| Project/Area Number |
07304025
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| Research Category |
Grant-in-Aid for Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Section | 総合 |
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| Research Field |
Astronomy
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| Research Institution | Niigata University |
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Principal Investigator |
TOMISAKA Kohji Faculty of Education, Niigata University, Associate Professor, 教育学部, 助教授 (70183879)
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| Co-Investigator(Kenkyū-buntansha) |
YOSHIDA Tatsuo Faculty of Science, Ibaragi University, Asscociate Professor, 理学部, 助教授 (60241741)
GOUDA Naoteru School of Science, Osaka University, Asscociate Professor, 理学部, 助教授 (50202073)
MATSUMOTO Ryoji Faculty of Science, Chiba University, Asscociate Professor, 理学部, 助教授 (00209660)
HANAWA Tomoyuki School of Science, Nagoya University, Asscociate Professor, 理学部, 助教授 (50172953)
NOGUCHI Masafumi School of Science, Tohoku University, Asscociate Professor, 理学部, 助教授 (20241515)
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| Project Period (FY) |
1995 – 1996
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| Project Status |
Completed (Fiscal Year 1996)
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| Budget Amount *help |
¥6,100,000 (Direct Cost: ¥6,100,000)
Fiscal Year 1996: ¥2,300,000 (Direct Cost: ¥2,300,000)
Fiscal Year 1995: ¥3,800,000 (Direct Cost: ¥3,800,000)
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| Keywords | Numerical Methods / Supercomputers / Parallel Computers / Adaptive Scheme |
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| Research Abstract |
We are able to use several kinds of supercomputers in the field of astrophysics. They are vector-parallel machines, massive parallel machines, and special purpose machines. To bring their full play, we have to choose the most effective numerical method. Although the field of numerical astrophysics is wide : from the solar system to the universe, there must be a common bottleneck which should be broken to make a breakthrough. This project were planned to answer the above point.
1.The (magneto-) hydrodynamics equation is one of the most important ones in the astrophysics. Equations for the unsteady hydrodynamics are hyperbolic-type. In this case, it is shown that data are easily divided and allocated onto a number of processors. We are able to parallelize the code and achive high performance.
2.On the other hand, the elliptical-type equation, such as the Poisson equation, which is also one of the most important ones in the astrophysics, is poorly parallelized. This is mainly due to the fact that it is difficult to parallelize the preconditioning of the coefficient matrix.
3.As a Poisson solver, we have found that "multigrid iteration method" is fast compared to the ordinary solvers which were poorly parallelized. We have measured the CPU time necessary to solve the Poisson equation once by this method. It is only a half of the time required to solve the magnetohydrodynamics equations for one time step.
4.It is shown that the nested grid technique is very efficient for a problem with a large spatial dynamic range. It uses a number of grids ; coarser grids covers a whole numerical box, while finer ones cover a region which require a fine spatial resolution.
5.To proceed from the nested grid scheme to a fully adaptive one, we have to develop a method of creation/destruction of the grids. This requires the code to understand which part should be calculated closely.
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