new scenario of plasma evolution in snrs nei describes the plasma evolution in standard snrs...
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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