2020/01/14 by Masanobu Kunitomo, Takeru K. Suzuki, Shu-ichiro Inutsuka +1 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Biological dispersal #Physics #Protoplanetary disk #Stars #Stellar wind #Stellar, planetary, and galactic studies #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1093/mnras/staa087
11 pages, 6 figures; corrected Table 2 and Equations (17) and (29); see Erratum at https://doi.org/10.1093/mnras/stab2748
openalex publication_date 2020/01/14 · openalex created_date 2020/01/23 · arxiv created 2021/11/14 · arxiv updated 2021/11/16 · openalex updated_date 2026/08/05
ABSTRACT We investigate the roles of magnetically driven disc wind (MDW) and thermally driven photoevaporative wind (PEW) in the long-time evolution of protoplanetary discs. We start simulations from the early phase in which the disc mass is 0.118 \rm M\odot around a 1 \rm M\odot star and track the evolution until the disc is completely dispersed. We incorporate the mass-loss by PEW and the mass-loss and magnetic braking (wind torque) by MDW, in addition to the viscous accretion, viscous heating, and stellar irradiation. We find that MDW and PEW, respectively, have different roles: magnetically driven wind ejects materials from an inner disc in the early phase, whereas photoevaporation has a dominant role in the late phase in the outer (≳1 au) disc. The disc lifetime, which depends on the combination of MDW, PEW, and viscous accretion, shows a large variation of ∼1–20 Myr; the gas is dispersed mainly by the MDW and the PEW in the cases with a low viscosity and the lifetime is sensitive to the mass-loss rate and torque of the MDW, whereas the lifetime is insensitive to these parameters when the viscosity is high. Even in discs with very weak turbulence, the cooperation of MDW and PEW enables the disc dispersal within a few Myr.