1 / 29

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

oholt
Download Presentation

マグネター研究の現状

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related