請用此 Handle URI 來引用此文件：
http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/43275完整後設資料紀錄
| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 闕志鴻(Tzi-Hong Chiueh) | |
| dc.contributor.author | Ui-Han Zhang | en |
| dc.contributor.author | 張瑋瀚 | zh_TW |
| dc.date.accessioned | 2021-06-15T01:46:37Z | - |
| dc.date.available | 2011-08-18 | |
| dc.date.copyright | 2011-08-18 | |
| dc.date.issued | 2011 | |
| dc.date.submitted | 2011-08-16 | |
| dc.identifier.citation | [1] NVIDIA (2010). NVIDIA CUDA C Programming Guide (Version 3.2). Santa Clara,
CA: NVIDIA. [2] Pen, U., Trac, H.(2003). A Prime on Eulerian Computational Fluid Dynamics for Astrophysics. PASP,115:303, 321. [3] Roe, P. L. (1981). Approximate Riemann solvers, parameter vectors, and difference schemes. J. Comput. Phys., 43, 357. [4] Schive, H., Tsai, Y., & Chiueh, T. (2010). GAMER: a graphic processing unit accelerated adaptive-mesh-refinement code for astrophysics. ApJS, 186, 457. [5] Schive, H., Zhang, U., & Chiueh, T. (2011). Directionally Unsplit Hydrodynamic Schemes with Hybrid MPI/OpenMP/GPU Parallelization in AMR. arXiv:1103.3373. [6] Stone, J. M., Gardiner, T. A., Teuben, P., Hawley, J. F., & Simon, J. B. (2008). Athena: a new code for astrophysical MHD. ApJS, 178, 137. [7] Toro, E. F. (2009). Riemann solvers and Numerical Methods for Fluid Dynamics. A Practical Introduction (3rd ed.). Berlin: Springer. | |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/43275 | - |
| dc.description.abstract | 本論文中，我完成了繪圖處理晶片(GPU)版本的理想三維磁流體之演算程序。在其中利用包含了磁場內稟限制條件下的傳輸方式(constraint transport)的立體邊角方向性傳輸(corner transport upwind)之演算法，來演算流體及感應方程式。
星際物質通常是由熱氣體與分子雲構成。在此我將展示以聲光效應為基礎的星系形成之機制 | zh_TW |
| dc.description.abstract | We have implemented graphic processing unit (GPU) solvers to the 3D ideal magnetohydrodynamcis (MHD) equations. Corner-transport upwind(CTU) scheme including constraint-transport(CT) method is adopted to evalu¬ate the hydro and induction equation.
Usually, the interstellar medium consists of the hot gas and the molecular cloud. In this thesis we will present the mechanism based on sonoluminescence for the formation of the star. | en |
| dc.description.provenance | Made available in DSpace on 2021-06-15T01:46:37Z (GMT). No. of bitstreams: 1 ntu-100-R98222001-1.pdf: 1408943 bytes, checksum: 20247dd8658e088a4d2449b8abdf875d (MD5) Previous issue date: 2011 | en |
| dc.description.tableofcontents | Contents
Acknowledgements v 摘要 vii Abstract ix Contents xi List of Figures xiii List of Tables xv 1 Introduction 1 2 Description of Numerical Computation 3 2.1 Basic equations‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 3 2.2 Numerical algorithm‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 6 2.2.1 Finite-volume method‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 7 2.2.2 Constraint transport method‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 8 2.2.3 Corner transport upwind scheme‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 11 2.3 GPU Computation‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 13 3 Application in Hydrodynamics 15 3.1 Sonoluminescence‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 15 3.2 The Model for Cooling‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 17 3.3 Modified Numerical Scheme‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 21 xii 4 Results for MHD Computation 27 4.1 Accuracy Tests‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 27 4.1.1 Linear Wave Tests‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 28 4.1.2 Shock Tube Tests‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 32 4.2 Performance Tests‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 36 5 Results for Sonoluminescence Mechanism 39 5.1 Stability of the Molecular Cloud‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 40 5.2 Perturbation Effects‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 42 5.2.1 Standing Wave Interaction‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 43 5.2.2 Frequency, Phase Response‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥ 46 5.2.3 Gaussian Wave Interaction‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥‥· 48 6 Conclusion 51 Bibliography 53 | |
| dc.language.iso | en | |
| dc.subject | 聲光效應 | zh_TW |
| dc.subject | 磁流體 | zh_TW |
| dc.subject | 立體邊角方向性傳輸 | zh_TW |
| dc.subject | 磁場內稟限制條件下的傳輸 | zh_TW |
| dc.subject | 星際物質 | zh_TW |
| dc.subject | interstellar medium | en |
| dc.subject | MHD | en |
| dc.subject | CTU | en |
| dc.subject | sonoluminescence | en |
| dc.subject | CT | en |
| dc.title | 使用顯示卡計算磁流體及其在純流體情況下的應用 | zh_TW |
| dc.title | MHD GPU Computation and Application in the Pure Hydro case | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 99-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 賴詩萍(Shih-Ping Lai),呂聖元(Sheng-Yuan Liu) | |
| dc.subject.keyword | 磁流體,立體邊角方向性傳輸,磁場內稟限制條件下的傳輸,星際物質,聲光效應, | zh_TW |
| dc.subject.keyword | MHD,CTU,CT,interstellar medium,sonoluminescence, | en |
| dc.relation.page | 53 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2011-08-16 | |
| dc.contributor.author-college | 理學院 | zh_TW |
| dc.contributor.author-dept | 物理研究所 | zh_TW |
| 顯示於系所單位： | 物理學系 | |
文件中的檔案：
| 檔案 | 大小 | 格式 | |
|---|---|---|---|
| ntu-100-1.pdf 未授權公開取用 | 1.38 MB | Adobe PDF |
系統中的文件，除了特別指名其著作權條款之外，均受到著作權保護，並且保留所有的權利。