| Project/Area Number |
17540212
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | Chiba University |
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Principal Investigator |
HANAWA Tomoyuki Chiba University, Center for Frontier Science, Professor, 先進科学研究教育センター, 教授 (50172953)
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| Co-Investigator(Kenkyū-buntansha) |
MATSUMOTO Tomoaki Hosei University, Department of Humanity and Environment, Associate Professor, 人間環境学部, 助教授 (60308004)
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| Project Period (FY) |
2005 – 2006
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| Project Status |
Completed (Fiscal Year 2006)
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| Budget Amount *help |
¥3,500,000 (Direct Cost: ¥3,500,000)
Fiscal Year 2006: ¥1,200,000 (Direct Cost: ¥1,200,000)
Fiscal Year 2005: ¥2,300,000 (Direct Cost: ¥2,300,000)
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| Keywords | Theoretical Astronomy / Star Formation / Numerical Simulation / Binary / Accretion |
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| Research Abstract |
Protostears and young stellar objects are characterized by their active gas accretion. Since most protostars are members of binary and multiple stars, it is important to assess the role of their companions on the gas accretion. However, the studies are very limited in part by technical difficulties. By employing nested grid technique we have succeeded in simulations of gas accretion in a binary system. They cover both the circumbinary disk and circumstellar disks simultaneously with high spatial resolution. We have found that pairs of spiral shock waves are excited in the circumbinary disk. A pair of the spiral shocks corotates with the binary while the other pairs rotate more slowly. When the corotating spiral shock waves get ahead of the others, the gas density rises near L2 point and the inflow onto the binary increases. Interaction between the other pairs of shock waves induce gas accretion within the circumbinary disk. It is also shown in simulations of high spatial resolution that the turbulence arises near L1 point. As related works we have performed simulations of binary formation. We also developed AMR code capable for still higher spatial resolution and numerical scheme for strong MHD shock waves for future studies.
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