Hot subdwarf stars physical parameter

While existing mass distribution analyses suggest additional channels beyond helium white dwarf (He-WD) mergers contribute to He-rich subdwarf formation, these conclusions are constrained by limited sample sizes of mass-measured He-rich objects. We developed a deep leaning model which combines a convolution neural network (CNN) together with a squeeze-and-excitation (SE) block to calculate synthetic spectral energy distributions (SEDs) for 1012 spectroscopically confirmed hot subdwarfs.

Through directly comparison between synthetic SEDs and observed flux density, we derived stellar parameters (mass, radius, luminosity) for unprecedented number size of hot subdwarf stars, enabling more conclusive channel discrimination than prior studies. The mass distribution of sdB/sdOB stars confirmed the results from model predictions of binary populations synthesis (BPS). A primary and secondary peak (i.e., around 0.56 and 0.4 Msun) is obviously presented in the mass distribution of He-rich hot subdwarf stars.