1. マグネター研究の現状 ・観測のまとめ ・エネルギー源 ・太陽フレアモデルとの比較 ・定常 X 線・ γ 線の放射モデル ・ QED 効果 ・ QPO ・今後の課題

2. SGR1900+14

3. Ulysses data for the August 1998 giant flare

4. SGR 1806-20

5. ・ recurrent bursts duration ~0.1 s rise times < 10 ms   ~30 keV (kT BB ~9 keV) L X (10 2 - 10 4 ) L edd (magnetic confinement) energy release Q ~< 10 42 erg association SNRs (1SGR, 3AXPs) ・ giant outbursts duration ~ 200, ~300 s initial spike L X ~10 6 L edd, Q >10 44 erg, kT~300, 500 keV tail Q ~ 10 44 erg, kT~20, 30 keV

6. ・ hyper flare initial spike duration ~0.2 s rise times < 1 ms   kT BB ~175 keV L X ~10 9 L Edd energy release Q 5 × 10 46 erg tail duration 380 s   kT BB ~ 4-9 keV energy release Q 10 44 erg

7. ・ persistent component from SGRs & AXPs L X 10 34 - 10 36 erg spectrum BB(~0.5keV) + PL(2-3) pulsation 5 - 12 s p-dot 10 -12 - 10 -10 s/s τ sd 10 3 - 10 5 yrs B(dipole field) 6 × 10 13 - 10 15 G ・ energy source ×Rotational energy ×Thermal energy ×Strain energy ○ magnetic energy

8. 太陽フレアモデルの応用 ・パーカー不安定による磁束管の浮上 ・対流による磁束管の捩り上げ（エネルギーの蓄積） ・リコネクションを伴う不安定性の発生（エネルギー解放） Model of repeated soft gamma ray bursts [Thompson and Duncan, MNRAS, 1995] (Duncan) magnetar 10 km

9. ・ unwinding and twist plastic unwinding of the internal fieldslow, plastic motion flux tube rise twist in the magnetosphere reconnection ・ tearing instability Alfven time Resistive time Tearing mode growth time + reconnection

11. Repeated bursts vs. Giant flares (Duncan) Localized energy release Repeated bursts Global energy release due to entire crust- core magnetic instability Giant flares [Thompson and Duncan, MNRAS, 1995 / ApJ 2001]

12. ・ X-ray and γ-ray emission Initial spike ---> jet Pulsating tail ---> evaporating trapped fireball (Thompson and Duncan, MNRAS,1995) A photon pair plasma (e - +e + ) Magnetic reconnection, or Nonlinear damping of waves

13. Persistent component Gotz et el., 2007

15. 2006 Input energy --> 99% -->neutrino Q ~ 10 49 - 10 50 ergs

18. A QED Model fast MHD wave e +- pair production synchrotron emission hard X rays Heyl & Hernquist 2005 Persistent Hard X-Ray Emission

19. ・ pair creation ・ photon splitting Baring & Harding1998 QED Effects

20. Camilo et al. 2000

22. QPO in the hyper flare of SGR 1806-20 (P=7.56 s) 92.5 Hz at t=170-220 s 50 Hz at t=45-175 ms and at t=430-567 ms ~18Hz, ~30Hz at t~200-300 s

26. Global seismic vibration model

27. The ratio of first radial overtone to fundamental frequency 30Hz 625 Hz --->

28. ・振動数 よく合っている ・ SGR 1806-20 の 18Hz, 26Hz はでない ・ SGR 1806-20 と SGR 1900+14 の振動数の違い ---> M, R, B の違い ・ SGR 1806-20 30Hz fundamental 625Hz first overtone ---> H/R ~ 0.1-0.13 ・ strange star --->much thinner crust ---> >>625Hz ・重力波 ---> 弱く advanced LIGO でも無理 課題 ・ core-crust coupling ・ dipole field and toroidal internal field

29. To be studied ・ formation of ultra-strong magnetic fields ・ unwinding and twist ・ reconnection & particle acceleration ・ emission & spectra