Image Details

Choose export citation format:

Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars

  • Authors: Bill Paxton, Matteo Cantiello, Phil Arras, Lars Bildsten, Edward F. Brown, Aaron Dotter, Christopher Mankovich, M. H. Montgomery, Dennis Stello, F. X. Timmes, and Richard Townsend

Paxton et al. 2013 The Astrophysical Journal Supplement Series 208 4.

  • Provider: AAS Journals

Caption: Figure 44.

Evolution of T c and ρ c in the massive rotating models. The locations of core helium, carbon, neon, oxygen, and silicon burning are labeled. A dashed curve marks the electron–positron pair-instability region where Γ 1 < 4/3. All models are rotating initially at 20% of critical rotation. The calculations include the effects of rotation and Spruit–Tayler magnetic fields as discussed in Section 6. Models with initial mass ⩽100  M have initial metallicity Z = 0.02, while models with mass ⩾120  M have initial metallicity Z = 0.001. The end of the line for each mass corresponds to the time of core collapse, defined as when any part of the collapsing core exceeds an infall velocity of 1000 km s −1. The tracks for the 60  M and 70  M overlap in this plot.

Other Images in This Article

Show More

Copyright and Terms & Conditions