HD018768
HD18768 in T.V.Mishenina+,AAP, 396, 189, 2002
taken from 5 paper(s):
/T.V.Mishenina et al.(2002)/
/T.V.Mishenina and V. V. Kovtyukh(2001)/
/J.Simmerer et al.(2004)/
/M.Takada-Hidai et al.(2002)/
/K.A.Venn et al.(2004)/

T.V.Mishenina et al.,AAP, 396, 189, 2002 (A0070,ADS)
Abundances of Cu and Zn in metal-poor stars: Clues for Galaxy evolution
Stellar Parameters
Chemical Abundances
| | Original Data | Converted Data Asplund et al. (2009) | |
Element | Nline | [X/H] | [X/Fe] | log-e | [X/H] | [X/Fe] | log-e | Element |
Fe | N/A | -0.51 | ... | ... | ... | ... | Fe |
Cu I | N/A | ... | -0.12+-0.25 | ... | ... | ... | Cu I |
Zn I | N/A | ... | 0.21+-0.23 | ... | ... | ... | Zn I |
Observing Log
Date of Observation | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
N/A | N/A | ELODIE | 42000 | >100 | N/A | N/A |
Galactic Longitude (l) : N/A | Galactic Latitude (b) : N/A | Declination : N/A | Right Ascension : N/A |
T.V.Mishenina et al.,AAP, 370, 951, 2001 (A0071,ADS)
Analysis of neutron capture elements in metal-poor stars
Stellar Parameters
Teff : 5700 | log g : 3.5 | vturb : 1.0 |
Chemical Abundances
| | Original Data | Converted Data Asplund et al. (2009) | |
Element | Nline | [X/H] | [X/Fe] | log-e | [X/H] | [X/Fe] | log-e | Element |
Mg I | N/A | ... | 0.00 | ... | ... | ... | Mg I |
Si I | N/A | ... | 0.10 | ... | ... | ... | Si I |
Ca I | N/A | ... | 0.15 | ... | ... | ... | Ca I |
Fe | N/A | -0.51 | ... | ... | ... | ... | Fe |
Sr I | N/A | ... | -0.04 | ... | ... | ... | Sr I |
Ba II | N/A | ... | 0.22 | ... | ... | ... | Ba II |
La II | N/A | ... | 0.03 | ... | ... | ... | La II |
Ce II | N/A | ... | -0.06 | ... | ... | ... | Ce II |
Nd II | N/A | ... | 0.01 | ... | ... | ... | Nd II |
Eu II | N/A | ... | 0.26 | ... | ... | ... | Eu II |
Observing Log
Date of Observation | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
N/A | N/A | ELODIE | 42000 | >100 | N/A | N/A |
J.Simmerer et al.,ApJ, 617, 1091, 2004 (A0131,ADS)
The Rise of the s-Process in the Galaxy
Chemical Abundances
| | Original Data | Converted Data Asplund et al. (2009) | |
Element | Nline | [X/H] | [X/Fe] | log-e | [X/H] | [X/Fe] | log-e | Element |
Fe I | N/A | -0.65 | ... | ... | ... | ... | Fe I |
Fe II | N/A | -0.71 | ... | ... | ... | ... | Fe II |
La II | N/A | ... | ... | 0.45 | ... | ... | La II |
Eu II | N/A | ... | ... | -0.07 | ... | ... | Eu II |
Observing Log
Date of Observation | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
| N/A | MCDONALD | 60000 | 100 | N/A | N/A |
Galactic Longitude (l) : N/A | Galactic Latitude (b) : N/A | Declination : N/A | Right Ascension : N/A |
M.Takada-Hidai et al.,ApJ, 573, 614, 2002 (A0184,ADS)
Behavior of Sulfur Abundances in Metal-poor Giants and Dwarfs
Stellar Parameters
Teff : 5750+-100 | log g : 3.84+-0.15 | vturb : 1.9+-0.5 |
Chemical Abundances
| | Original Data | Converted Data Asplund et al. (2009) | |
Element | Nline | [X/H] | [X/Fe] | log-e | [X/H] | [X/Fe] | log-e | Element |
S I | N/A | -0.36 | ... | 6.86 | ... | S I |
Fe I | N/A | -0.70 | ... | 6.71 | ... | Fe I |
Observing Log
Date of Observation | JD | Facility | Resolution | S/N | Exposure Time | Vrad |
| N/A | OAO | 24500 | 120-400 | N/A | N/A |
Galactic Longitude (l) : N/A | Galactic Latitude (b) : N/A | Declination : N/A | Right Ascension : N/A |
K.A.Venn et al.,AJ, 128, 1177, 2004 (C0011,ADS)
Stellar Chemical Signatures and Hierarchical Galaxy Formation
Chemical Abundances
| | Original Data | Converted Data Asplund et al. (2009) | |
Element | Nline | [X/H] | [X/Fe] | log-e | [X/H] | [X/Fe] | log-e | Element |
Na | N/A | ... | 0.1 | ... | ... | ... | Na |
Mg | N/A | ... | 0.17 | ... | ... | ... | Mg |
Ca | N/A | ... | 0.05 | ... | ... | ... | Ca |
Ti | N/A | ... | 0.09 | ... | ... | ... | Ti |
Fe | N/A | -0.62 | ... | ... | ... | ... | Fe |
Ni | N/A | ... | 0.04 | ... | ... | ... | Ni |
Y | N/A | ... | -0.11 | ... | ... | ... | Y |
Ba | N/A | ... | -0.25 | ... | ... | ... | Ba |
Observing Log
Galactic Longitude (l) : N/A | Galactic Latitude (b) : N/A | Declination : +470638 | Right Ascension : 030252.3 |