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ふみなすえがら
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1 2 nd Mar 2011 恒星進化星形成から探る銀河の形成進化の研究宇宙最初の星から太陽系形成まで

5 Fe Si NS/BH Massive Star (>10M ) e - -capture SNe (8-10M ) O C He H SN Ic SN Ib SN II Temp [10 8 K] Burning Stage H He C Ne O Si NSE Products He C,O Ne,Mg O,Mg Si Cr,Mn 56 Ni Core collapse driven by Fe photodisociation NS/BH formation Energy deposition

6 Abundances Post-shock Temperature T R -3/4 E 1/4 Shock propagation Presupernova structure 4 He 54 Fe56 Ni Si O fallback 4 He 20 Ne Mr[M ] 12 C 24 Mg 28 Si Temperature [10 9 K] Heavier elements higher-t & inner layers Complete Si burning Fe,α,Ni,Zn,Co,V Incomplete Si burning Fe,Si,Cr,Mn O burning Si

8 (e.g., Cayrel + 04; Honda + 04) 元素組成が不均一 r-process process [Fe/H]<-5 Hyper Metal-Poor (HMP) [Fe/H]<-4 Ultra Metal-Poor (UMP) [Fe/H]<-3 Extremely Metal-Poor (EMP) [Fe/H]<-2 Very Metal-poor (VMP) (Beers & Christlieb 05) HMP UMP EMP CEMP VMP A few SNe contributed to the EMP stars(e.g., Tumlinson 06)

9 H, He Fe, C, O, Mg, Si, Ca SN-induced Star Formation (e.g., Cioffi et al. 1988; Shigeyama & Tsujimoto 1998) The next-generation star is made from the mixture of the matter ejected by the SN (Fe, C, O, etc.) and swept-up by the shockwave (H, He). If ISM is metal-poor (Z<10-3 Z ), all metals in the next-generation stars are synthesized and ejected by the parent SN. [A/H]~log(M ej (A)/M sw (H))+con. [A/B]~log(M ej (A)/M ej (B))+con.

12 H, He 星形成超新星爆発重元素汚染 H, He, Z

13 M(Fe)/2 M(Fe)x2 Timmes+95

14 Normal SN model (25M, E 51 =1) 金属欠乏星 (Cayrel+04) SN model (NT+07b) 1 C O Ne Mg Si S Ar Ca Ti Cr Fe Ni Zn Hypernova model (25M, E 51 =10) [X/Fe] 0-1 B N F Na Al P Cl K Sc V Mn Co Cu Ga NT+07b Z

15 Mixing-fallback model Umeda & Nomoto 2002 M mix (out) f M cut (ini) H.Umeda

16 1 C O Ne Mg Si S Ar Ca Ti Cr Fe Ni Zn Hypernova model with mixing and fallback [X/Fe] 0-1 B N F Na Al P Cl K Sc V Mn Co Cu Ga NT+07b Z Kobayashi,,NT+06

17 すばる望遠鏡

18 Umeda & Nomoto 03,05; Iwamoto,,NT,+05

19 ~ Mixing region Si 層まで Ejection factor f~0.1 EMP ~ ONeMg 層まで f~10-3 CEMP ~ C+O 層まで f~10-5 HMP

20 Rayleigh-Taylor 不安定 + Fallback (e.g., SN1987A) ジェット状爆発 (e.g., GRB-HNe) NT+07b weak explosion E<10 51 erg に限る

21 Mixing mechanism Rayleigh-Taylor 不安定 + Fallback ジェット状爆発 Fe O Joggerst+10 NT+07a

22 Rayleigh-Taylor 不安定 + Fallback Low [(Co.Zn)/Fe] ジェット状爆発 Not-high [C/Fe,Mg] Joggerst+10 NT+07a

24 Metal-poor stars tend to have high [C/Fe] for low [Fe/H]. Hyper metal poor (HMP) 4 [C/Fe] 3 2 Ultra metal poor (UMP) C enhanced EMP (CEMP) 1. Faint SN 2. 2 種類の SNe (Fe 無 + normal SN) 3. AGB 伴星からの質量降着 4. 回転する大質量星からの質量放出 1 Extremely metalpoor 0 (EMP) [Fe/H]

25 C N O (Suda+04; Nishimura+09)

26 C-rich DLA ([Fe/H]~-3) HE ([Fe/H] = 2.21, Cohen + 04) BD ([Fe/H] = 3.73, Ito + 09)

27 C-rich DLA ([Fe/H]~-3, z=2.3) peculiar DLA ([Fe/H]~-1.5, z=1.6, Cooke+10) Kobayashi, NT + 11 ApJL in press (arxiv: )

29 HK survey: ~10,000 MP candidates Hamburg/ESO survey: ~10,000 MP candidates SDSS/SEGUE: ~100,000 candidates 2007: SEGUE (Sloan Digital Sky Survey) 2009: Skymapper (ANU) 2011: APOGEE (SDSS: R~20,000, 10 6 stars) 201?: HERMES (AAT: R~28,000, 10 6 stars) 201?: SuMIRe-PFS (IPMU/SUBARU: R~4,000, 10 6 stars)

30 Caveat O+Mg [Mg/Si]~1.4 Jet Fe Si He O+Mg Fe Si Abundance mixing due to the ISM interaction?? H NT09 Nakasato & Shigeyama 2000 R/10 14 [cm]

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