2002ApJ...579..616J

Query : 2002ApJ...579..616J

2002ApJ...579..616J - Astrophys. J., 579, 616-625 (2002/November-2)

The r-process in the early galaxy.

JOHNSON J.A. and BOLTE M.

Abstract (from CDS):

We report Sr, Pd, and Ag abundances for a sample of metal-poor field giants and analyze a larger sample of Y, Zr, and Ba abundances. The [Y/Zr] and [Pd/Ag] abundance ratios are similar to those measured for the r-process-rich stars CS 22892-052 and CS 31082-001. The [Pd/Ag] ratio is larger than predicted from the solar system r-process abundances. The constant [Y/Zr] and [Sr/Y] values in the field stars place strong limits on the contributions of the weak s-process and the main s-process to the light neutron-capture elements. Stars in the globular cluster M15 possess lower [Y/Zr] values than the field stars. There is a large dispersion in [Y/Ba]. Because the r-process is responsible for the production of the heavy elements in the early Galaxy, these dispersions require varying light-to-heavy ratios in r-process yields.

Abstract Copyright: ∼

Journal keyword(s): Galaxy: Halo - Nuclear Reactions, Nucleosynthesis, Abundances - Stars: Abundances - Stars: Population II

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 BD-11 145 Pe* 00 48 24.3140894760 -10 41 30.892554816   11.54 10.72     KIIvw 52 0
2 BD-16 251 RG* 01 29 31.1311443552 -16 00 45.495314460 12.527 12.427 11.642 11.189 10.713 CEMP 291 0
3 V* HP Eri LP* 04 38 55.7330378304 -13 20 48.133934448 10.91 9.72 8.33     G8/K0IIIwF7 132 0
4 HD 63791 PM* 07 54 28.7247271128 +62 08 10.773103272   8.81 7.90     G0 112 0
5 HD 88609 Pe* 10 14 28.9853799600 +53 33 39.342740796 9.930 9.540 8.620 7.78 7.15 G5IIIw 202 0
6 HD 103113 * 11 52 24.3742253880 +07 32 41.360006940   11.17 9.71     K5 5 0
7 HD 108577 Pe* 12 28 16.8614710944 +12 20 41.089853184   10.18 9.6 9.8   KIIvw 74 0
8 BD+04 2621 Pe* 12 28 44.6433260568 +04 01 26.631027984   10.86 9.90     KIIvw 59 0
9 BD+10 2495 SB* 12 59 19.9306410576 +09 14 35.634594444   10.44 9.73     G0 77 0
10 HD 115444 Pe* 13 16 42.4590842616 +36 22 52.692135420   9.77 8.97 8.3 7.88 G9V 243 0
11 HD 122563 Pe* 14 02 31.8455084952 +09 41 09.944391876 7.47 7.10 6.19 5.37 4.79 G8:III:Fe-5 854 0
12 HD 126587 Pe* 14 27 00.3636631296 -22 14 38.992940592   9.88 9.60 8.75   CEMP-no 132 0
13 BD+18 2890 HB* 14 32 13.4860470912 +17 25 24.289741704   10.49 9.73     ~ 67 0
14 HD 128279 Pe* 14 36 48.5108525999 -29 06 46.612858494 8.64 8.63 8.00     Gw 194 0
15 BD+05 3098 Pe* 15 52 17.2564983936 +05 17 44.338170732   11.26 10.56     ~ 46 0
16 BD+09 3223 HB* 16 33 35.5815849384 +09 06 16.307942544   9.85 9.27     ~ 77 0
17 BD+17 3248 HB* 17 28 14.4690179544 +17 30 35.847574776   10.02 9.34     KIIvw 224 0
18 V* V2564 Oph LP? 18 04 40.0713763656 +03 46 44.716990584 9.53 8.59 7.30 6.24 5.43 F6/7V 259 0
19 HD 186478 SB* 19 45 14.1409752672 -17 29 27.071239056   10.116 9.302 8.527 7.961 K2III 154 0
20 BD-18 5550 Pe* 19 58 49.7371417608 -18 12 11.140126164 10.18 10.03 9.35 9.04 8.74 CEMP-no 173 0
21 BD-17 6036 Pe* 20 37 15.9313308384 -16 33 58.063824468   11.27 10.56     ~ 46 0
22 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3140 0
23 BPS CS 22892-0052 Pe* 22 17 01.6558764360 -16 39 27.051026544   14.03 13.20 13.06 12.19 KIIvw 448 0
24 HD 216143 Pe* 22 50 31.0883724288 -06 54 49.554279360   8.78 7.81 7.44   G2/3(IV)(we) 143 0
25 HD 218857 Pe* 23 11 24.5948299440 -16 15 04.026507912   9.60 9.0     G5/8w(a) 115 0

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