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

KES /4/23 G /28+11/12 G /25 G /22 G /29 G /17 Kes /2/20 ? G (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)

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:

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

kT e kT z (keV) TeV γ-rays Shocked MC W 28 Spatial distribution of kTe and kTz

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

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

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

Ｒａｒｅｆ ａｃｔｉｏ ｎ Ｐｈｏｔｏ Ｉｏｎｉｚ ａｔｉｏｎ /n (yr)

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

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

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

Results of Key Project SNRs: QL by Katsuda

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

G349G350 Temperature kTz1.2 keV1.0 keV Abundance Fe 1.0 ( ) 2.1 ( ) Ni 3.5 ( ) 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)

W49B : Extreme RP Te= 1.3 Tz=2.5 G G Tycho: Extreme IP keV All the SNRs, more or less, had an event of RP production

AO7 target: G ASCA Spectrum Fe-K

The End

3C397 G344 Tycho Very strong Cr, M, Ni (Yamaguchi et al. submitted to ApJ Fe /- 1.3 Ni / Line E c Flux E E-06

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

W 44 Spatial distribution of kTz and kTe

AO7: Simulation for G (300 ksec) Te (keV)0.635 ( ) Tz (keV)0.635 ( ) Tz/Te --- Z_Si (solar)1.23 ( ) Z_S (solar)1.39 ( ) Z_Ar (solar)1.11 ( ) chi2/dof572.43/418 = 1.40 Te (keV)0.495 ( ) Tz (keV)0.713 ( ) Tz/Te1.44 ( ) Z_Si (solar)1.82 ( ) Z_S (solar)2.25 ( ) Z_Ar (solar)2.19 ( ) chi2/dof447.50/417 = 1.07 CIE RP