| 报告题目： |
Orbit design, deployment and TDI simulation for the new LISA and some thoughts on the TDI simulation for TIANQIN |
| 报告人： |
倪维斗 |
| 报告人单位： |
台湾 清华大学 |
| 报告时间： |
2017年6月22日 上午10:00 |
| 报告地点： |
引力中心三楼会议室 |
| 报告人简介： |
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倪维斗教授为台湾清华大学物理系荣誉退休教授，多年来从事引力理论和实验以及相关领域的教学与研究工作，曾获加州理工学院物理及数学博士，分别在中国科学院国家天文台、紫金山天文台、上海理工大学等任客座教授。 |
| 报告摘要： |
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In order to attain the requisite sensitivity, laser frequency noise must be suppressed to below the secondary noises such as the optical path noise, acceleration noise etc. In early investigations, we have performed the numerical simulation of the time delay interferometry (TDI) for original LISA, ASTROD-GW and eLISA together with a LISA-type mission with a nominal arm length of 2 × 106 km using the CGC 2.7.1 ephemeris framework. In this talk, we follow the same procedure to simulate the TDI numerically for the new LISA mission and the TAIJI mission together with LISA-like missions of arm length 1×106 km, 2×106 km, 4×106 km, 5×106 km and 6×106 km. To do this, we work out a set of 6-year optimized mission orbits of each mission starting at March 22, 2028 using the CGC 2.7.1 ephemeris framework. We then use numerical method to calculate the residual optical path differences of first-generation TDI configurations - Michelson X, Y & Z; Sagnac α, β & γ; Relay U, V & W; Beacon P, Q & R; Monitor E, F & G --- and the second generation TDI configurations - 2 arm type [ab, ba]'s; [aabb, bbaa]'s; [abab, baba]'s; [abba, baab]'s; Sagnac-type α12-1, α12-2 & α12-3. We compile and compare the resulting differences of various TDI configurations due to the different arm lengths for various LISA-like mission proposals and for the ASTROD-GW mission proposal. I will also present some thoughts on the TDI simulation for TIANQIN and discuss with you about how to approach it both experimentally and numerically. |
