New Model Predicts Convective Core Mass Evolution in Massive Stars

Recent research by Minori Shikauchi, Ryosuke Hirai, and Ilya Mandel presents a semi-analytical model that explores the evolution of convective core mass in massive stars during their main-sequence phase. The study, titled "Evolution of the Convective Core Mass during the Main Sequence," was submitted to arXiv on August 31, 2024.

The authors conducted a series of one-dimensional stellar evolution calculations to understand how convective core masses change under various mass loss scenarios. They discovered several universal relationships between the global properties of stars that remain consistent, regardless of their mass loss history. By integrating these relationships, the researchers developed a framework capable of predicting the evolution of convective core mass for any mass loss history, which also allows for the estimation of helium core mass at the end of the main sequence.

This advancement is significant as it enhances existing methods used in rapid population synthesis codes, which are essential for simulating stellar populations and understanding their evolution. The findings could impact how astronomers model the life cycles of massive stars, particularly in environments where mass loss is prevalent, such as in binary systems or during supernova events.

The full paper can be accessed at arXiv:2409.00460.