J/AZh/81/209 Neutron capture elements in stars: neodymium (Mashonkina+, 2004)
Neutron capture elements in halo, thick disk and thin disk stars: neodymium.
Mashonkina L.I., Kamaeva L.A., Samotoev V.A., Sakhibullin N.A.
<Astron. Zh. 81, 209 (2004)>
=2004AZh....81..209M 2004AZh....81..209M
=2004ARep...48..185M 2004ARep...48..185M
ADC_Keywords: Stars, dwarfs; Spectroscopy; Abundances
Abstract:
We have derived the LTE neodymium abundances in 60 cool stars with
[Fe/H] from 0.25 to -1.71 by applying a synthetic-spectrum analysis to
spectroscopic observations of NdII lines with a resolution of
λ/Δλ∼60000 and signal-to noise ratios of 100-200.
Description:
We determined the neodymium abundances for 60 of the 78 stars studied
by Mashonkina et al. (2003A&A...397..275M 2003A&A...397..275M). We obtained spectroscopic
observations of seven stars in April 2001 with the UVES echelle
spectrometer mounted on the 8-m VLT2 telescope of the European
Southern Observatoryin Chile. These observations cover 3800-4500Å
and 4750-6650Å. Spectroscopic observations of 53 stars at
4100-6700Å were obtained in 1995-2001 with the FOCES echelle
spectrometer mounted on the 2.2-m telescope of the German-Spanish
Astronomical Center in Calar Alto, Spain.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 60 Stellar parameters of the selected
sample and the final [Nd/Fe] ratios
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name HD/BD name
14- 17 I4 K Teff Effective temperature (1)
20- 23 F4.2 [cm/s2] logg Surface gravity (2)
26- 28 F3.1 km/s VTurb Microturbulence velocity
31- 35 F5.2 [Sun] [Fe/H] Relative iron abundance
38- 42 F5.2 [Sun] [Nd/Fe] Neodymium abundance
45- 48 F4.2 [Sun] e_[Nd/Fe] ? Standard deviation in [Nd/Fe]
51 I1 --- o_[Nd/Fe] Number of lines used
55- 56 A2 --- Pop Code for population (3)
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Note (1): Effective temperature derived from the profiles of the H(α)
and H(β) lines.
Note (2): Surface gravity was determined using two methods - by analyzing
the wings of strong MgI lines and from HIPPARCOS trigonometric parallaxes
Note (3): Code indicates the galactic population as follows:
0: thin disk
1: thick disk
2: halo
01: the transition between the thin and thick disks
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(End) Veta Avedisova[INASAN] 10-Dec-2004