TY - GEN
T1 - Radiation magnetohydrodynamic simulations of protostellar core formation
AU - Tomida, Kengo
N1 - Funding Information:
KT is supported by the Research Fellowship from the Japan Society for the Promotion of Science. Numerical computations were partly performed on NEC SX-9 at Center for Computational Astrophysics of National Astronomical Observatory of Japan, at Japan Aerospace Exploration Agency and at Osaka University.
Publisher Copyright:
© Springer International Publishing Switzerland 2014.
PY - 2014
Y1 - 2014
N2 - We perform 3D nested-grid radiation magnetohydrodynamic (RMHD) simulations of the formation of proto-stellar cores from molecular cloud cores with and without the Ohmic dissipation of magnetic fields. In the ideal RMHD models, the evolution of the protostellar core is very similar to that in the spherically symmetric non-rotating model due to the efficient angular momentum transport. However, if the resistivity presents, the angular momentum transport is considerably suppressed due to the loss of magnetic flux, and rotationally-supported circumstellar disks are rapidly built up in the vicinity of the protostellar cores. Magnetic fields are amplified by rotation and fast outflows are launched from the protostellar cores via magnetic pressure gradient force. To our knowledge, these are the first 3D RMHD simulations resolving the protostellar cores in the world.
AB - We perform 3D nested-grid radiation magnetohydrodynamic (RMHD) simulations of the formation of proto-stellar cores from molecular cloud cores with and without the Ohmic dissipation of magnetic fields. In the ideal RMHD models, the evolution of the protostellar core is very similar to that in the spherically symmetric non-rotating model due to the efficient angular momentum transport. However, if the resistivity presents, the angular momentum transport is considerably suppressed due to the loss of magnetic flux, and rotationally-supported circumstellar disks are rapidly built up in the vicinity of the protostellar cores. Magnetic fields are amplified by rotation and fast outflows are launched from the protostellar cores via magnetic pressure gradient force. To our knowledge, these are the first 3D RMHD simulations resolving the protostellar cores in the world.
UR - http://www.scopus.com/inward/record.url?scp=84959569537&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84959569537&partnerID=8YFLogxK
U2 - 10.1007/978-3-319-03041-8_6
DO - 10.1007/978-3-319-03041-8_6
M3 - Conference contribution
AN - SCOPUS:84959569537
SN - 9783319030401
T3 - Astrophysics and Space Science Proceedings
SP - 35
EP - 39
BT - The Labyrinth of Star Formation - Conference Dedicated to Prof. Anthony Whitworth
A2 - Goodwin, Simon
A2 - Stamatellos, Dimitris
A2 - Ward-Thompson, Derek
PB - Kluwer Academic Publishers
T2 - Conference on Labyrinth of Star Formation dedicated to Prof. Anthony Whitworth, 2012
Y2 - 1 June 2012
ER -