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Quest for the lost siblings of the Sun

Liu, Cheng LU ; Ruchti, Gregory LU ; Feltzing, Sofia LU ; Martinez-Barbosa, C. A.; Bensby, Thomas LU ; Brown, A. G. A. and Zwart, S. F. Portegies (2015) In Astronomy & Astrophysics 575.
Abstract
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... (More)
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 Suns birth cluster in analytical Galactic model and found that most of the radial velocities of the solar siblings lie in the range -10 <= V-r <= 10 km s(-1), which is smaller than the radial velocity of HIP 40317 (V-r = 34.2 km s(-1)), under different Galactic parameters and different initial conditions of the Suns birth cluster. The sibling status for HIP 40317 is not directly supported by our dynamical analysis (Less)
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author
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
stars: abundances, stars: fundamental parameters, solar neighborhood
in
Astronomy & Astrophysics
volume
575
publisher
EDP Sciences
external identifiers
  • wos:000350249100051
  • scopus:84923247614
ISSN
0004-6361
DOI
10.1051/0004-6361/201424998
language
English
LU publication?
yes
id
3693fb80-e142-4f03-8e95-72449e92514e (old id 5297127)
date added to LUP
2015-04-27 08:54:18
date last changed
2017-01-01 06:05:50
@article{3693fb80-e142-4f03-8e95-72449e92514e,
  abstract     = {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 Suns birth cluster in analytical Galactic model and found that most of the radial velocities of the solar siblings lie in the range -10 &lt;= V-r &lt;= 10 km s(-1), which is smaller than the radial velocity of HIP 40317 (V-r = 34.2 km s(-1)), under different Galactic parameters and different initial conditions of the Suns birth cluster. The sibling status for HIP 40317 is not directly supported by our dynamical analysis},
  articleno    = {A51},
  author       = {Liu, Cheng and Ruchti, Gregory and Feltzing, Sofia and Martinez-Barbosa, C. A. and Bensby, Thomas and Brown, A. G. A. and Zwart, S. F. Portegies},
  issn         = {0004-6361},
  keyword      = {stars: abundances,stars: fundamental parameters,solar neighborhood},
  language     = {eng},
  publisher    = {EDP Sciences},
  series       = {Astronomy & Astrophysics},
  title        = {Quest for the lost siblings of the Sun},
  url          = {http://dx.doi.org/10.1051/0004-6361/201424998},
  volume       = {575},
  year         = {2015},
}