Volume 567, July 2014
|Number of page(s)||5|
|Published online||04 July 2014|
Departamento de Astronomia do IAG/USPUniversidade de São Paulo, rua do
Matão 1226, Cidade Universitária,
2 Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston ACT 2611, Australia
3 McDonald Observatory and Department of Astronomy, University of Texas at Austin, USA
Received: 9 May 2014
Accepted: 9 June 2014
Context. The standard solar model fails to predict the very low lithium abundance in the Sun, which is much lower than the proto-solar nebula (as measured in meteorites). This Li problem has been debated for decades, and it has been ascribed either to planet formation or to secular stellar depletion due to additional mixing below the convection zone, either during the pre-main sequence and thus possibly linked to planet formation, or additionally on secular time-scales during the main sequence. In order to test the evolution of Li, it is important to find solar twins in a range of ages, i.e., stars with about one solar mass and metallicity but in different evolutionary stages. Furthermore, the study of stars similar to the Sun is relevant in relation to the signature of terrestrial planet formation around the Sun, and for anchoring photometric and spectroscopic stellar parameter scales.
Aims. We aim to identify and analyse solar twins using high quality spectra, in order to study Li depletion in the Sun and the possible relation between chemical abundance anomalies and planet formation.
Methods. We acquired high-resolution (R ~ 110 000), high S/N (~300) ESO/VLT UVES spectra of several solar twin candidates and the Sun (as reflected from the asteroid Juno). Among the solar twin candidates we identify HIP 114328 as a solar twin and perform a differential line-by-line abundance analysis of this star relative to the Sun.
Results. HIP 114328 has stellar parameters Teff = 5785 ± 10 K, log g = 4.38 ± 0.03, [ Fe/H] = −0.022 ± 0.009, and a microturbulent velocity 0.05 ± 0.03 km s-1 higher than solar. The differential analysis shows that this star is chemically very similar to the Sun. The refractory elements seem slightly more depleted than in the Sun, meaning that HIP 114328 may be as likely to form terrestrial planets as the Sun. HIP 114328 is about 2 Gyr older than the Sun, and is thus the second oldest solar twin analysed at high precision. It has a Li abundance of A(Li)NLTE ≲ 0.46, which is about 4 times lower than in the Sun (A(Li)NLTE = 1.07 dex), but close to the oldest solar twin known, HIP 102152.
Conclusions. Based on the lower abundances of refractory elements when compared to other solar twins, HIP 114328 seems an excellent candidate to host rocky planets. The low Li abundance of this star is consistent with its old age and fits very well the emerging Li-age relation among solar twins of different ages.
Key words: Sun: abundances / stars: fundamental parameters / stars: abundances / planetary systems
Based on observations obtained at the European Southern Observatory (ESO) Very Large Telescope (VLT) at Paranal Observatory, Chile (observing program 083.D-0871).
Table 1 is available in electronic form at http://www.aanda.org
© ESO, 2014
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