Massive Stellar Cannibals: How Stellar Mergers Drive Mass-Loss in Extremely Massive Stars

Simulation outputs for stellar mergers of extremely massive stars using MESA.Description:results_1e3Msun.tar.zst: Compressed data including MESA history and profile files for stellar mergers involving a 1000 solar mass star.results_3e3Msun.tar.zst: Compressed data including MESA history and profile files for stellar mergers involving a 3000 solar mass star.results_5e3Msun.tar.zst: Compressed data including MESA history and profile files for stellar mergers involving a 5000 solar mass star.merger_discrimination.txt: Table summarizing the predicted mass loss produced during a stellar merger. The columns are:M_EMS: Extremely massive star mass in solar masses.M_COMP: Mass of the companion star in solar masses.L_R: Maximum latus rectum (in solar radii) to produce a direct merger for mergers with eccentricity of unity. Interactions with a latus rectum above this value will produce orbital scattering instead.R_EMS: Radius of the extremely massive star in solar radii.log10(E_orb): log10 of the orbital energy (erg) lost during the interaction, either during the merger or orbital scattering.M_UNB: Unbound mass in solar masses. This is the predicted mass loss.T_MERGER: Timescale in yr from the start of the interaction until either both stars merge or the companion exits the EMS.