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shock  heating of Ions and electrons as:

Ion temperature, T i. Ionization temeprature: T z. shock  heating of Ions and electrons as:. Study of ＳＮＲ Canonical Scenario of Dynamical Evolution This determines the shell-like morphology and thermal spectrum. mv 2 = 3 kT. Enegy transfer.

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shock  heating of Ions and electrons as:

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  1. Ion temperature, Ti Ionization temeprature: Tz shock heating of Ions and electrons as: Study of ＳＮＲ Canonical Scenario of Dynamical Evolution This determines the shell-like morphology and thermal spectrum mv2 = 3kT Enegy transfer Electron temperature: Te NEI  CIE

  2. 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

  3. ○ Are Spectra of MM-SNR SuzakuLegacy? • Yes, because • A few Observation Unexpected facts may be found • （Observation-Oriented study = DNA of Ｘ-ray Astronomy) • Suzaku has Low background, High energy resolution • and Large effective area. Radiative Recombination Continuum (RRC: 1-st time for Collisional Ionized Plasma) Over-ionized Plasma （Recombining Plasma: RP): vs　（Ionizing Plasma ：IP=NEI) RP may provide a New Science of Suzaku Paradigm is SSS (Einstein) ○ What progress would be in RP ? Hint: RP-detected MM-SNRs ( IC443, W44, W28, W49B, G359.1-0.5)are allTeV/GeV Sources

  4. RRC has large Impacts on the Abundances • In RP, Radiative Recombination • Continuum (RRC) is Dominant. • kTebecomes low-> emissivity • of collisional excitation small. •  bremss becomes small • Abundances become large • On the other hand, • Line flux becomes large by • cascade after recombination •  Abundances become small G359.1-0.5 1-CIE kT Ab(Si) Ab(S) 0.772.3 2.5 2-CIE (abundances-link) 0.55 11 23 5 RP Model 0.2912170.77 (kTz) CIE model RP model RRC Bremss • Relaiable abundances  Proper model of the Plasma • Line and RRC based diagnosis is essential (not bremss) • Revise the abundances using Suzaku • (in particular, those in MM-SNR) •  Path Finderof Astro-H Spectrum of W28-Center (Sawada et al.) kTe=kTz= 0.90 keV kTe=0.47, kTz=0.96

  5. ＡＳＣＡ：　 Shell-like MM SNR RP Region Suzaku A few ＭＭ-ＳＮＲ, Compared to Shell -like SNRs Added a few MM-SNR with AO5 Ｇ３５９．１ Then, what does Suzaku change from ASCA ? kTe, Abundances IP (NEI) Kawasaki et al.

  6. IC443 Brems+lines List of RP SNRs and our Progress of the RP Analysis W44 W28 W49B ICIE+Ly+RRC Upper: 1CIE Lower: Full RP G359.1-0.5 1CIE+Ly+RRCs

  7. Science of Recombining Plasma Ionizing Plasma (IP) traces standard evolution of shock dynamics Canonical model : Shell-llike, NEI, PSHOCK Recombining Plasma (RP) remembers some events in the early phase of MM-SNR. Our mission is to search for these some events. We provide observational evidence for the events.

  8. Ｗ４９Ｂ RP is not Local but Ｇｌｏbａｌ Tz/Te map all > 1 ○　Initial photo ionization such as ＧＲB ? f> 1050 erg (Same order of UV photons in HII region) ○　Rarefaction in initial phase ○　Related to the particle accelaration (CR)？ IC443

  9. ＩSM n ~小 Initial rarefaction High density CSM: Te=Tz break out to low density ＩＳＭ adiabatic cooling Te decrease ○ Sudden increase shock velocity ( >normal case) High Energy (∝v2） Low density of ISM suppress the Coulomb interaction with thermal particles more efficient acceleration CSM n ~大 Diffusive Shock Acceleration model does not reach to the Knee Energy （The problem of Cosmic Ray Acceleration ) The rarefaction Ｓｃｉｎａｒｉｏ may solve this problem ？ 1 0 log r(pc) log t (year) Itoh & Masai 1 2 3

  10. Big solar flare RPassociated with Hard X-ray Ｈａｒｄ　Ｘ Memory Ｔｚ event Ｔｅ kTz CIE Time　（～1000 sec） (Kato and Masai) kTe Normalized by nt , A few thousand years for SNRs

  11. GeV・TeV/RP : What is a key? May be Supra Thermal (＝CRInjector) +2keV 0.5keV 2-component Ｃross-Coupling Only a few % of Thermal can make RRC, RＰ Flux ~1 keV CIE Recombination Supra Thermal (2 keV) ：　Highly Ionize : CR Injector GeV/TeV Strong Injector for MM-SNR Effective acceleration for Shell-like ？ Ionization of Ｓｉ X-ray Energy

  12. What will the RP Science tell us ? Possible answers are; Cosmic Ray Injector Supra Thermal RP  GeV, ＴｅＶ　astronomy RRC: kT e and Bremss are separately determined  Abundances  Search for hidden hａｒｄ　components Information of Line and RRC is essential forthe Plasma Diagnosis  Path Finder for Astro-H

  13. Very strong Cr-line (and Ni) ! Unexpectd discovery may not be only RP | | Unbiased MM-SNR study will make the Suzaku legacy Obserbation-oriented science which is the DNA of X-ray astronomy (Nature may be much more imaginative than we are) 3C397 G344 Tycho G344 There must be unknown Gold Mines . Lets search for Gold Mines ! StrongAl ! (Yamaguchi et al., submitted to ApJ

  14. Target selection from ASCA ----------------------------------------------------------------------------------------------- Name kTe He-α(Si)* Size(arcmin) Obs(ksec) & ------------------------------------------------------------------------------------------------ G292.0+1.8 0.5 0.512×8 40 Kes 79+0.7 0.5 10 50 G350.1-0.3 1.46 0.3 4 70 G290.1-0.8 0.63 0.2 19×14 110 Kes27 0.55 0.2 21 120 G272.2-3.2 0.73 0.15 15 150 G349.7+0.2+\1.1 0.13 3 160 G337.2-0.7 0.85 0.08 6 200 $$ --------------------------------------------------------------------------------------------- * peak values of Si Heα (unit is arbitrary) from ASCA, For comparison, the Heα flux in W49B is ~1. + maser source\ GeV source $$Truncated to 2/3 & Observation time is estimated by the simulationassuming that RP spectrum is Tz/Te = 1.4 (typical) and that CIE model is rejected with ~3σ level.

  15. e.g. Simulation for G337.2-0.7 (200ksec ob.) CIE RP

  16. The End

  17. Path Finder for Astro-H= Physics of high Temperature Space Plasma （PurePlasma） Diagnosis with degenerated Kα Line Energy  Diagnosis with resolved lines （New Science） Excitation (w) vs Cascade, Recombination line (z) : RP 1.2 kTz 0.3 z/w e.g. ：z/wis not only for density diagnosis Plasma is more fantastic • e.g. • Suzaku can plot data on the kTe-kTz plane. • The center energy of He-like Kαshould be give by fine structure • 2. If it deviates , then the plasma has bulk motion, ornon/Supra-thermal components or Else ？ • These are the subjects of Astro-H • Suzaku is the path-finder 0.3 kTe 1.2 kTz kTe

  18. Fe Kα< 6.7 keV Ｉｏｎｉｚｉｎｇ　Ｐｌａｓｍａ　 ｋTe=3 keV kTz=1 keV Cas A Recombining Plasma ｋTe=1keV kTz=3 keV W49B

  19. (1) Initial condition kTz >>kTe  Canonical SNRPhoto-ionization by GRB and Afterglow: W49B (2) Canonical SNR, kTe is cooled down by thermal conduction to clouds. (3) Explosion in a dense CSM (high kT CIE plasma) break-out to the ISM  kTe cooling by adiabatic expansion. (4) Ionization by supra /non-thermal electrons (big solar flares: a RP phenomena and a hard X-ray tail ). Hard X-ray is hidden behind the continuum . All the RP-detected SNRs (5 MM-SNRs) are TeV/GeV sources .

  20. ---------------------------------------------------------------------------------------------------------------------------------------------------------------------------- Name kTe He-α(Si) * (Fe)* -------------------------------------------------------------------------------------- Kes 79 0.7 0.5 G272.2-3.2 0.73 0.15 G290.1-0.8 0.63 0.2 G292.0+1.8 0.5+1.5 0.5 G309.2-0.6 1.96 0.07 Kes27 0.4-0.7 0.2 G337.2-0.7 0.85 0.06 G349.7+0.2 1.1 0.13 0.003 G350.1-0.3 1.46 0.3 0.0015 G352.7-0.1 1.6 0.05 0.001 -------------------------------------------------------------------------------------- Caption: * peak values of Heα (Si) and Fe (unit is arbitrary), For comparison, W49B are 0.55 (Heα, Si) and 0.15 (Fe). With XIS, these values become 2 time(for Si) and 10 times (for Fe) larger. ------------------------------------------------------------------------------------ Thse are the ASCA picture Suzaku make revolution on the ASCA picture And move on Astro-H Which is Line+ RRC based Plasma Diagnosis

  21. -------------------------------------------------------------------------------------------------------------------------------------------------------------------------- Name kTe1kTz kTe2 TeV GeV --------------------------------------------------------------------------------------- -----RP detected------ W28 0.47 0.96 Y Y W44 0.55 0.71 Y Y W49B 1.5 2.7 Y Y IC443 0.6 1-1.2 Y Y G359.1-0.5 0.29 0.77 Y ----possibly detected------ G346.6-0.2 0.7 1.0 ----Non-detection of RP ------ G344.7-0.1 0.95 5.0 G348.5+0.1 0.4 0.9 Y Y G355.6-0.0 0.6 3C397 ? 3C391 ? ---------------------------------------------------------------------------------------- Captions: “Y” marks in the row of TeV, GeV, OH and MC Back: Proper Project Blue: Sub Product Red :AO5 IP

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