2013 Fiscal Year Final Research Report
Star formation in turbulent cloud cores with magnetic diffusion
| Project/Area Number |
23540270
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Multi-year Fund |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | Hosei University |
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Principal Investigator |
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| Project Period (FY) |
2011 – 2013
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| Keywords | 星形成 / 星間ガス / 数値シミュレーション / 適合格子細分化法 |
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| Research Abstract |
A molecular cloud core undergoes gravitational collapse to form a protostar and protoplanetary disk. Observations suggest that molecular cloud cores have magnetic field and turbulence. The magnetic field has a dissipative mechanism especially in the high-density gas.
In this study, we investigated collapse of magnetized and turbulent molecular cloud cores, taking account of magnetic dissipation. We fallowed the evolution of the cloud cores from onset of collapse to formation of a protostar and protoplanetary disk, by using high-resolution adaptive mesh refinement (AMR) simulations. All the cloud cores produce protoplanetary disks irrespective of assumed strengths of magnetic field and turbulence. There is a tendency that a strong magnetic field model shows slower growth of a protoplanetary disk. The strong magnetic field models exhibit cavities in the infalling envelopes, which are caused by the interchange instability of the magnetic field.
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[Journal Article] Molecular Clumps and Infrared Clusters in the S247, S252, and BFS52 Regions2013
Author(s)
Shimoikura, Tomomi; Dobashi, Kazuhito; Saito, Hiro; Matsumoto, Tomoaki; Nakamura, Fumitaka; Nishimura, Atsushi; Kimura, Kimihiro; Onishi, Toshikazu; Ogawa, Hideo
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Journal Title
The Astrophysical Journal
Volume: Volume 768, Issue 1
Pages: 27
DOI
Peer Reviewed
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