1. 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”

2. Japanese historical record of SNR On 8 Nov. 1230, Teika Fujiwara wrote guest 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 SN1006 3C58 Crab Nebula

3. SN1006 Crab Nebula 1054 3C58 1182 Teika Fujiwara, 1230, Meigetsuki Vol 52, page ? 1

4. 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.

5. 1006/05/01, Midnight Southern Sky of Kyoto Mars Antares SN 1006 如螢惑 (similar to Mars)

6. 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 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 -8 Mag -10 Mag Ref ： Full Moon = -12.6 Mg 、 Venus= -4.6 Mag

7. SN1006 : Historical Galactic SNR Type Ia SN Distance = 2.2 kpc Maximum Mag = -20 Mag Days after 1006/05/01 Magnitude -12 -10 -8 -6 -4 -2 0 2 4 2006 was one millennium after SN1006 memory X-ray picture of SN1006 by Suzaku

8. 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

9. High Temperature Plasmas in SN1006 Black : FI-CCD Red : 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 not be applied by the conventional plasma code. What is unusual, what is the difference between this plasma and those in the other SNRs ?

10. He-Kβat 670 eV 575eV 672eV 820eV 730eV 920eV He-like Kα: 570eV H-like Ｌｙ α :650eV H-like oxygen He-like oxygen 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 (kT e ~ 1.5 [keV] ), but He-like is in low ionization states (kT i ~ 0.15 [keV])

11. ↑ ↑ ↑ nt SN1987A Cas A CygnusLoop Kepler&Tycho The plasma evolution in SNRs TpnTpn TeTe TiTi T p :proton temp. T e : Electron temp T i : Ionization temp. Shock by Velocity (V) kT p =m p V 2, kT e =m e V 2 T p ～ 1000*T e (m p /m e =1000) kT p  kT e, kT e  kT i Energy Transfer ∝ nt Thermal ages ∝ nt SN1006 is the “youngest” SNR in our Galaxy! SN1006

12. 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, n e t= 6.7×10 9 :solar abundance 2) kT e = 1.2 (1.1-1.3) keV, n e t = 1.3×10 10 :over abundance 3) kT e = 1.5 (1.5-1.6) keV, n e t = 7.4×10 8 : over abundance

13. Ejecta1: Reverse shock of Early heating (Outer Shell) Ejecta2: Reverse shock of Recent heating (Inner Shell) Ejecta 2 C O Mg SiS C Fe Large Ca, Fe (Nomoto el al. 1984) Ejecta 1 Large Si, S 2) kT e = 1.2 (1.1-1.3) keV, n e t = 1.3×10 10 = Ejecta1 3) kT e = 1.5 (1.5-1.6) keV, n e t = 7.4×10 8 = Ejecta2

14. 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.

15. Cas AKeplerTycho 0.02pc 0.04pc 0.007pc 0.02pc 0.06pc 0.01pc Many SNRs have thin filaments! Non-Thermal Shell SN1 00 6