Hovis-Afflerbach et al. (2025)
We use the binary population synthesis code MOSS to model the number of stripped stars in stellar populations that continuously form stars and across a range of metallicities. The population models interpolate the evolutionary models for single and stripped stars.
We use CMFGEN to compute spectral models for stripped stars across a range of surface gravities, hydrogen to helium surface mass fractions and effective temperatures. This model grid is used to fit to observed spectra, and obtain best-fit models.
We prepare spectral models for massive main sequence stars at three points during their evolution: 20%, 60%, and 90% through their main-sequence durations. The spectral models are computed with CMFGEN and by using surface properties from evolutionary models computed for single stars.
We use MOSS to approximate the number of stripped star binaries in the Milky Way that are in sufficiently tight orbits to radiative gravitational waves detectable by the future LISA mission.
The MOSS binary population synthesis code requires a grid of single star models in order to properly map out the parameter space that leads to stripped star formation. The grids used in this article were computed in association with the evolutionary grids for stripped stars published in 2018 and have similar settings in the MESA inlists. The models are computed for initially solar scaled metallicities with Z = 0.014, 0.006, 0.002 and 0.0002.
We use the spectral binary population synthesis part of MOSS to calculate the ionizing contribution from stripped stars to stellar populations. The population predictions are making use of the evolutionary and spectral models for stripped stars that were published in 2018.
We use MESA and CMFGEN to model the evolution and spectra of stars stripped via Case B mass transfer in binaries. We cover initial masses from 2 to 18.2 solar masses and metallicities Z = 0.014, 0.006, 0.002, and 0.0002.