TY - JOUR
T1 - Self-gravitational collapse of a magnetized cloud core
T2 - Proceedings of the 18th International Conference
AU - Matsumoto, Tomoaki
AU - Machida, Masahiro N.
AU - Tomisaka, Kohji
AU - Hanawa, Tomoyuki
N1 - Funding Information:
Numerical computations were carried out onVPP5000 at the Astronomical Data Analysis Center of the National Astronomical Observatory, Japan, which is an inter-university research institute of astronomy operated by the Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT). This study was financially supported in part by Grants-in-Aid for the Encouragement of Young Scientists (12740123, 14740134), for Scientific Research on Priority Areas (A) (13011204) from MEXT, and for Scientific Research (C) (13640237) from the Japan Society of Promotion of Science (JSPS).
PY - 2004/12/1
Y1 - 2004/12/1
N2 - We investigate self-gravitational collapse of magnetized molecular cloud cores and formation of the outflow. We employ a nested grid in order to resolve fine structures of protostar and outflow generation, of which size is as small as 1 AU, and to follow the whole structure of the molecular cloud core, of which radius reaches 0.1-1 pc, simultaneously. The nested grid allows us to follow the evolution of the cloud core with the high dynamic range of 105-106 in the spatial resolution. In this paper, we introduce implementations of the self-gravitational MHD nested grid code and show applications to early stages in star formation: gravitational collapse of cloud core, "first core" formation, and bipolar outflow ejection. In both cases of single and binary star formation, magnetic fields play important role in the outflow formation. The outflow region has extremely low beta regions of β= 10 -6-10-3, and our code shows no sign of numerical instability even in these low-beta regions.
AB - We investigate self-gravitational collapse of magnetized molecular cloud cores and formation of the outflow. We employ a nested grid in order to resolve fine structures of protostar and outflow generation, of which size is as small as 1 AU, and to follow the whole structure of the molecular cloud core, of which radius reaches 0.1-1 pc, simultaneously. The nested grid allows us to follow the evolution of the cloud core with the high dynamic range of 105-106 in the spatial resolution. In this paper, we introduce implementations of the self-gravitational MHD nested grid code and show applications to early stages in star formation: gravitational collapse of cloud core, "first core" formation, and bipolar outflow ejection. In both cases of single and binary star formation, magnetic fields play important role in the outflow formation. The outflow region has extremely low beta regions of β= 10 -6-10-3, and our code shows no sign of numerical instability even in these low-beta regions.
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U2 - 10.1016/j.cpc.2004.06.033
DO - 10.1016/j.cpc.2004.06.033
M3 - Conference article
AN - SCOPUS:10444290679
SN - 0010-4655
VL - 164
SP - 229
EP - 236
JO - Computer Physics Communications
JF - Computer Physics Communications
IS - 1-3
Y2 - 7 September 2003 through 10 September 2003
ER -