| Project/Area Number |
12640269
|
|---|
| Research Category |
Grant-in-Aid for Scientific Research (C)
|
| Allocation Type | Single-year Grants |
|---|
| Section | 一般 |
|---|
| Research Field |
素粒子・核・宇宙線
|
|---|
| Research Institution | KYOTO UNIVERSITY (2003)
Osaka University (2000-2002) |
|---|
Principal Investigator |
SASAKI Misao Yukawa Institute, Professor, 基礎物理学研究所, 教授 (70162386)
|
|---|
| Co-Investigator(Kenkyū-buntansha) |
TAGOSHI Hideyuki Osaka University, Assistant, 大学院・理学研究科, 助手 (30311765)
|
|---|
| Project Period (FY) |
2000 – 2003
|
| Project Status |
Completed (Fiscal Year 2003)
|
| Budget Amount *help |
¥4,000,000 (Direct Cost: ¥4,000,000)
Fiscal Year 2003: ¥800,000 (Direct Cost: ¥800,000)
Fiscal Year 2002: ¥800,000 (Direct Cost: ¥800,000)
Fiscal Year 2001: ¥1,100,000 (Direct Cost: ¥1,100,000)
Fiscal Year 2000: ¥1,300,000 (Direct Cost: ¥1,300,000)
|
|---|
| Keywords | black hole / gravitutional wave / radiation reaction / self regularization / 重力波天文学 / 重力波源 / 自己力の正則化 / 自己力正則化 / 自己重力正則化 / コンパクト連星 / ポストニュートン展開 / 自己重力の反作用 |
|---|
| Research Abstract |
In recent years, much attention has been paid to establishing the basis for gravitational wave astronomy, that is, to understand physics of gravitational wave sources accurately.
In this project, adopting the black hole perturbation approach, we focused on the orbital evolution of a binary system with a supermassive black hole and a compact star that includes gravitational radiation force. In this approach, a compact star is approximated as a point. particle and this requires us to regularize the reaction force acting on it. To derive the regularized reaction force, it is necessary to solve a so-called gauge problem as well as to construct an accurate and efficient method of regularization.
To solve the gauge problem, we proposed two methods: One is to regularize the reaction force in the harmonic gauge and the other is to do so in the Regge-Wheeler gauge. Through this research, we made clear how the gauge problem can be solved.
As for constructing an efficient method of regularization, we developed an analytical method based on the post-Newton expansion. The advantage of this method is, though it needs the post-Newton expansion, once the calculation is done it can be applied to any orbit.
At present, we are investigating the necessary post-Newton order for an actual computation of the orbital evolution, and it will be made clear in the near future.
|
