(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

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. 騎陣将軍 (Kijin-Shogun) Lupusκ 騎官 (kikan) SN 1006: an interesting remnant for Suzaku SN1006 : Historical Galactic SNR, Type Ia SN

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 n e t~2×10 9 cm -3 s (Vink et al. 2000, 2003) Extreme NEI: Low ISM density (n < 0.1 cm -3 ) (SN1006 : b = +14.6)

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

The keV band: Mg, Si, S Lines １ -component plasma is rejected Si: ΔE = 40 eV If Thermal Doppler Boarding kT Si = 13 MeV  15,000 km/s shock speed Black : FI Red : BI Mg Si S ～ 40eV Hα measurement v s = 2890 km/s 2- kTe, 1-net Plasma × 2- n e t, 1-kT Plasma ○ kTe = 1.2 ( ) keV n e t 1 = 1.3 ( )×10 10 n e t 2 = 7.4 ( )×10 8 metal abundance > solar → Mg, Si, S ： ejecta origin χ 2 /d.o.f. = 393/332

Broad Band Spectrum 1 kT e = 1.2 ( ) keV, n e t = 1.3×10 10 :over abundance 2 kT e = 1.5 ( ) keV, n e t = 7.4×10 8 : over abundance 3 kT e =0.54 ( ) keV, n e t= 6.7×10 9 :solar abundance 4 Power-law of Γ= 2.9 ( ) Fit with the Initial parameters of kT=1.2 keV n e t 1 = 1.3×10 10 n e t 2 = 7.4×10 8 and, kT ~0.6 keV n e t= 6.7×10 9 Free Abundances. Then the results are;

Interpretation of 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) Ejecta 1Ejecta 2 C O Ne Mg SiS Ca Fe C O Ne Mg Si S Ca Fe Large Si, SLarge Ca, Fe (Nomoto el al. 1984)

SN1006 is the “youngest” SNR in our Galaxy! ↑ ↑ ↑ ↑ nt SN1987A SN1006 Cas A Cygnus Loop Kepler&Tycho T io n TeTe TzTz The plasma evolution in SNRs Ion temp. Electron temp. Ionization temp.

Cygnus Loop: no He-Kβ SN1006 : no H-Kα kT H = 10 ( n e t / 5× 10 9 [cm -3 s] ) -1 (kT e / 0.54 [keV] ) 5/2 [keV] (Laming et al. 2001) → kT H ～ 20 kT （ ISM Density ～ 0.04 cm -3 ) He-Kα H-Kα He-Kβ He-Kγ, δ, ε… BI Red: Cygnus Loop (1-2 万 年） Black: SN1006 ( 千 年）

The Oxygen Band 820eV 730eV 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 n e t ～ O: solar