1. K. Ioka (Osaka U.) N. Sago (Kyoto U.) T. Nakamura (Kyoto U.)
スペース重力波アンテナWG第２回ミーティング
GRBs with GW memory
K. Ioka (Osaka U.)
N. Sago (Kyoto U.)
T. Nakamura (Kyoto U.)

2. 1. Introduction GRB: brightest object but mystery Ｅｘｔｅｒｎａｌ ｓｈｏｃｋｓ ？
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ＩＳＭ
Ｉｎｔｅｒｎａｌ ｓｈｏｃｋｓ
Luminosity
time

3. To see the center, photon but GW Guaranteed GW: Jet acceleration
Break in afterglow
To see the center, photon but GW
Guaranteed GW: Jet acceleration

4. 2. GW memory: point mass case
Burst with memory

5. Point mass
No beaming
Photon case

6. 3. GW memory: GRB jet case
① Jet
Point mass case
Thin shell case

7. Point approximation is OK for Dq<g-1 or qv>Dq
Dh is reduced at qv<Dq
Dt～r0g[1-cos(qv+Dq)]～r0g(qv+Dq)2/2

8. Counter jet
We will ignore Dhcounter (<Dhforward)

9. ② Deceleration at internal shock
Radiation
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Kinetic energy
Internal energy
If radiation is not emitted
Even if radiation is emitted

10. ③ Not a single explosion
GRB light curve

11. 4. Detectability
Single burst

12. Energy
Event rate

13. GRB light curve as a template

14. 5. Summary GRB jet emits GW with memory DECIGO may detect GRB@10Mpc
Ultimate
⇒ information for, e.g., eg
Light curve may be used as template