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Summary
The kinematics, orbital dynamics and chemical properties of stars
around the sun play an important role in testing the chemical structure of
our Galaxy and its accompanying formation scenarios. The origins of
metal-poor young and old stars of the G-spectral type will be investigated
using compatible methods within the scope of the project.
Such studies of metal-poor stars in the
solar neighborhood serve as a bridge
between stellar astrophysics and galaxy astrophysics. In this context, the
data to be obtained will make an important contribution to the literature on
the chemical structures and dynamics of stars in the solar neighborhood. The findings from a large
number of stars to be examined within the scope of the project proposal will
be included in the literature as a study of statistical importance. Another
feature that makes the project proposal unique is that the spectral,
kinematic and orbital dynamic
properties of a sample of a large number of stars in the solar neighborhood
have not been scrutinized together in the literature. Population distinctions
based on kinematics will be tested with α and Fe abundances to be determined within
the scope of the project proposal for stars. Spectral, kinematic and
orbital dynamic data of stars will be evaluated as a whole with globular
clusters in our galaxy and satellite dwarf galaxies around our galaxy to
investigate possible origin states (evaluation of rupture scenarios) for this
metal-poor sample in the solar neighborhood, including high proper motion
(HPM) sources. In this way, when they are examined within the scope of
rupture scenarios, it will be possible to evaluate whether the HPM stars
included in the sample are natural members of the solar neighborhood.
Within our knowledge, this study is considered to be the most comprehensive
study on metal-poor HPM stars in the literature.
Spectral data of selected program stars for
the realization of the project objectives will be provided from the high
resolution and high S/N (signal/noise) ratio ELODIE, NARVAL
and/or ESPaDOnS Echelle spectra, astrometric data will also be provided from
Gaia eDR3. For program stars that appear to exhibit large changes in model
atmosphere parameters reported in the literature, determination of sensitive
model parameters and element abundances (for example, [Element/Fe] ratios, [α/Fe]),
sensitive age and orbital parameters to be calculated for these sources will
make an important contribution to the literature at the stage of
understanding the physical nature of solar neighborhood.
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