(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 NoiseMemorial Picture of the 1000 years birth day

net~2×109 cm-3s (Vink et al. 2000, 2003) Extreme NEI: Low ISM density (n < 0.1 cm-3) (SN1006 : b = +14.6)

Thermal EmissionSuzaku 4-pointings ‥Covers all the SN1006 (d～ 30’) regionThe spectrum from the SE quadrant is

OVII band

SE spectra

Black : FI-CCDRed : BI-CCD

Detection of a Clear Fe-K Line E ～ 6.42 keV 　 (+- 0.01 keV)　 → Fe XVII (Ne-like) Fe-K band

The 1.2-2.8 keV band: Mg, Si, S Lines

１ -component plasma is rejectedSi: ΔE = 40 eVIf Thermal Doppler Boarding kTSi = 13 MeV 15,000 km/s shock speed

Black : FIRed : BI

Mg Si

S

～ 40eV

Hα measurementvs = 2890 km/s

2- kTe, 1-net Plasma ×2- net, 1-kT Plasma 　○

kTe = 1.2 (1.0-1.4) keVnet1 = 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

Broad Band Spectrum

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)

Fit with the Initial parameters ofkT=1.2 keVnet1 = 1.3×1010

net2 = 7.4×108

and, kT ~0.6 keV net= 6.7×109

Free Abundances.

Then the results are;

Interpretation　 of the thermal spectra

1: Ejecta of reverse shock with Early heating2: Ejecta of Reverse shock with late heating3: ISM : Forward shock 4: Non-thermal components (same as the rim)

Ejecta 1 Ejecta 2

CO

Ne

Mg

Si SCa

Fe CO

Ne

Mg

Si SCa Fe

Large Si, S Large Ca, Fe

(Nomoto el al. 1984)

SN1006 is the “youngest” SNR in our Galaxy!

↑ 　↑　　　　↑　　　　　　　 　↑　　 nt 　　　 SN1987A SN1006 　 Cas A Cygnus Loop 　　　 Kepler&Tycho

Tion

Te

Tz

The plasma evolution in SNRs

Ion temp.

Electron temp.

Ionization temp.

Cygnus Loop: no He-Kβ SN1006 : no H-KαkTH = 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)

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

820eV730eV

730eV = (3s→2p)820eV = (3d→2p)But need verystrong 730 eV

K-shell transition series: Kδ, ε, ζ

Extremely NEILow kT ~0.6 keVMedium net　　～ 6.7 109

O: solar