1. Type Ia Supernova Remnant “youngest”
Suzaku Results of SN 1006: Chemical abundances of the 　youngest 　Galactic
Type Ia Supernova Remnant
Katsuji Koyama
Department of physics, Kyoto University, Kitashirakawa,
Sakyo-ku, Kyoto
“youngest”

2. SN1006 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
如螢惑（Mars）
騎官 (kikan)
On May 1st 1006, a
great guest star
appeared in “Kikan” (the Oriental name of the constellation Lupus and Centaurus.).
It was very bright like
Mars, and visible in the southern sky in every night.
SN1006のみが「大客星」という表現が用いられています。
いかに大きく、明るかったかがわかります。

3. 1006/05/01, Midnight Southern Sky of Kyoto
Mars
Antares
SN 1006
如螢惑
(similar to Mars)

4. Old record from Asia and Arabia
明月記（Kyoto）：寛弘三年四月二日(= 5/1)如螢惑（like Mars）
Ibn al-Jawzi （Baghdad） ：　 A large star similar to Venus
appeared to the left of qibla.
at the beginning of the month of
Sha’ban (= 5/3).
Ali ibn Ridwan（Egypt） ：　 to 3 times as large as Venus.
The intensity of its light was a little
more than a quarter of that moonlight.
(5/5?)
宋史天文志（China） ：景徳三年四月戊寅(=5/6)如半月( half moon)
-2　Mag
-4 Mag
戊寅　ぼいん　つちのえとら
-8 Mag
-10 Mag
Ref： Full Moon = Mg、 Venus= -4.6 Mag

5. SN1006 : Historical Galactic SNR Type Ia SN
Days after 1006/05/01
Magnitude
-12
-10 -8 -6 -4 -2 2 4
2006 was one millennium after SN1006
memory X-ray picture of SN1006 by Suzaku
Distance = 2.2 kpc
Maximum Mag = -20 Mag

6. Suzaku The 5th Japanese X-ray astronomical
Satellite, lauched on July 10th 2005
Suzaku
Suzaku
Wall painting in the old tomb“Kitora　Kofun”
Suzaku: “red angel bird” of the Oriental Mythology, living in the Southern Sky of the Palace
XIS (X-ray Imaging
Spectrometer: CCD)
XRT
XIS
XRT (X-Ray
Telescope)
In 2006, Suzaku saw
a southern sky, and took a millennium-memorial X-ray picture of SN1006

7. High Temperature Plasmas in SN1006
Discovery of Ar, Ca and Fe Lines
Black : FI-CCD
Red : BI-CCD
This spectrum is very unusual, hence can not
be applied by the conventional plasma code.
What is unusual, what is the difference between
this plasma and those in the other SNRs ?
In normal cases, we can determine the chemical
compositions using the conventional plasma code.
The plasma code has been made based on the laboratory
plasma physics. However,

8. We found Kγ、Kδ lines at 730 eV and 820 eV
He-like
oxygen
730eV
920eV
575eV
H-like
oxygen
672eV
820eV
He-like Kα: 570eV
H-like Ｌｙα :650eV
He-Kβat 670 eV
We found Kγ、Kδ　lines at 730 eV and 820 eV
This is very surprising (no plasma code !)
High electron temperature (kTe ~ 1.5 [keV] ), but
Low ionization states (kTi ~ 0.15 [keV])
If we see this spectrum in the other SNRs, most of the X-ray
Astronomers believe that these two-lines are He-like and
H-like Ka. This, in fact, is true for any other SNRs.

9. SN1006 is the “youngest” SNR in our Galaxy! Shock by Velocity (V)
kTp=mpV2, kTe=meV2
Tp～1000*Te (mp/me =1000)
kTp  kTe , kTe kTi
Energy Transfer ∝　nt
The plasma evolution in SNRs
Tp:proton temp.
Tpn
Te: Electron temp Te
Ti: Ionization temp.
SN1006 is the “youngest”
SNR in our Galaxy! Ti
↑　　　　　↑　　　　　　　 　↑　　 nt　
SN1987A 　 Cas A CygnusLoop
Kepler&Tycho
SN1006
Thermal
ages ∝ nt

10. 1) kTe=0.54 (0.52-0.58) keV, net= 6.7×109 :solar abundance
2) kTe = 1.2 ( ) keV, net = 1.3×1010 :over abundance
3) kTe = 1.5 ( ) keV, net = 7.4×108 : over abundance

11. 2) kTe = 1.2 (1.1-1.3) keV, net = 1.3×1010 = Ejecta1
Ejecta1: Reverse shock of Early heating (Outer Shell)
Ejecta2: Reverse shock of Recent heating (Inner Shell)
Ejecta 2
Ejecta 1 Si S Fe Mg O C C
Large Si, S
(Nomoto el al. 1984)
Large Ca, Fe

12. Conclusion We discovered Ar, Ca and Fe Lines for the first time
(2) We found extremely non-equilibrium between
electron temperature and ionization temperature.
(3) The ejecta consists of two plasma components:
One has almost identical abundance profile to
that of the theoretical prediction of type Ia SNR,
and the other has lower abundance in Fe.
The former would be due to an inner part of the
SNR and the latter is due to an outer part.