請用此 Handle URI 來引用此文件：
http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/38037完整後設資料紀錄
| DC 欄位 | 值 | 語言 |
|---|---|---|
| dc.contributor.advisor | 闕志鴻 | |
| dc.contributor.author | Yu-Cheng Chen | en |
| dc.contributor.author | 陳宇承 | zh_TW |
| dc.date.accessioned | 2021-06-13T15:57:59Z | - |
| dc.date.available | 2009-07-07 | |
| dc.date.copyright | 2008-07-07 | |
| dc.date.issued | 2007 | |
| dc.date.submitted | 2008-06-02 | |
| dc.identifier.citation | Aarseth, S. J., and Heggie, D. C., 1998, MNRAS, 297, 794
Aarseth, S. J., 2003, Gravitational N-Body Simulations, Press of Syndicate of the University of Cambridge Barnes, J. E. and Hernquist, L., 1996, ApJ, 471, 115 Benson, A. J., Baugh, C. M., Cole, S., Frenk, C. S., and Lacey, C. G., 2000, MNRAS, 316, 107 Binney, J., and Tremaine, S., 1987, Galactic Dynamics, Princeton University Press Dyer, C. C., and Ip, P. S. S., 1993, ApJ, 409, 60 Fernando, R., and Kilgard, Mark J., 2003, The Cg Tutorial, Addison Wesley Professional Hut, P., and Makino, J., 2007, Moving Stars Around, The Maya Open Lab Jing, Y. P., 2000, ApJ, 535, 30 Makino, J., 1991, PASJ, 43, 859 Makino, J., and Aarseth, S. J., 1992, PASJ, 44, 141 Navarro, J. F., Frenk, C. S., and White, S. D. M., 1995, MNRAS, 275, 720 Navarro, J. F., Frenk, C. S., and White, S. D. M., 1996, ApJ, 462, 563 Narasimhan, K. S. V. S., and Alladin, S. M., 1986, Ap&SS, 128, 307 Nitadori, K., Makino, J., and Hut, P., 2006, New Astronomy, 12, 169 Nuijten, Martijn J. J. M., Simard, L., Gwyn, S., and Rottgering, Huub J. A., 2005, ApJ, 626, 77 Portegies Zwart, S. F., Belleman, R. G., and Geldof, P. M., 2007, New Astronomy, 20, 58 Shreiner, D., Woo, M., Neider, J., and Davis, T., 2004, OpenGL Programming Guide 4th Edition, OpenGL Architecture Review Board Spitzer, L., 1987, Dynamical Evolution of Globular Clusters, Princeton University Press Spurzem, R., 1999 JCoAM, 109, 407 | |
| dc.identifier.uri | http://tdr.lib.ntu.edu.tw/jspui/handle/123456789/38037 | - |
| dc.description.abstract | 重力多體問題的模擬，在天文研究中向來扮演重要角色，尤其是利用直接積分法，更可以達到高解析度的結果。但受限於電腦運算效能低落，人們被迫採取近似法以減少運算時間。
由於顯示卡具有多處理器、平行運算的特性，我們利用它取代中央處理器，來計算重力直接積分問題。本實驗室首先建構了顯示卡電腦群，由16台個人電腦與32張顯示卡組成，經實測證明，由顯示卡處理直接多體問題的效能，比起中央處理器的效能快了300多倍。操作顯示卡的方法，以及我們數值模擬的程式碼將被詳細討論。 我們用電腦群模擬星系碰撞的問題，本篇論文主要探討兩個星系碰撞並融合的演化過程，並且討論星系中心二維與三維質量密度的變化。經模擬發現，具有 Sersic model 分布的星系，經碰撞融合後，其 Sersic index 會由小變大，且其變化與初始條件的動能有關係；此外，我們亦發現，不論碰撞前與碰撞後，星系三維密度都遵守 NFW model 的分布。 | zh_TW |
| dc.description.provenance | Made available in DSpace on 2021-06-13T15:57:59Z (GMT). No. of bitstreams: 1 ntu-96-R94222065-1.pdf: 1234283 bytes, checksum: b2ed945e3fa90abea86ea88fd94d2ee0 (MD5) Previous issue date: 2007 | en |
| dc.description.tableofcontents | 口試委員會審定書................................................................................i
序言.......................................................................................................ii 摘要......................................................................................................iii Contents ..............................................................................................iv Chapter 1 Introduction .......................................................................1 Chapter 2 Direct N-Body Simulation ................................................3 2.1 Numerical simulation ......................................................................3 2.2 The Hermite scheme ........................................................................4 2.3 The Ring algorithm .........................................................................7 2.4 Time-step treatments .......................................................................9 Chapter 3 The GPU cluster .............................................................10 3.1 Something about GPU ...................................................................10 3.2 Structure and efficiency of GPU clusters .....................................11 3.3 From Cg and OpenGL to N-body code ........................................13 3.4 Details of our force calculation code .............................................19 Chapter 4 Initial Conditions ............................................................22 4.1 Galaxy cluster halos .......................................................................22 4.2 Density profiles of initial galaxies .................................................23 4.3 Several situations of galactic collisions .........................................24 Chapter 5 Outcome of simulation ...................................................27 5.1 Energy analysis ..............................................................................27 5.2 2D density profile ...........................................................................31 5.3 3D density profile ...........................................................................33 Chapter 6 Conclusions .....................................................................35 6.1 High performance, high accuracy, low cost .................................35 6.2 Future work.....................................................................................35 Reference ...........................................................................................37 Appendix 1. .......................................................................................38 Appendix 2. .......................................................................................40 Appendix 3. .......................................................................................64 | |
| dc.language.iso | en | |
| dc.subject | 質量密度 | zh_TW |
| dc.subject | 直接積分法 | zh_TW |
| dc.subject | 重力多體模擬 | zh_TW |
| dc.subject | 顯示卡 | zh_TW |
| dc.subject | 星系碰撞 | zh_TW |
| dc.subject | gravitational n-body simulation | en |
| dc.subject | density profile | en |
| dc.subject | galactic collisions | en |
| dc.subject | Graphic Processing Units | en |
| dc.subject | direct integrator method | en |
| dc.title | 以繪圖運算器處理多體問題:模擬星系碰撞之動力演化過程 | zh_TW |
| dc.title | Direct N-Body Simulation with Graphic Processing Units: dynamical evolution of galactic collisions | en |
| dc.type | Thesis | |
| dc.date.schoolyear | 96-2 | |
| dc.description.degree | 碩士 | |
| dc.contributor.oralexamcommittee | 黃崇源,吳俊輝 | |
| dc.subject.keyword | 直接積分法,重力多體模擬,顯示卡,星系碰撞,質量密度, | zh_TW |
| dc.subject.keyword | direct integrator method,gravitational n-body simulation,Graphic Processing Units,galactic collisions,density profile, | en |
| dc.relation.page | 66 | |
| dc.rights.note | 有償授權 | |
| dc.date.accepted | 2008-06-04 | |
| 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-96-1.pdf 未授權公開取用 | 1.21 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。