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arXiv · 2405.12274

A Model for Eruptive Mass Loss in Massive Stars

Shelley J. Cheng·Jared A. Goldberg·Matteo Cantiello·Evan B. Bauer·Mathieu Renzo·Charlie Conroy
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Abstract

Eruptive mass loss in massive stars is known to occur, but the mechanism(s) are not yet well-understood. One proposed physical explanation appeals to opacity-driven super-Eddington luminosities in stellar envelopes. Here, we present a 1D model for eruptive mass loss and implement this model in the MESA stellar evolution code. The model identifies regions in the star where the energy associated with a locally super-Eddington luminosity exceeds the binding energy of the overlaying envelope. The material above such regions is ejected from the star. Stars with masses $10-100~M_\odot$ at solar and SMC metallicities are evolved through core helium burning, with and without this new eruptive mass-loss scheme. We find that eruptive mass loss of up to $\sim10^{-2}~M_\odot \mathrm{yr}^{-1}$ can be driven by this mechanism, and occurs in a vertical band on the HR diagram between $3.5 \lesssim \log(T_\mathrm{eff}/\mathrm{K}) \lesssim 4.0$. This predicted eruptive mass loss prevents stars of initial masses $\gtrsim20~M_\odot$ from evolving to become red supergiants, with the stars instead ending their lives as blue supergiants, and therefore offers a possible explanation for the observed lack of red supergiants in that mass regime.

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Shelley J. Cheng, Jared A. Goldberg, Matteo Cantiello, Evan B. Bauer, Mathieu Renzo, Charlie Conroy. 2024-05-20. A Model for Eruptive Mass Loss in Massive Stars. https://arxiv.org/abs/2405.12274

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