Version 1
: Received: 20 October 2024 / Approved: 21 October 2024 / Online: 21 October 2024 (12:01:35 CEST)
How to cite:
Yushchenko, A.; Andrievsky, S.; Demessinova, A.; Jeong, Y.; Yushchenko, V.; Doikov, D.; Gopka, V.; Jeong, K. S.; Alimgazinova, N. The Possible Signs of Accretion from Interstellar Medium in the Atmospheres of G-K-Type Disk and Halo Stars. Preprints2024, 2024101548. https://doi.org/10.20944/preprints202410.1548.v1
Yushchenko, A.; Andrievsky, S.; Demessinova, A.; Jeong, Y.; Yushchenko, V.; Doikov, D.; Gopka, V.; Jeong, K. S.; Alimgazinova, N. The Possible Signs of Accretion from Interstellar Medium in the Atmospheres of G-K-Type Disk and Halo Stars. Preprints 2024, 2024101548. https://doi.org/10.20944/preprints202410.1548.v1
Yushchenko, A.; Andrievsky, S.; Demessinova, A.; Jeong, Y.; Yushchenko, V.; Doikov, D.; Gopka, V.; Jeong, K. S.; Alimgazinova, N. The Possible Signs of Accretion from Interstellar Medium in the Atmospheres of G-K-Type Disk and Halo Stars. Preprints2024, 2024101548. https://doi.org/10.20944/preprints202410.1548.v1
APA Style
Yushchenko, A., Andrievsky, S., Demessinova, A., Jeong, Y., Yushchenko, V., Doikov, D., Gopka, V., Jeong, K. S., & Alimgazinova, N. (2024). The Possible Signs of Accretion from Interstellar Medium in the Atmospheres of G-K-Type Disk and Halo Stars. Preprints. https://doi.org/10.20944/preprints202410.1548.v1
Chicago/Turabian Style
Yushchenko, A., Kyung Sook Jeong and Nazgul Alimgazinova. 2024 "The Possible Signs of Accretion from Interstellar Medium in the Atmospheres of G-K-Type Disk and Halo Stars" Preprints. https://doi.org/10.20944/preprints202410.1548.v1
Abstract
The relationships between the relative abundances of chemical elements
and their second ionization potentials, as well as their condensation
temperatures, were analyzed using four published homogeneous abundance
surveys of halo and thin disk stars.
We selected 932 stars with effective
temperatures ranging from 4900 K to 5900 K and used the abundances of
10 chemical elements common across all surveys: Mg, Si, Ca, Sc, Ti, V,
Cr, Mn, Fe, and Ni. The correlation coefficients between the relative
abundances of these elements and their second ionization potentials
and condensation temperatures were investigated in relation to
metallicity and the stars' location in the Galaxy.
The observed
correlations may result from certain physical processes, such as the
accretion of interstellar gas onto stellar atmospheres. We also
analyzed the dependencies of relative abundances on second ionization
potentials based on published abundance patterns in five halo stars.
Evidence of charge-exchange reactions in the atmospheres of these
stars was found.
For more accurate determination of stellar ages from
the abundance ratios of radioactive and stable chemical elements in
stellar atmospheres, processes such as charge-exchange reactions and
dust-gas separation should be considered in future detailed
investigations. Additionally, changes in the chemical abundances in
the atmospheres of halo stars after crossing the Galactic plane were
found to be possible.
Keywords
stars; abundances – stars; circumstellar matter – stars; atmospheres – stars; Population I 16 – stars; Population II – physical data and processes: accretion
Subject
Physical Sciences, Astronomy and Astrophysics
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
