Evolutionary models of the rotating sun

TLDR

The authors develop a new rotating stellar evolution code and apply it to the Sun. The code evolves a hydrostatic, fully convective pre‑main‑sequence model to the Sun’s age, incorporating angular‑momentum loss via a magnetic wind and redistribution by rotationally induced instabilities. The resulting models match the Sun’s observed oblateness limits and show minimal radial differential rotation in the outer layers while preserving a rapidly rotating core, a behavior robust across parameter variations. Published in The Astrophysical Journal (March 1989, DOI 10.1086/167210).

Abstract

view Abstract Citations (555) References (55) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Evolutionary Models of the Rotating Sun Pinsonneault, M. H. ; Kawaler, Steven D. ; Sofia, S. ; Demarque, P. Abstract A new rotating stellar evolution code is developed and applied to the sun. A hydrostatic fully convective premain-sequence model is evolved to the age of the sun. As the model evolves, it accounts for angular-momentum loss via a magnetic wind and angular-momentum redistribution by rotationally induced instabilities. The resulting models have an oblateness in agreement with observed upper limits. The rotation curves show two main features: the outer layers exhibit minimal radial differential rotation, and a rapidly rotating central core is preserved. These basic features persist through a wide range of model parameters. Publication: The Astrophysical Journal Pub Date: March 1989 DOI: 10.1086/167210 Bibcode: 1989ApJ...338..424P Keywords: Abundance; Solar Interior; Solar Rotation; Stellar Evolution; Stellar Models; Angular Velocity; Beryllium; Lithium; Periodic Variations; Solar Velocity; Stellar Rotation; Solar Physics; STARS: EVOLUTION; SUN: ABUNDANCES; SUN: INTERIOR; SUN: ROTATION full text sources ADS |