2021/03/01 by Masanobu Kunitomo, Shigeru Ida, Taku Takeuchi +3
Physics and Astronomy · #Accretion (finance) #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Photoevaporation #Protoplanetary disk #Stars #Stellar collision #Stellar evolution #Stellar physics #Stellar, planetary, and galactic studies #T Tauri star #Young stellar object #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/abdb2a
published as ApJ (2021), 909, 109 · 21 pages, 15 figures, published in ApJ. Evolutionary models of young 0.5-5 Msun stars are available at https://zenodo.org/record/4595807
openalex publication_date 2021/03/01 · arxiv created 2021/03/13 · openalex created_date 2021/03/15 · arxiv updated 2021/03/16 · openalex updated_date 2026/08/05
Abstract We aim to understand the effect of stellar evolution on the evolution of protoplanetary disks. We focus in particular on the disk evolution around intermediate-mass (IM) stars, which evolve more rapidly than low-mass ones. We numerically solve the long-term evolution of disks around 0.5–5 M ☉ stars considering viscous accretion and photoevaporation (PE) driven by stellar far-ultraviolet (FUV), extreme-ultraviolet (EUV), and X-ray emission. We also take stellar evolution into account and consider the time evolution of the PE rate. We find that the FUV, EUV, and X-ray luminosities of IM stars evolve by orders of magnitude within a few million years, along with the time evolution of stellar structure, stellar effective temperature, or accretion rate. Therefore, the PE rate also evolves with time by orders of magnitude, and we conclude that stellar evolution is crucial for the disk evolution around IM stars.