TY - JOUR
T1 - Theoretical Models of Protostellar Binary and Multiple Systems with AMR Simulations
AU - Matsumoto, Tomoaki
AU - Tokuda, Kazuki
AU - Onishi, Toshikazu
AU - Inutsuka, Shu Ichiro
AU - Saigo, Kazuya
AU - Takakuwa, Shigehisa
N1 - Funding Information:
Numerical computations were carried out on Cray XC30 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. This research was supported by JSPS KAKENHI Grant Numbers 26400233, 26287030, 24244017, 23540270.
Publisher Copyright:
© Published under licence by IOP Publishing Ltd.
PY - 2017/5/30
Y1 - 2017/5/30
N2 - We present theoretical models for protostellar binary and multiple systems based on the high-resolution numerical simulation with an adaptive mesh refinement (AMR) code, SFUMATO. The recent ALMA observations have revealed early phases of the binary and multiple star formation with high spatial resolutions. These observations should be compared with theoretical models with high spatial resolutions. We present two theoretical models for (1) a high density molecular cloud core, MC27/L1521F, and (2) a protobinary system, L1551 NE. For the model for MC27, we performed numerical simulations for gravitational collapse of a turbulent cloud core. The cloud core exhibits fragmentation during the collapse, and dynamical interaction between the fragments produces an arc-like structure, which is one of the prominent structures observed by ALMA. For the model for L1551 NE, we performed numerical simulations of gas accretion onto protobinary. The simulations exhibit asymmetry of a circumbinary disk. Such asymmetry has been also observed by ALMA in the circumbinary disk of L1551 NE.
AB - We present theoretical models for protostellar binary and multiple systems based on the high-resolution numerical simulation with an adaptive mesh refinement (AMR) code, SFUMATO. The recent ALMA observations have revealed early phases of the binary and multiple star formation with high spatial resolutions. These observations should be compared with theoretical models with high spatial resolutions. We present two theoretical models for (1) a high density molecular cloud core, MC27/L1521F, and (2) a protobinary system, L1551 NE. For the model for MC27, we performed numerical simulations for gravitational collapse of a turbulent cloud core. The cloud core exhibits fragmentation during the collapse, and dynamical interaction between the fragments produces an arc-like structure, which is one of the prominent structures observed by ALMA. For the model for L1551 NE, we performed numerical simulations of gas accretion onto protobinary. The simulations exhibit asymmetry of a circumbinary disk. Such asymmetry has been also observed by ALMA in the circumbinary disk of L1551 NE.
UR - http://www.scopus.com/inward/record.url?scp=85020472540&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85020472540&partnerID=8YFLogxK
U2 - 10.1088/1742-6596/837/1/012009
DO - 10.1088/1742-6596/837/1/012009
M3 - Conference article
AN - SCOPUS:85020472540
SN - 1742-6588
VL - 837
JO - Journal of Physics: Conference Series
JF - Journal of Physics: Conference Series
IS - 1
M1 - 012009
T2 - 11th International Conference on Numerical Modeling of Space Plasma Flows, ASTRONUM 2016
Y2 - 6 June 2016 through 10 June 2016
ER -