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Expanding velocity Random velocity (shock) : temperature of Ion ( T i) is higher than electron (Te ). Ion temperature, T i. Ionization temeprature: T z. Study of SNR Canonical Scenario of Dynamical Evolution This determines the shell-like morphology and thermal
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Expanding velocity • Random velocity (shock) • : temperature of Ion(Ti) is • higher than electron (Te) Ion temperature, Ti Ionization temeprature: Tz 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 (Te > Tz) CIE (Te=Tz)
Thin thermal spectra = 2 Type of SNRs 1. Shell-like SNR Canonical evolution of dynamics: Canonical model & analysis:NEI, PSHOCK Many proposals, 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
○ Are Spectra of MM-SNR SuzakuLegacy? • Yes, because • A few Observation sUnexpected 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
RRC has large Impacts on the Abundances • In RP, Radiative Recombination • Continuum (RRC) is Dominant. • kTe: low -> emissivity • of collisional excitation : small. • bremss : small • Abundancess: large • On the other hand, • Line flux is increased by • cascade after recombination • Abundances : small G359.1-0.5 1-CIE kT e Ab(Si) Ab(S) 0.772.3 2.5 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
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.
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
Science of Recombining Plasma Ionizing Plasma (IP) traces standard evolution of shock dynamics Canonical model : Shell-like, 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 to search for the some events.
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
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) Max Energy (∝v2) Low density (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
Big solar flare : RPis associated with Hard X-ray Hard X Memory Tz event Te Tz CIE Time (~1000 sec) (Kato and Masai) Te Normalized by nt , A few thousand years for SNRs
GeV・TeV/RP : What is a key? May be Supra Thermal (=CRInjector) +2keV 0.5keV off-diagonal model Astro-H Only a few % can make RRC, RP Flux ~1 keV CIE Recombination Supra Thermal (2 keV) : Highly Ionize Ionization of Si : CR Injector GeV/TeV Strong Injector for MM-SNR X-ray Energy
What will the RP Science tell us ? Possible answers are; Cosmic Ray Injector Supra Thermal RP GeV, TeV astronomy T e are separately determined by RRC and Bremss Abundances Search for hidden hard components Information of Line and RRC is essential forthe Plasma Diagnosis Path Finder for Astro-H
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
Target List (priority order) from the ASCA results ----------------------------------------------------------------------------------------------- Name kTe He-α(Si)* Size(arcmin) Obs(ksec) & ------------------------------------------------------------------------------------------------ G349.7+0.2+\1.1 0.13 3 160 Kes 79+0.7 0.5 10 50 G292.0+1.8 0.5 0.512×8 40 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 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.
e.g. Simulation for Kes 79 (50 ksec: Upper Left) & G337.2-0.7 (200 ksec: Lower Left and Right.) CIE: Kes 79 CIE RP CIE: G337.2
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
Fe Kα< 6.7 keV Ionizing Plasma kTe=3 keV kTz=1 keV Cas A Recombining Plasma kTe=1keV kTz=3 keV W49B
(1) Initial condition kTz >>kTe Canonical SNRPhoto-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 .
---------------------------------------------------------------------------------------------------------------------------------------------------------------------------- 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
-------------------------------------------------------------------------------------------------------------------------------------------------------------------------- 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