Context :

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 \leq \mathrm { V _ { r } } \leq 10 \mathrm { km~ { } s ^ { -1 } } , which is smaller than the radial velocity of HIP 40317 ( \mathrm { V _ { r } } = 34.2 ~ { } \mathrm { 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 .

Conclusions :