. Smartt
6. Mario Spera
7. G. Meynet
8. N. Giacobbo

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): “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).”
• The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “This includes the importance of rotation in both the evolution of the star (Heger et al. 2000; Hirschi et al. 2004) and in the mixing of nu-cleosynthesised material to the stellar surface (Maeder 1987; Heger & Langer 2000; Frischknecht et al. 2010).”
• Present-day cosmic abundances - A comprehensive study of nearby early B-type stars and implications for stellar and Galactic evolution and interstellar dust models (2012, background): “…cycles throughout most of their lifetime and the nuclearprocessed material may reach their surface layers through rotational mixing already during their main sequence phase (e.g. Maeder & Meynet 2000; Heger & Langer 2000), opening up a very powerful diagnostic to test models of stellar evolution.”
• The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, methodology): “…et al. (2009) (b) as used in HGL06 (c) Hunter et al. (2007) (d) Korn et al. (2005) (e) H ii regions (Kurt & Dufour 1998) (f) as adopted in this work (g) including the whole iron group (h) mean value from Trundle et al. (2007) terior, such as rotational induced mixing (e.g. Heger & Langer 2000).”
• Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “The mixing can be enhanced by rotation (Langer 1992; Heger & Langer 2000; Maeder & Meynet 2000).”
• TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS (2010, background): “…as surface abundances of CNO elements of massive stars and Wolf-Rayet (WR) star populations at different metallicities (e.g., Maeder & Meynet 2000; Heger & Langer 2000; Meynet & Maeder 2005), their adopted angular momentum transport mechanisms turned out to be too inefficient to explain the…”
• Progenitors of Core-Collapse Supernovae (2009, methodology): “…rate and probably magnetic fields play critical roles in forming evolved objects of various radii, density profiles and surrounding circumstellar medium (Podsiadlowski, Joss, and Hsu 1992, Heger and Langer 2000, Eldridge and Tout 2004, Hirschi, Meynet, and Maeder 2004, Yoon and Langer 2005).”
• Probing the properties of convective cores through g modes : high-order g modes in SPB and γ Doradus stars (2008, background): “Different approaches have been proposed to treat the effects of rotation on the transport of angular momentum and chemicals (see e.g. Heger & Langer 2000; Maeder & Meynet 2000; Pinsonneault et al. 1989, and references therein).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “…the stellar evolution community has come a long way in understanding stars with 1D simulations (Meynet & Maeder 1997; Langer et al. 1999; Maeder & Meynet 2000b; Heger & Langer 2000; Hirschi et al. 2004; Cantiello & Langer 2010), thus motivating our need to fully incorporate rotation within MESA.”
• Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars (2005, methodology): “As predicted by models of stellar evolution (Endal & Sofia 1979; Pinsonneault et al. 1991; Heger & Langer 2000; Meynet & Maeder 2000), fast rotation is further expected to generate several instabilities that contribute to redistributing the internal angular momentum.”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, background): “Significant advances have been made in this field (e.g., Heger & Langer 2000; Meynet & Maeder 2000), which demonstrated that the evolutionary paths of rapidly rotating massive stars can differ from those of non-rotating stars.”
• Stellar and wind parameters of Galactic O-stars - The influence of line-blocking/blanketing (2004, unknown): “Unfortunately, is not possible to perform a similar comparison using evolutionary calculations based on rotating models as presented by Meynet & Maeder (2000) and Heger & Langer (2000), since we do not know the initial rotational velocity of our objects.”
• The VLT FLAMES Survey of Massive Stars: Rotation and Nitrogen Enrichment as the Key to Understanding Massive Star Evolution (2007, unknown): “The nitrogen abundances and rotational velocities in group 4 are indeed consistent with the predictions for a blue loop stage (Heger & Langer 2000).”
• First Results from the CHARA Array. I. An Interferometric and Spectroscopic Study of the Fast Rotator α Leonis (Regulus) (2005, background): “The position of Regulus in this diagram shows that the star is overluminous for its mass as predicted for rotating stars that evolve to higher luminosity as fresh H is mixed into their convective cores (Heger & Langer 2000; Meynet & Maeder 2000).”