30 4 Vol. 30, No. 4 2012 11 PROGRESS IN ASTRONOMY Nov., 2012 1000-8349(2012)04-453-14 1,2,3 1,2 Kirby Evan N 4,5 Guhathakurta Puragra 6 (1. 100012 2. 100012 3. 100049 4. California Institute of Technology, 1200 E. California Blvd., MC 249-17, Pasadena, CA 91125, USA 5. Hubble Fellow 6. University of California Observatories/Lick Observatory, University of California, 1156 High St., Santa Cruz, CA 95064, USA) T > 2.5 10 6 K 7 Li(p, α) 4 He A(Li) = 12 + lg[n(li)/n(h)] A(Li) < 0.5 P152 A 1 ( 7 Li) [1] WMAP(Wikinson Microwave Anisotropy Probe) 3 He(α, γ) 7 Li A(Li) = 2.72 [2] 140 2012-04-17 2012-07-02 (10973015, 11061120454) Hubble Fellowship grant(51256.01) NASA(NAS 5-26555) NSF(AST09-37525, AST-1010039)
454 30 7 Li 6 Li [3, 4] ISM (Galactic cosmic ray) 7 Li 6 Li ( R 100 000 S/N 500 ) 7 Li I II ; [5] Spite Plateau [6] [6, 7] [8, 9] (A(Li) = 2.3 A(Li) = 12 + lg[n(li)/n(h)] n ) T > 2.5 10 6 K 7 Li(p, α) 4 He ( 6 Li T > 2.0 10 6 K ) 1/20 1/15 [8] (extra mixing) [10] bump A(Li) 0.5 [8] 1% [11 15] 2 2.5 10 6 K Spite CFH [16] 5700 K 6250 K ( 2.4 [Fe/H] 1.4) A(Li)=2.05 Spite Plateau [8, 17 19], A(Li) = 2.3 Spite Plateau (A(Li) = 2.3) (A(Li) = 2.72) [2] (forbidden zone)
4 455 Piau 2/3 [20] Charbonnel Talon [21] Spite Plateau Sbordone ( 3.5 [Fe/H] 2.5) [Fe/H]< 3 A(Li) 1 dex A(Li) 0.3 dex A(Li) [22] 10 [5] 3 1982 Wallerstein Sneden [23] 30 1 64 [12, 15] 1 Star name [Fe/H] /dex T eff /K lg(g)/dex A(Li)/dex C1012254-203007 [12] 2.55 4518.0 1.1 2.52 J043154.1-063210 [12] 1.85 5440.0 2.5 1.69 J142546.2-154629 [12] 2.08 4341.0 0.9 3.86 J195244.9-600813 [12] 1.41 5025.0 2.1 1.73 T5496-00376-1 [12] 0.63 4887.0 2.2 3.28 T6953-00510-1 [12] 1.93 4867.0 1.8 2.82 T8448-00121-1 [12] 2.45 4655.0 1.1 3.71 T9112-00430-1 [12] 2.21 4370.0 0.0 3.15 M3-IV101 [12] 1.52 4236.0 0.6 3.49 M68-A96 [12] 2.18 4549.0 0.9 2.95 PDS 365 [24] 0.09 4540.0 2.2 3.3 IRAS 19285+0517 [25] 0.14 4500.0 2.5 2.5 HD 30834 [26] 0.5 4500.0 1.5 2.4 HD 146850 [26] 0.4 4270.0 1.4 2.0 HD 219025 [26] 0.1 4500.0 2.3 3.0 G0928+73.2600 [27] 0.25 4885.0 2.65 3.3 Monaco142173 [14] 0.69 4330.0 1.5 2.8
456 30 Star name [Fe/H] /dex T eff /K lg(g)/dex A(Li)/dex Monaco171877 [14] 0.77 3930.0 1.1 2.49 Monaco225245 [14] 0.99 3920.0 0.65 2.9 Monaco313132 [14] 0.01 4530.0 2.0 3.45 Monaco343555 [14] 0.62 4530.0 2.25 1.79 HD 8676 [28] 0.02 4860.0 2.95 3.86 HD 10437 [28] 0.1 4830.0 2.85 3.76 HD 12203 [28] 0.27 4870.0 2.65 2.01 HD 37719 [28] 0.09 4650.0 2.4 2.7 HD 40168 [28] 0.1 4800.0 2.5 1.49 HD 51367 [28] 0.2 4650.0 2.55 2.58 HD 77361 [28] 0.02 4580.0 2.35 3.96 HD 88476 [28] 0.1 5100.0 3.1 2.12 HD 107484 [28] 0.18 4640.0 2.5 2.04 HD 118319 [28] 0.25 4700.0 2.2 1.88 HD 133086 [28] 0.02 4940.0 2.98 2.03 HD 145457 [28] 0.08 4850.0 2.75 2.49 HD 150902 [28] 0.09 4690.0 2.55 2.64 HD 167304 [28] 0.18 4860.0 2.95 2.95 HD 170527 [28] 0.1 4810.0 2.85 3.31 D461 [29] 2.0 3600.0 0.0 3.5 Monaco1016 [30] 0.78 3800.0 0.8 4.29 Monaco1076 [30] 0.74 3750.0 0.7 3.58 labzelter42 [31] 0.85 4096.0 1.2 3.2 labzelter80 [31] 0.83 4099.0 1.5 2.0 labzelter123 [31] 0.96 4278.0 1.7 2.1 Scl 1004838 [15] 1.59 4564.0 1.49 4.08 Scl 1004861 [15] 1.7 4866.0 1.74 2.98 For 55609 [15] 0.73 3863.0 0.55 4.09 For 60521 [15] 0.86 4193.0 0.69 2.89 For 90067 [15] 0.68 3768.0 0.4 2.94 For 100650 [15] 0.95 4422.0 1.18 4.49 LeoI 21617 [15] 1.1 4249.0 0.75 4.38 LeoI 32266 [15] 1.35 4690.0 1.16 2.31 LeoI 60727 [15] 1.42 4182.0 0.72 4.21 LeoI 71032 [15] 1.29 4410.0 0.9 3.09 LeoII C-3-146 [15] 1.24 4981.0 1.57 3.4 LeoII C-7-174 [15] 1.4 4501.0 1.18 4.43 CVnI 195 195 [15] 2.61 4286.0 0.66 4.64
4 457 Star name [Fe/H] /dex T eff /K lg(g)/dex A(Li)/dex CVnI 196 129 [15] 2.82 4507.0 0.85 4.58 HD 90633 [32] 0.02 4596.0 2.3 1.85 HD 63798 [32] 0.1 5004.0 2.5 1.75 HD 9746 [11] 0.13 4420.0 2.3 2.7 HD 112127 [11] 0.31 4340.0 2.1 2.7 HD 19745 [33] 0.05 4700.0 2.25 3.7 IRAS 13539-4153 [33] 0.13 4300.0 2.25 4.1 IRAS 17596-3952 [33] 0.1 4600.0 2.5 2.2 HD 39853 [34] 0.5 3900.0 1.16 2.8 6708 Å Li I 2 [35] Li I 6103.54 Å 6103.65 Å [36] 2 Li I [35] J J F F λ/å gf 7 Li 1/2 3/2 1 0,1,2 6707.7561 0.373 2 1,2,3 6707.7682 0.622 1/2 1/2 1 2 6707.9066 0.031 1 1 6707.9080 0.156 2 2 6707.9187 0.156 2 1 6707.9200 0.156 6 Li 1/2 3/2 1/2 1/2,3/2 6707.9196 0.332 3/2 all 6707.9230 0.664 1/2 1/2 all all 6708.0728 0.498 1 A(Li) 0.5 AGB [37] RGB bump [38] [39] RGB AGB TIP-RGB s
458 30 1 x y A(Li) = 12 + lg[n(li)/n(h)] [11, 12, 14, 15, 24, 26 31, 33, 34, 40, 41] II [5] WMAP 3.1 AGB 1971 Cameron Fowler (AGB) 7 Be ( 7 Be-transport mechanism) Cameron-Fowler [42] 3 He 3 He 3 He(α, γ) 7 Be 7 Be 3 7 M AGB 7 Be 7 Be 7 Li( 7 Be(e, ν) 7 Li ) HBB(Hot Bottom Burning) Sackmann Boothroyd 1992 [13] Ventura D Anona 2009 5 M AGB HBB HBB [43] HBB AGB [44] Smith Lambert 1989 5 Li I S A(Li) 2.2 3.8 TIP-AGB HBB (3 7 M ) s Smith Lambert HBB S HBB AGB AGB RGB [12, 23, 40] (Draco) D461 [29] AGB HBB
4 459 3 He 7 Be HBB (extra mixing) 3.2 RGB 2.5 7 Be [39, 45] CBP(Cool bottom Processing) CBP A(Li)=4 3 He AGB CBP CBP [14] [23], bulge [31] Kraft 1999 M3 (NGC5272) A(Li)=3.0 IV-101 [40] 2011 Ruchti RAVE IV-101 [12] 700 ([Fe/H]< 0.5) 8 1 M68 Ruchti RGB-bump RGB-tip CBP RGB-bump 3 He RGB-tip 3.1 D461 Monaco Bonifacio 2008 4.29 3.58 RGB-tip [30] 4 14 Kirby 2010 Keck II DEIMOS (R=6500) [46] 8 Li I 6708 Å 10 2054 [15] 14 3 14 D461 [29] 15 2054
460 30 [11 14] 14 (Sculptor) (Fornax) I (Leo I) II (Leo II) I (Canes Venatici I) 3 CVnI 196 129 3 7 M HBB AGB 2 CMD AGB RGB 2 5 [15] RGB bump [47] RGB bump 3 14 Li I 175 694 må Li I LTE ATLAS9 [48, 49] MOOG σ noise σ Teff σ noise A(Li), σ Teff 100 K 100 K NLTE σ Teff σ noise σ Teff 3 6 Li 6 Li [50] 9 A(Li)=2.72 [2] NLTE 3 Lind [51] NLTE NLTE A(Li) LTE σ
4 461 3 14 Star Name Teff/K lg(g)/cm s 2 [Fe/H] EW(Li I λ6708) /må A(Li)LTE A(Li)NLTE σnoise σteff Scl 1004838 4564 1.49 1.59 ± 0.11 363 ± 19 3.32 2.97 0.12 0.24 Scl 1004861 4866 1.74 1.70 ± 0.12 193 ± 28 2.46 2.37 0.15 0.15 For 55609 3863 0.55 0.73 ± 0.11 694 ± 24 3.69 3.68 0.10 0.14 For 60521 4193 0.69 0.86 ± 0.11 382 ± 34 2.11 2.25 0.13 0.20 For 90067 3768 0.40 0.68 ± 0.11 503 ± 23 2.02 1.76 0.30 0.11 For 100650 4422 1.18 0.95 ± 0.11 492 ± 27 3.74 3.57 0.14 0.22 LeoI 21617 4249 0.75 1.10 ± 0.11 546 ± 52 3.53 3.43 0.37 0.19 LeoI 32266 4690 1.16 1.35 ± 0.12 175 ± 31 2.07 2.15 0.13 0.17 LeoI 60727 4182 0.72 1.42 ± 0.12 514 ± 49 3.49 3.40 0.39 0.19 LeoI 71032 4410 0.90 1.29 ± 0.11 322 ± 28 2.50 2.48 0.15 0.23 LeoII C-3-146 4501 1.18 1.40 ± 0.11 449 ± 31 3.52 3.26 0.16 0.33 LeoII C-7-174 4981 1.57 1.24 ± 0.12 225 ± 42 2.92 2.72 0.15 0.16 CVnI 195 195 4286 0.66 2.61 ± 0.12 527 ± 18 3.98 3.85 0.20 0.28 CVnI 196 129 4507 0.85 2.82 ± 0.13 380 ± 35 3.64 3.15 0.23 0.27
462 30 3 14 M v V 0 V RGB bump V RGB bump T eff lg g [Fe/H] 3 Ruchti [12]
4 463 3 (1) Drake, (v sin i 8 km s 1 ), Hα [24] (v sin i 1 km s 1 ) [52] Kumar (Hipparcos catalog) 15 [28] (2) AGB AGB HBB 3 7 M AGB (3) (ISM) 6 Li [3, 4] 6 Li( 2) ISM 6 Li 7 Li R 100 000 S/N 500 Melo [53] Denissenkov Weiss (extra mixing) [54] 14 5 Spite Plateau 30
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466 30 Observation of Lithium-rich Giants FU Xiao-ting 1,2,3, DENG Li-cai 1,2, KIRBY Evan N 4,5, GUHATHAKURTA Puragra 6 ( 1. Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; 2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; 3. Graduate University of Chinese Academy of Sciences, Beijing 100049, China; 4. California Institute of Technology, 1200 E. California Blvd., MC 249-17, Pasadena, CA 91125, USA; 5. Hubble Fellow; 6. University of California Observatories/Lick Observatory, University of California, 1156 High St., Santa Cruz, CA 95064, USA) Abstract: Lithium is efficiently destroyed via the 7 Li(p, α) 4 He reaction when the temperature reaches T > 2.5 10 6 K. The standard model of stellar evolution predicts that the Li abundances of evolved red giants, whose convective envelopes reach such high temperatures, should be below A(Li)=0.5. However, some giants with various spectral types and at various evolutionary stages have been found to have higher Li abundances. Some of them have Li abundances even higher than the primordial abundance from the Big Bang. Such discoveries challenge the standard theory of stellar evolution. We review Li abundance observations from the main sequence to the red giant branch. The latest survey for Li-rich giants in the dwarf galaxies of the Milky Way is discussed in detail, including the most metal-poor Li-rich giants known to date. Because lots of the stars have a Li abundance larger than the universe s primordial value, lithium in these stars must have been created rather than survived from destruction. This article provides an overview on the current status of the observations of Li-rich giants and the possible scenarios proposed so far to explain their lithium enhancement. Key words: stars; giant; abundances; lithium