  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. 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.
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.
