10.5281/zenodo.4567927
https://zenodo.org/records/4567927
oai:zenodo.org:4567927
Takasao, Shinsuke
Shinsuke
Takasao
0000-0003-3882-3945
Osaka University
Tomida, Kengo
Kengo
Tomida
Tohoku University
Iwasaki, Kazunari
Kazunari
Iwasaki
National Astronomical Observatory of Japan
Suzuki, Takeru
Takeru
Suzuki
University of Tokyo
3D MHD simulations of an accreting young star
Zenodo
2021
Young stars
Magnetospheric accretion
MHD simulations
Wolk, Scott
Scott
Wolk
2021-02-26
Poster
10.3847/2041-8213/ab22bb
10.3847/1538-4357/aab5b3
10.5281/zenodo.4565628
https://zenodo.org/communities/coolstars20half
Creative Commons Attribution 4.0 International
Young stars such as protostars and pre-main-sequence stars evolve via the interaction with the surrounding accretion disks. It is believed that stellar and disk magnetic fields play important roles in shaping the accretion structure and exchanging the angular momentum between the stars and the disks. However, because of the complexity of gas dynamics around the stars, the star-disk interaction remains poorly understood, which makes the construction of the stellar evolution models difficult. To reveal the interaction processes, we have been performing 3D magnetohydrodynamic simulations of accretion onto a young star with different stellar magnetic fields. In the case of a weakly magnetized, magnetosphere-free star, we found that failed disk wind becomes supersonic, high-latitude accretion flows onto the star (Takasao et al. 2018). This result may explain the reason why Herbig Ae/Be stars show fast accretion. In a different model with stronger disk fields, we showed that the star can produce recurrent explosions via magnetic reconnection (Takasao et al. 2019). We consider that the mechanism is relevant to protostellar flares in class-0/I protostars. In addition to the above two models, we have been investigating the magnetospheric accretion which is very relevant to classical T-Tauri stars. In this talk, we will introduce our 3D modeling and discuss how the star-disk interaction changes depending on the stellar and disk field strengths.