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New Scenario of Plasma Evolution in SNRs

Std (Shell) SNRs. Shock Heated Plasma. IP. Non-Std SNRs. A Mid-Term Report of the Key Project (AO6). New Scenario of Plasma Evolution in SNRs. NEI describes the plasma evolution in standard SNRs (shell-like ): Ionizing Plasma (IP). ● SN1006. ● Tycho. CIE

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New Scenario of Plasma Evolution in SNRs

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  1. Std (Shell) SNRs Shock Heated Plasma IP Non-Std SNRs A Mid-Term Report of the Key Project (AO6) New Scenario of Plasma Evolution in SNRs NEI describes the plasma evolution in standard SNRs (shell-like ): Ionizing Plasma (IP) ● SN1006 ● Tycho CIE Colisional Ionization Equilibrium ? RP Recombining Plasma (RP) may traces a missing branch of the plasma in non-standard SNRs (e.g. MM). What is a missing event ? • How is the evolution in a missing branch

  2. Key Project (AO6) KES 79 2011/4/23 G272.2-3.2 5/28+11/12 G290.1-0.86/25 G292.0+1.87/22 G349.7+0.2 9/29 G350.1-0.3 9/17 Kes 27 2012/2/20 ? G277 2012 (AO7) We have only 0.5—0.8 year for data analysis,hence the analysis is still preliminary phase. I therefore include the Pre-KP, the Long Observation (AO5). W 28 W 44 Long Observation (Pre-KP)

  3. Best-fit RP model kTe=0.40 keV kTz: 0.5—1.0 keV (z-dependent) W 28 Model χ2/d.o.f 1-CIE 2160/641 2-CIE 1753/639 Multi-kTz 893/634 1-kTe Sawada & Koyama 2012, PASJ accepted, arXiv:1202.3125

  4. Si ■ ■S ■Mg ■Fe ■ Ne The best-fit temperatures (kTz) for kTe=0.40 keV

  5. 0.8 0.2 (keV) kTe 1.2 0.3 (keV) kTz W 28 Spatial distribution of kTe and kTz Shocked MC TeV γ-rays

  6. kTe and kTz distributions vs distances from candidate sources No correlation kTe kTz Ionization by High energy particle X Thermal conduction to Molecular cloud X

  7. Tz Te Tz Te Dense CSM Photo Ionization γ-rayburst Time Time Rarefaction:electron cooling by adiabatic expansion (Itoh & Masai 89) Thin ISM Photo Ionization: highly ionization by X-rays (γ-ray after glow) (Kawasaki, 02, 05)

  8. Si ■ ■S ■Mg ■Fe ■ Ne The best-fit temperatures (kTz)

  9. /n (yr) Ｒａｒｅｆａｃｔｉｏｎ Ｐｈｏｔｏ　 Ｉｏｎｉｚａｔｉｏｎ /n (yr)

  10. Std (Shell) SNRs IP: Standard Evolution Heating Non-Std SNRs CIE Missing Event Missing Branch of Evolution Missing Event: Rarefaction Missing Branch:Recombining (RP)

  11. Best-fit Model kTz=1.1 kTe=0.48 Log(nt)=11.85 W 44 Chi2/d.o.f 1-CIE 2121/353 1-RP 1175/352 Tz+Te+nt 536/349 Energy (keV) Uchida et al. 2012, to be submitted

  12. W 44 Spatial distribution of Initial kTz, kTe and Recombining time-scale (log nt) Initial kTzkTent

  13. Results of Key Project SNRs: QL by Katsuda

  14. All except G290 &G350 seem to be IP (Te> Tz), but ! S-Lya These have strong Fe-K shell lines, so what ?

  15. Fe Ionization state is nearly He-like, in sharp contrast to typical SNRs such as Tycho, Kepler, SN1006 and RCW 86 (Neutral --Ne-like) G349 G350 Temperature kTz 1.2 keV 1.0 keV Abundance Fe 1.0 (0.9-1.1) 2.1 (1.7-2.6) Ni 3.5 (2.1-5.0) 15 (7-25)

  16. 6.4 6.7 keV W49B : Extreme RP Te= 1.3 Tz=2.5 G349 1.2 1.2 G350 1.0 1.0 1.0 0.3 Tycho: Extreme IP All the SNRs, more or less, had an event of RP production

  17. AO7 target: G 337.2-0.7 ASCA Spectrum Fe-K

  18. The End

  19. Very strong Cr, M, Ni 3C397 G344 Tycho Fe 12.5 +/- 1.3 Ni 90.8 +/- 15.8 Line E c Flux 5.61 9.72E-06 6.10 4.46E-06 (Yamaguchi et al. submitted to ApJ

  20. Thin thermal spectra = 2 Type of SNRs 1. Shell-like SNR Canonical evolution of dynamics：　　 Canonical model & analysis:NEI, PSHOCK  Many proposal, Observations & Papers 2. Mixed Morphology (MM) SNR No Canonical Model No analysis method  A few observations Key Project Make a New Scenario of Thermal Plasma in MM-SNRs. This is not theory-oriented, but observation-oriented project： Spectrum Survey of bright MM-SNRs

  21. W 44 Spatial distribution of kTz and kTe

  22. AO7: Simulation for G337.2-0.7 (300 ksec) CIE RP

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