The physics of deep-interior convective shell boundaries in a massive pre-supernova star: Internal gravity wave mixing at the N squared peak

arXiv:2609.28667 · astro-ph.SR · Submitted 2026-09-23 · Read on arXiv

astro-ph.SR

Submitted: 2026-09-23

Updated: 2026-09-23

Comments: Submitted to ApJL

Code: https://github.com/PPMstar/PyPPM

License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/

Terminology

• Core — 15× in this paper · explained in 2 episodes
• Entrainment — 9× in this paper · explained in 2 episodes
• Abundance — 1× in this paper · explained in 1 episode
• Calibration — 1× in this paper · explained in 7 episodes

Sources

• Pre-supernova O-C shell mergers could produce more $^{44}\mathrm{Ti}$ than the explosion
• 3D Macro Physics and Light Odd-Z Element Production in O-C Shell Mergers: Implications for $^{40}\mathrm{K}$ production and radiogenic heating inventories of rocky exoplanets
• The Occurrence and Impact of Carbon-Oxygen Shell Mergers in Massive Stars

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