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マグネター研究の現状

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. SGR1900+14. Ulysses data for the August 1998 giant flare. SGR 1806-20. ・ recurrent bursts duration ~0.1 s rise times < 10 ms

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マグネター研究の現状

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  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 eg ~30 keV (kTBB~9 keV) LX (102 - 104) Ledd (magnetic confinement) energy release Q ~< 1042 erg association SNRs (1SGR, 3AXPs) ・giant outbursts duration ~ 200, ~300 s initial spike LX ~106 Ledd, Q >1044 erg, kT~300, 500 keV tail Q ~ 1044 erg, kT~20, 30 keV

  6. ・hyper flare initial spike duration ~0.2 s rise times < 1 ms eg kTBB~175 keV LX ~109 LEdd energy release Q 5 × 1046 erg tail duration 380 s eg kTBB~ 4-9 keV energy release Q 1044 erg

  7. ・persistent component from SGRs & AXPs LX 1034 - 1036 erg spectrum BB(~0.5keV) + PL(2-3) pulsation 5 - 12 s p-dot 10-12 - 10-10 s/s τsd 103 - 105 yrs B(dipole field) 6× 1013 - 1015 G ・energy source ×Rotational energy ×Thermal energy ×Strain energy ○ magnetic energy

  8. (Duncan) 10 km magnetar magnetar 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） [Thompson and Duncan, MNRAS, 1995] Model of repeated soft gamma ray bursts

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

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

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

  12. Persistent component Gotz et el., 2007

  13. 2006 Input energy --> 99% -->neutrino Q ~ 1049 - 1050 ergs

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

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

  16. Camilo et al. 2000

  17. 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

  18. Global seismic vibration model

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

  20. ・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

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

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