New Scenario of Plasma Evolution in SNRsNEI describes the plasma evolution in

standard SNRs (shell-like ): Ionizing Plasma (IP)

CIEColisional Ionization Equilibrium

Std (Shell) SNRsShock HeatedPlasma 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 79 2011/4/23 G272.2-3.2 5/28+11/12G290.1-0.8 6/25G292.0+1.8 7/22G349.7+0.2 9/29 G350.1-0.3 9/17

Kes 27 2012/2/20 ? G277 2012 (AO7)

W 28W 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)

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Model χ2/d.o.f

1-CIE 2160/641

2-CIE 1753/639

Multi-kTz 893/6341-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

■ Ne

■ Mg

Si ■■ S

■ Fe

The best-fit temperatures (kTz) for kTe=0.40 keV

kTe

kTz

0.8

0.2

1.2

0.3

(keV

)(k

eV)

TeV γ-rays

Shocked MC

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Spatial distribution of kTe and kTz

kTe and kTz distributions vs distances from candidate sources No correlation

Ionization by High energy particle XThermal conduction to Molecular cloud X

kTz kTe

Photo Ionization: highly ionization by X-rays (γ-ray after glow)

Photo Ionization γ-ray 　 burst Time

Te

Tz

(Kawasaki, 02, 05)

Dense CSM

Time

Te

Tz

(Itoh & Masai 89)Thin ISM

Rarefaction:electron cooling by adiabatic expansion

■ Ne

■ Mg

Si ■■ S

■ Fe

The best-fit temperatures (kTz)

Ｒａｒｅｆａｃｔｉｏｎ

Ｐｈｏｔｏ　Ｉｏｎｉｚａｔｉｏｎ

/n (yr)

/n (yr)

CIE

Std (Shell) SNRs

Heating IP: Standard Evolution

Non-Std SNRs

Missing Branch of Evolution

Missing Event

Missing Event: RarefactionMissing Branch: Recombining (RP)

Best-fit Model

kTz=1.1kTe=0.48Log(nt)=11.85

Chi2/d.o.f

1-CIE 2121/353

1-RP 1175/352

Tz+Te+nt 536/349

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Energy (keV) Uchida et al. 2012, to be submitted

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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

G349 G350Temperature kTz 1.2 keV 1.0 keVAbundance 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)

W49B : Extreme RP Te= 1.3 Tz=2.5

G349 1.2 1.2

G350 1.0 1.0

1.0 0.3Tycho: Extreme IP

6.4 　 6.7 keV

All the SNRs, more or less, had an event of RP production

AO7 target: G 337.2-0.7 ASCA Spectrum

Fe-K

The End

3C397

G344

Tycho

Very strongCr, 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 6.10 4.46E-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

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Spatial distribution of kTz and kTe

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/dof 572.43/418 = 1.40

Te (keV) 0.495 (0.477 -- 0.514)

Tz (keV) 0.713 (0.675 -- 0.750)

Tz/Te 1.44 (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/dof 447.50/417 = 1.07

CIE RP