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2 Galactic Archaeology [Fe/H] and [X/Fe] evolve in a galaxy: fossils to tell the evolution history of the galaxy Galactic Archaeology"
3 GRB Hypernovae SN Light Curve & Spectra" bright, broad, blended line" E>10 52 erg,m(fe)>0.1m HN efficiency=0.5 for M>20 SN1998bw Nomoto et al. 2002!
4 Type Ia Supernovae Single Degenerate Scenario: WD+star" SNIa Lifetime ~ lifetime of companion star" Companion mass ranges from binary calculation (Hachisu, Kato, Nomoto)" WD+RG WD+MS CK & Nomoto (2009)! MS, ~3M " 0.1-1Gyr" in spirals or high-z" RG, ~1M " 1-20Gyr" in ellipticals
5 One-zone Chemical Evolution PopIII"?! EMP" SNII! PopII" SNIa! PopI" Time" M,rotation! M,E,Z" Lifetime, Z" Greggio 05; Matteucci+ 06" for other SNIa models
6 Elemental Abundances SN+HN (CK+ 06); SN+HN+AGB (CK, Karakas, Umeda 2011, MNRAS)" Romano+ 10 for H-W, L-C yields time
7 Isotope Ratios CK, Karakas, Umeda (2011)! SNcc: 12 C, 16 O, ( 18 O), 24 Mg, ( 25,26 Mg)" 4-7M AGB: 13 C, 14 N, 17 O, 25, " 1-4M AGB: 12 C, time
8 Isotope Ratios CK, Karakas, Umeda (2011)! time
9 Chemodynamical Simulations
10 Dynamics of DM, gas, star particles Computing:! Gravity:! GRAPE-SPH code (CK 04)" Parallel Tree-PM SPH code" " Gadget-3 (Springel 05)" Hydrodynamics:! (2001-) Linux (2002-) Linux (2008-) Dρ + ρ v = 0 Dt Dv 1 = P Φ Dt ρ Du P Dρ (κ T) Γ Λ = + + Dt ρ 2 Dt ρ ρ Computational Astrophysics Laboratory COALA@Mt.Stromlo (2009-) 2Φ = 4 πgρ SPH method" ρ i = m jw (ri r j ;h) P P Dv i = m j f i 2i iw ij (hi ) + f j 2j iw ij (h j ) m j Π ij i W ij Dt ρj ρ i STRI-cluster@Herts (2011-) Miracle Consortium@UCL DAi 1 γ 1 γ 1 = m j Π ij v ij i W ij + γ (Γ Λ) γ 1 Dt 2 ρ i ρi With SF&SN: No instantaneous recycling approximation, No multi-phase model" Without AGN Feedback: The issue is not energetics but how to distribute "
11 Physical Processes UV background radiation" (Haardt & Madau 1996)" BH,NS,WD" P=1-exp(-Δt/t sf )" Cooling:" Z-dependent Λ (Sutherland & Dopita 93)" Star Formation! " (1) v<0" " (2) tcool<tdyn" " (3) tdyn<tsound" " Schmidt SFR" " t sf =t dyn /c, c=0.1" " Salpeter/Kroupa IMF" Feedback" 100% thermal" to N FB ~400" or 1kpc" SNIa! SD(Kobayashi et al.1998)! primary: 3-8M WD" secondary: ~1-3M " Z-effect: [Fe/H] > -1.1" 1.3x10 51 erg" SNII/HN" 8-50M " Stellar Wind! 8-120M " 0.2x10 51 (Z/Z ) 0.8 erg" ~ erg" yields (W7, Nomoto et al. 1997) " M,Z,E dependent yields (Kobayashi et al. 2006)"
12 Milky Way-type galaxy Face on" Initial Condition: λcdm fluctuated sphere with λ~0.1, r~3mpc, " M tot ~10 12 M, N tot ~ , M gas ~10 6 M, M DM ~10 7 M " (CK & Nakasato 2011, ApJ, 729, 16) " Edge on"
13 Star Formation Rate Bulge r<1, Solar Neighborhood: 7.5<r<8.5, z <0.5 kpc
14 Metallicity z=0 CK & Nakasato (2011)
15 Metallicity z=0.5 CK & Nakasato (2011)
16 Evolution of Gradients metallicity gradient [dex/kpc] Pilkington, Few, GIbson, CK, 2012 Kobayashi & Nakasato (2011) model redshift
17 Age-Metallicity Relation Observation: Holmberg et al. (2007)
18 Age-Metallicity Relation
19 [O/Fe]-[Fe/H] Relation Observation: Edvardsson et al. (1993), Bensby et al. (2004), Gratton et al. (2003), Cayrel et al. (2004)
20 [O/Fe]-[Fe/H] Relation Observation: McWilliam & Rich (2004), Lecureur et al. (2008)
21 Chemodynamical Simulation (CK & Nakasato 2011) Solar neighborhood
22 Chemodynamical Simulation (CK & Nakasato 2011)
23 Aquarius IC Code: Gadget-3 + SF+FB+CE (CK, Springel, White 07)" Aq-5-C (M gas ~10 5 M ), z=0.5.." Aquila comparison project (Scannapieco et al. 11)
24 Inhomogeneous Chemical Enrichment Star Formation and Chemical Enrichment depend on the local density" Mixing due to dynamical effects (merging, migration) " There is a significant scatter in Age-Metallicity Relation (even in ~1 kpc)" Most metal-poor stars Oldest stars" Some of CEMP/NEMP stars can be explained with the local enrichment from AGB stars (without binary)"
25 Galactic Archaeology surveys Elemental Abundances (from Li to Eu) of million stars in the Local Group will be measured" SEGUE (R~1800)" RAVE (R~7500)" HERMES on AAT (R~28000)" HERMES APOGEE (R~20000) IR" GAIA-ESO (R~20000/40000)" WFMOS on Subaru" WEAVE on WHT" 4MOST on VISATA/NTT" ngcfht!! Chemical Tagging" Freeman & Bland-Hawthorn 2002" Principal Component Analysis (PCA)" Ting, Freeman, CK, De Silva, Bland-Hawthorn 2012 "
26 Principal Component Analysis Y. S. Ting, Freeman, CK, De Silva & Bland-Hawthorn 2011 α-production with/without heavy Fe-peak (Co,Zn) and r-process elements HNe and normal SNe?"
27 Summary CDM! z>2 assembly [α/fe] [(Na,Al,Cu)/Fe] [Mn/Fe] dissipative [α/fe] " inside-out & " thick disk [α/fe] [(Na,Al,Cu)/Fe] &[α/ Fe] " Ia MF " z<1.5 Major merger " " r "
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