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

2. KES 792011/4/23 G272.2-3.25/28+11/12 G290.1-0.86/25 G292.0+1.87/22 G349.7+0.29/29 G350.1-0.39/17 Kes 27 2012/2/20 ? G2772012 (AO7) W 28 W 44 Long Observation (Pre-KP) 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). Key Project (AO6)

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

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

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

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

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

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

9. Ｒａｒｅｆ ａｃｔｉｏ ｎ Ｐｈｏｔｏ Ｉｏｎｉｚ ａｔｉｏｎ /n (yr)

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

11. Best-fit Model kTz=1.1 kTe=0.48 Log(nt)=11.85 Chi2/d.o.f 1-CIE 2121/353 1-RP 1175/352 Tz+Te+nt 536/349 W 44 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 kTz kTe nt

13. Results of Key Project SNRs: QL by Katsuda

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

15. G349G350 Temperature kTz1.2 keV1.0 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) Fe Ionization state is nearly He-like, in sharp contrast to typical SNRs such as Tycho, Kepler, SN1006 and RCW 86 (Neutral --Ne-like)

16. 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 6.4 6.7 keV 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. 3C397 G344 Tycho Very strong Cr, M, Ni (Yamaguchi et al. submitted to ApJ Fe 12.5 +/- 1.3 Ni 90.8 +/- 15.8 Line E c Flux 5.61 9.72E-06 6.104.46E-06

20. 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 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 Thin thermal spectra = 2 Type of SNRs

21. W 44 Spatial distribution of kTz and kTe

22. AO7: Simulation for G337.2-0.7 (300 ksec) Te (keV)0.635 (0.626 -- 0.645) Tz (keV)0.635 (0.626 -- 0.645) Tz/Te --- Z_Si (solar)1.23 (1.17 -- 1.29) Z_S (solar)1.39 (1.32 -- 1.47) Z_Ar (solar)1.11 (0.843 -- 1.38) chi2/dof572.43/418 = 1.40 Te (keV)0.495 (0.477 -- 0.514) Tz (keV)0.713 (0.675 -- 0.750) Tz/Te1.44 (1.38 -- 1.49) Z_Si (solar)1.82 (1.71 -- 1.93) Z_S (solar)2.25 (2.05 -- 2.45) Z_Ar (solar)2.19 (1.64 -- 2.79) chi2/dof447.50/417 = 1.07 CIE RP