2004ApJ...605..864B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.06CET00:23:07

2004ApJ...605..864B - Astrophys. J., 605, 864-873 (2004/April-3)

Beryllium abundances in F and G dwarfs in Praesepe and other young clusters from Keck HIRES observations.

BOESGAARD A.M., ARMENGAUD E. and KING J.R.

Abstract (from CDS):

The study of both Be and Li gives useful clues about stellar internal structure. Of particular interest is the study of these light elements in open clusters, which have a known age and metallicity. In this paper we present a study of Be abundances in 10 F-type stars in Praesepe and a comprehensive discussion about Be abundances in other open clusters: Hyades, Pleiades, α Per, Coma, and UMa. We have made observations of the doublet of Be II around 3130 Å in Praesepe stars, using the Keck I telescope and the High Resolution Echelle Spectrometer (HIRES). Beryllium abundances were derived from the spectra using the spectrum synthesis method. We find four stars with definite Be depletion in the temperature range of the Li dip like we found in our previous cluster studies, notably for the Hyades and Coma clusters. Putting all the clusters together, we confirm the existence of a Be dip in a narrow temperature range for F stars. Beryllium depletion in this dip is less pronounced than Li depletion. For the cooler stars there is little or no Be depletion, even though there are large depletions of Li. For stars that have little or no Li depletion, A(Li)≥3.0, the ratio Li/Be is 75±4.6, compared to the meteoritic ratio of 77.6. For stars cooler than ∼5900 K there appears to be little or no Be depletion, and the mean A(Be) is 1.30±0.02. For these cooler stars within a given cluster there is no evidence for intrinsic star-to-star differences in A(Be), with the possible exception of the cool Pleiades stars. In the temperature range of the Li-Be dip, a strong correlation exists between Li and Be, consistent with the theory of rotationally induced mixing. Moreover, the slopes of the Li versus Be correlations are different depending on the temperature range. For the full sample of 42 stars between 5900 and 6650 K the slope is 0.43±0.05 [where A(Li) is the abscissa]. The slope is 0.48±0.08 for 6300K<Teff<6650 K and 0.30±0.05 for 5900K<Teff<6300 K. For the Li plateau stars (the cooler subset), the slope is smaller as the impact of the increasing surface convection zone affects the mixing, thus depleting more Li relative to Be. The different behavior in Be depletion for clusters of different ages is consistent with the idea of slow mixing related to rotation during the main-sequence phase of evolution. The range in metallicity in this sample of clusters is only 0.2 dex, so it is difficult to discern any influence of metallicity on the Li-Be relationship; however, the mean A(Be) in the cooler Hyades stars (with [Fe/H]=+0.13) is 1.35±0.02, which is higher than that for the Coma stars (with [Fe/H]=-0.09) of 1.26±0.02 by 0.09 dex.

Abstract Copyright:

Journal keyword(s): Galaxy: Open Clusters and Associations: Individual: Name: Praesepe - Stars: Abundances - Stars: Interiors

CDS comments: Fig. 8 : * Tr 19 = Cl Melotte 111 19

Simbad objects: 55

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Number of rows : 55

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 Cl Melotte 20 OpC 03 26 42 +48 48.0           ~ 769 0
2 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3064 0
3 BD+19 641 SB* 04 00 39.5359905492 +20 22 49.498637871   9.33   8.2   G4V 68 0
4 HD 25825 PM* 04 06 16.1277831435 +15 41 53.234613641   8.416 7.811 7.484 7.169 G0V 168 0
5 HD 26345 PM* 04 10 42.3629962013 +18 25 23.714440814   7.005 6.576 6.329 6.095 F6V 133 0
6 * 45 Tau PM* 04 11 20.2823319709 +05 31 22.987536222   6.057 5.699 5.487 5.284 F4V 228 0
7 HD 26756 PM* 04 14 25.6502208510 +14 37 30.119616339   9.125 8.419 8.039 7.682 G5V 185 0
8 HD 26736 BY* 04 14 32.3143718674 +23 34 29.798017740   8.711 8.047 7.691 7.356 G5V 192 0
9 HD 26784 PM* 04 14 34.3408001832 +10 42 04.995568324   7.606 7.080 6.791 6.511 F8V 176 0
10 HD 27282 PM* 04 19 08.0080652475 +17 31 29.118551040 9.46 9.157 8.427 8.034 7.675 G8V 169 0
11 HD 27406 BY* 04 20 12.9666887102 +19 14 00.523124676   8.016 7.444 7.131 6.826 F9V+ 176 0
12 HD 27561 PM* 04 21 34.7950093588 +14 24 35.245998570   6.999 6.578 6.338 6.099 F5IV-V 210 0
13 * 60 Tau dS* 04 22 03.5181535031 +14 04 37.917221958   6.054 5.710 7.05 5.38 A3m 256 0
14 HD 27808 PM* 04 24 14.5735497717 +21 44 10.484870739   7.646 7.125 6.830 6.550 F8V 181 0
15 HD 28069 PM* 04 25 57.3384056045 +05 09 00.523446879   7.870 7.350     F7V 94 0
16 V* V992 Tau Ro* 04 26 05.8321048864 +15 31 27.616476211 8.11 8.027 7.472 7.161 6.858 ~ 144 0
17 HD 28033 SB* 04 26 18.4986266367 +21 28 13.557737195   7.897 7.334     F8V 146 0
18 V* V906 Tau BY* 04 26 24.6147463863 +16 51 12.093831724 8.86 8.69 8.05 7.51 7.16 G1V 209 0
19 HD 28099 BY* 04 26 40.1215422118 +16 44 48.884181598 8.98 8.78 8.12 7.56 7.23 G2+V 378 0
20 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2743 0
21 V* V993 Tau BY* 04 27 35.8913866973 +15 35 21.092605003   7.949 7.404 7.102 6.805 ~ 211 0
22 HD 28237 PM* 04 27 46.0745623833 +11 44 11.108366342   8.066 7.482     F8 132 0
23 V* V918 Tau BY* 04 28 37.2159666702 +19 44 26.482689542   9.316 8.580 8.182 7.816 G5 122 0
24 HD 28394 SB* 04 29 20.5589466330 +17 32 41.834829803   7.512 7.007 6.724 6.434 F8V 131 0
25 HD 28406 PM* 04 29 30.3505336847 +17 51 47.395473227 7.36 7.352 6.890 6.631 6.373 F6V 174 0
26 HD 28483 PM* 04 30 17.9777149991 +19 50 25.913280997   7.583 7.087     F6V 147 0
27 HD 28608 PM* 04 30 57.1713987199 +10 45 06.362771222   7.491 7.015 6.741 6.479 F7V 114 0
28 HD 28593 PM* 04 31 15.6942612546 +20 07 59.409641235   9.327 8.572 8.169 7.801 G8V 114 0
29 V* V997 Tau BY* 04 32 59.4512598102 +15 49 08.285618403   9.396 8.641 8.235 7.867 ~ 152 0
30 HD 28992 BY* 04 34 35.3101760915 +15 30 16.643497474   8.530 7.898 7.556 7.226 ~ 189 0
31 HD 29225 PM* 04 36 40.7179502876 +15 52 09.677553504   7.074 6.619 6.371 6.115 ~ 128 0
32 HD 29461 PM* 04 38 57.3279273979 +14 06 20.016018199   8.593 7.945 7.585 7.253 G5 111 0
33 HD 30311 PM* 04 46 45.5880309740 +09 01 02.453239840   7.799 7.228 6.906 6.590 F9.5V 89 0
34 HD 30355 PM* 04 47 37.5748280455 +18 15 31.493078594   9.258 8.522     G0 66 0
35 HD 30738 EB* 04 50 48.5434455463 +16 12 37.623048440   7.797 7.266     ~ 121 0
36 HD 30869A SB* 04 51 49.978609 +13 39 18.53294   6.81 6.36     ~ 179 0
37 HD 30869 ** 04 51 49.9954760810 +13 39 18.503094115   6.751 6.250 7.34 5.674 ~ 181 0
38 * 101 Tau PM* 04 59 44.3215855444 +15 55 00.238515439   7.220 6.747     F5V 122 0
39 BD+19 2045 SB* 08 36 29.8525487287 +18 57 56.988077325   9.86 9.50     F6V 33 0
40 HD 73597 * 08 39 54.3270222879 +20 33 36.761726975   9.859 9.606     F6V 46 0
41 BD+20 2151 * 08 39 55.0643361479 +20 03 54.091691893   10.553 10.098 10.06   F4V 43 0
42 HD 73641 * 08 39 58.0672424750 +19 12 05.871841674   9.92 9.54     F3V 64 0
43 NGC 2632 OpC 08 40 24 +19 40.0           ~ 1290 0
44 Cl* NGC 2632 S 121 Er* 08 40 25.5399945410 +19 28 32.737748021   10.37 9.89     F5V 44 0
45 BD+19 2074 * 08 40 46.0856797986 +19 18 34.561499324   9.967 9.50     F4V 49 0
46 BD+20 2176 Ro* 08 41 10.0217721604 +19 30 32.064558222   10.613 10.080     F7V 49 0
47 HD 73854 V* 08 41 10.6779287328 +19 49 46.344451866   9.37 9.03     F2IV+ 65 0
48 BD+20 2180 * 08 41 26.9796188896 +19 32 32.873963951   10.315 9.816     F4V 41 0
49 BD+20 2183 SB* 08 41 42.2954949252 +19 39 37.963331268   10.02 9.60     F6V 46 0
50 HD 73994 SB* 08 41 57.8188013976 +18 54 42.224882965   9.84 9.44     F5V 47 0
51 NGC 2682 OpC 08 51 18 +11 48.0           ~ 2088 0
52 V* GM Com dS* 12 12 24.8946040823 +27 22 48.355145120   8.44 8.1     F2-3V 105 0
53 Cl Melotte 111 OpC 12 25 06.00 +26 06 00.0           ~ 419 0
54 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 390 2
55 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4319 2

    Equat.    Gal    SGal    Ecl

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2021.03.06-00:23:07

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