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 606-8502

“youngest”

Japanese historical record of SNROn 8 Nov. 1230, Teika Fujiwara wroteguest star events in his diary “Meigetsuki”

「客星古現例」the ancient samples of “guest stars”.

Guest stars = comets, novae, and supernovae

8 7 6 5 4 3 2 1

SN10063C58

Crab Nebula

SN1006Crab Nebula1054

3C581182

Teika Fujiwara, 1230, Meigetsuki Vol 52, page ?

1

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

騎官 (kikan)

如螢惑（ Mars ）

On May 1st 1006, a great guest star appeared in “Kikan” (the Oriental name of the constellations Lupus and Centaurus).It was very bright like Mars, and visible in the southern sky in every night.

1006/05/01, Midnight Southern Sky of Kyoto

Mars

Antares

SN 1006

如螢惑 (similar to Mars)

Old records 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 ） ：　 2.5 to 3 times as large as Venus.

The intensity of its light was a littlemore 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

-8 Mag

-10 Mag

Ref ： Full Moon = -12.6 Mg 、 Venus= -4.6 Mag

SN1006 : 　 Historical Galactic SNR Type Ia SN

Distance = 2.2 kpcMaximum Mag = -20 Mag

Days after 1006/05/01

Mag

nit

ud

e-12

-10

-8

-6

-4

-2

0

2

4

2006 was one millennium after SN1006memory X-ray picture of SN1006 by Suzaku

Suzaku The 5th Japanese X-ray astronomical Satellite, lauched on July 10th 2005

Suzaku: “red angel bird” of the Oriental Mythology, living in the Southern Sky of the Palace

Suzaku

Wall painting in the old tomb“Kitora 　 Kofun”

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

High Temperature Plasmas in SN1006 　

Black : FI-CCDRed : BI-CCD

Discovery of Ar, Ca and Fe Lines

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,

This spectrum is very unusual, hence can notbe applied by the conventional plasma code.What is unusual, what is the difference between this plasma and those in the other SNRs ?

He-Kβat 670 eV

575eV672eV

820eV

730eV 920eV

He-like Kα: 570eVH-like Ｌｙ α :650eV

H-like oxygen

He-likeoxygen

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 is true for any SNRs other than SN1006 .

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] ), butHe-like is in low ionization states (kTi ~ 0.15 [keV])

↑ 　　　　　↑　　　　　　　 　↑　　 nt　SN1987A 　 Cas A CygnusLoop Kepler&Tycho

The plasma evolution in SNRs

Tpn

Te

Ti

Tp:proton temp.

Te: Electron temp

Ti: Ionization temp.

Shock by Velocity (V) kTp=mpV2, kTe=meV2

Tp ～ 1000*Te (mp/me =1000)kTp kTe , kTe kTi

Energy Transfer ∝ 　 nt

Thermal ages ∝ nt

SN1006 is the “youngest” SNR in our Galaxy!

SN1006

Taking these non-equilibrium effects into account, we modified the conventional plasma codes, and fit the spectrum . It was very complicated job, hence

1) kTe=0.54 (0.52-0.58) keV, net= 6.7×109 :solar abundance

2) kTe = 1.2 (1.1-1.3) keV, net = 1.3×1010 :over abundance

3) kTe = 1.5 (1.5-1.6) keV, net = 7.4×108 : over abundance

Ejecta1: Reverse shock of Early heating (Outer Shell)Ejecta2: Reverse shock of Recent heating (Inner Shell)

Ejecta 2

CO

Mg

Si S

C

Fe

Large Ca, Fe (Nomoto el al. 1984)

Ejecta 1

Large Si, S

2) kTe = 1.2 (1.1-1.3) keV, net = 1.3×1010 = Ejecta1

3) kTe = 1.5 (1.5-1.6) keV, net = 7.4×108 = Ejecta2

Conclusion

(1) 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.

Cas A Kepler Tycho

0.02pc0.04pc

0.007pc

0.02pc

0.06pc

0.01pc

Many SNRs have thin filaments!

Non-Thermal Shell

SN1006