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(1) Soft X-rays : Thermal Plasma (SN1006) (2) Hard X-rays: Non-thermal

(1) Soft X-rays : Thermal Plasma (SN1006) (2) Hard X-rays: Non-thermal (SN 1006, RCW 86) (3) Mysterious 6.4 keV line (RCW 86, GC) Reports of the Suzaku Results Katsuji Koyama

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(1) Soft X-rays : Thermal Plasma (SN1006) (2) Hard X-rays: Non-thermal

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  1. (1) Soft X-rays : Thermal Plasma (SN1006) (2) Hard X-rays: Non-thermal (SN 1006, RCW 86) (3) Mysterious 6.4 keV line (RCW 86, GC) Reports of the Suzaku Results Katsuji Koyama Department of Physics, Kyoto University

  2. 騎官 (kikan) 騎陣将軍 (Kijin-Shogun) Lupusκ SN 1006: an interesting remnant for Suzaku SN1006 :Historical Galactic SNR, Type Ia SN 一條院 寛弘三年四月二日葵酉夜以降騎官中有大客星如螢惑光明動耀連夜正見南方或云 騎陣将軍星本体 増変光 In the reign-period of Ichijo-In, April 2nd, 3rd year of Kanko (= May 1st, 1006), a great guest star appeared within the constellation “Kikan” (=Imperial Guards). It was very bright like Mars, and visible in the southern sky every night.

  3. net~2×109 cm-3s (Vink et al. 2000, 2003) Extreme NEI: Low ISM density (n < 0.1 cm-3) (SN1006 : b = +14.6) The “youngest” Ia SNR in the Galaxy. The best SNR to study early phase of Type Ia Cosmic Ray acceleration The best SNR to study the cosmic ray origin The best mission is Suzaku: It has High Efficiency, Spectral Resolution, and low Noise Memorial Picture of the 1000 years birth day

  4. SE spectra OVII band Black : FI-CCD Red : BI-CCD Detection of a Clear Fe-K Line E ～ 6.42 keV(+- 0.01 keV) 　 → Fe XVII (Ne-like) Fe-K band Thermal Emission Suzaku ‥ 4-pointings Covers all the SN1006 (d～30’) region The spectrum from the SE quadrant is

  5. The 1.2-2.8 keV band: Mg, Si, S Lines １-component plasma is rejected Si: ΔE = 40 eV If Thermal Doppler Boarding kTSi = 13 MeV  15,000 km/s shock speed Mg Si S Black : FI Red : BI ～40eV Hα measurement vs = 2890 km/s 2- kTe, 1-net Plasma × 2- net, 1-kT Plasma　○ kTe = 1.2 (1.0-1.4) keV net1 = 1.3 (0.97-1.7)×1010 net2 = 7.4 (6.4-8.6)×108 metal abundance > solar → Mg, Si, S ：　ejecta origin χ2/d.o.f. = 393/332

  6. Broad Band Spectrum Fit with the Initial parameters of kT=1.2 keV net1 = 1.3×1010 net2 = 7.4×108 and, kT ~0.6 keV net= 6.7×109 Free Abundances. Then the results are; 1 kTe = 1.2 (1.1-1.3) keV, net = 1.3×1010 :over abundance 2 kTe = 1.5 (1.5-1.6) keV, net = 7.4×108 : over abundance 3 kTe=0.54 (0.52-0.58) keV, net= 6.7×109 :solar abundance 4 Power-law of Γ= 2.9 (2.8-3.0)

  7. Ejecta 1 Ejecta 2 S Si S Si Ca Ca Fe Mg Mg O O Ne Fe Ne (Nomoto el al. 1984) C C Large Si, S Large Ca, Fe Interpretationof the thermal spectra 1: Ejecta of reverse shock with Early heating 2: Ejecta of Reverse shock with late heating 3: ISM : Forward shock 4: Non-thermal components (same as the rim)

  8. SN1006 is the “youngest” SNR in our Galaxy! The plasma evolution in SNRs Tion Ion temp. Te Electron temp. Tz Ionization temp. ↑　↑　　　　↑　　　　　　　 　↑　　 nt SN1987A SN1006Cas A Cygnus Loop Kepler&Tycho

  9. He-Kα H-Kα He-Kβ BI He-Kγ, δ, ε… Red: Cygnus Loop(1-2 万年） Black: SN1006(千年） Cygnus Loop: no He-Kβ SN1006 : no H-Kα kTH = 10 ( net / 5× 109 [cm-3s] ) -1 (kTe / 0.54 [keV] ) 5/2 [keV](Laming et al. 2001) → kTH～ 20 kT　（ISM Density ～ 0.04 cm-3)

  10. The Oxygen Band 730eV = (3s→2p) 820eV = (3d→2p) But need very strong 730 eV K-shell transition series : Kδ, ε, ζ Extremely NEI Low kT ~0.6 keV Medium net 　　～6.7 109 O: solar 730eV 820eV

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