Abstract
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.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
References
R.B. Larson, MNRAS 145, 271 (1969)
M.R. Bate, ApJL 508, L95 (1998).
K. Tomisaka, ApJL 502, L163+ (1998).
M.N. Machida, S.i. Inutsuka, T. Matsumoto, ApJL 647, L151 (2006).
M.N. Machida, S.i. Inutsuka, T. Matsumoto, ApJ 676, 1088 (2008).
M.R. Bate, MNRAS 404, L79 (2010).
B. Commerçon, P. Hennebelle, E. Audit, G. Chabrier, R. Teyssier, A&A 510, L3+ (2010).
K. Tomida, K. Tomisaka, T. Matsumoto, K. Ohsuga, M.N. Machida, K. Saigo, ApJL 714, L58 (2010).
Z.Y. Li, R. Krasnopolsky, H. Shang, ApJ 738, 180 (2011).
K. Tomida, K. Tomisaka, T. Matsumoto, Y. Hori, S. Okuzumi, M.N. Machida, K. Saigo, ArXiv e-prints (2012)
K. Tomida, Radiation Magnetohydrodynamic Simulations of Star Formation Processes. Ph.D. thesis, The Graduate University for Advanced Studies (2012)
J.K. Truelove, R.I. Klein, C.F. McKee, J.H. Holliman, II, L.H. Howell, J.A. Greenough, ApJL 489, L179 (1997).
T. Miyoshi, K. Kusano, Journal of Computational Physics 208, 315 (2005).
C.D. Levermore, G.C. Pomraning, ApJ 248, 321 (1981).
C.D. Levermore, Journal of Quantitative Spectroscopy and Radiative Transfer 31, 149 (1984).
S. Okuzumi, ApJ 698, 1122 (2009).
V. Alexiades, G. Amiez, P. Gremaud, Communications in numerical methods in engineering 12(1), 31 (1996)
H. Masunaga, S.i. Inutsuka, ApJ 531, 350 (2000).
M.N. Machida, T. Matsumoto, MNRAS 413, 2767 (2011).
Acknowledgements
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.
Author information
Authors and Affiliations
Corresponding author
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 2014 Springer International Publishing Switzerland
About this paper
Cite this paper
Tomida, K. (2014). Radiation Magnetohydrodynamic Simulations of Protostellar Core Formation. In: Stamatellos, D., Goodwin, S., Ward-Thompson, D. (eds) The Labyrinth of Star Formation. Astrophysics and Space Science Proceedings, vol 36. Springer, Cham. https://doi.org/10.1007/978-3-319-03041-8_6
Download citation
DOI: https://doi.org/10.1007/978-3-319-03041-8_6
Published:
Publisher Name: Springer, Cham
Print ISBN: 978-3-319-03040-1
Online ISBN: 978-3-319-03041-8
eBook Packages: Physics and AstronomyPhysics and Astronomy (R0)