| Issue |
A&A
Volume 575, March 2015
|
|
|---|---|---|
| Article Number | A51 | |
| Number of page(s) | 15 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/201424998 | |
| Published online | 20 February 2015 | |
Quest for the lost siblings of the Sun ⋆,⋆⋆
1 Lund ObservatoryDepartment of Astronomy and Theoretical Physics Box 43 221 00 Lund Sweden
e-mail: cheng@astro.lu.se; greg@astro.lu.se; sofia@astro.lu.se
2 Leiden Observatory, University of Leiden, PB 9513, 2300 RA Leiden, The Netherlands
Received: 16 September 2014
Accepted: 19 November 2014
Aims. The aim of this paper is to find lost siblings of the Sun by analyzing high resolution spectra. Finding solar siblings will enable us to constrain the parameters of the parental cluster and the birth place of the Sun in the Galaxy.
Methods. The solar siblings can be identified by accurate measurements of metallicity, stellar age and elemental abundances for solar neighbourhood stars. The solar siblings candidates were kinematically selected based on their proper motions, parallaxes and colours. Stellar parameters were determined through a purely spectroscopic approach and partly physical method, respectively. Comparing synthetic with observed spectra, elemental abundances were computed based on the stellar parameters obtained using a partly physical method. A chemical tagging technique was used to identify the solar siblings.
Results. We present stellar parameters, stellar ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Ti, Cr, Fe, and Ni for 32 solar sibling candidates. Our abundances analysis shows that four stars are chemically homogenous together with the Sun. Technique of chemical tagging gives us a high probability that they might be from the same open cluster. Only one candidate – HIP 40317 – which has solar metallicity and age could be a solar sibling. We performed simulations of the Sun’s birth cluster in analytical Galactic model and found that most of the radial velocities of the solar siblings lie in the range −10 ≤ Vr ≤ 10 km s-1, which is smaller than the radial velocity of HIP 40317 (Vr = 34.2 km s-1), under different Galactic parameters and different initial conditions of the Sun’s birth cluster. The sibling status for HIP 40317 is not directly supported by our dynamical analysis.
Key words: stars: abundances / stars: fundamental parameters / solar neighborhood
Based on observations made with Nordic Optical Telescope at La Palma under programme 44-014. Based on observations made with ESO VLT Kueyen Telescope at the Paranal observatory under program me ID 085.C-0062(A), 087.D-0010(A), and 088.B-0820(A). Based on data obtained from the ESO Science Archive Facility under programme ID 078.D-0080(A), 080,A-9006(A), 082.C-0446(A), 082.A-9007(A), 083,A-9004(B), and 089.C-0524(A).
Full Table 2 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/575/A51
© ESO, 2015
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