1 / 21

Expanding velocity Random velocity (shock) : temperature of Ion ( T i) is

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

rupert
Download Presentation

Expanding velocity Random velocity (shock) : temperature of Ion ( T i) is

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. 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)

  2. 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

  3. ○ Are Spectra of MM-SNR SuzakuLegacy? • Yes, because • A few Observation s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. • 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

  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-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.

  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) 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

  10. 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

  11. 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

  12. 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

  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 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.

  15. 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

  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

More Related