Gespeichert in:
| 1. Verfasser: | |
|---|---|
| Format: | Preprint |
| Veröffentlicht: |
2025
|
| Schlagworte: | |
| Online-Zugang: | https://arxiv.org/abs/2509.20047 |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| _version_ | 1866918147247833088 |
|---|---|
| author | Takeda, Yoichi |
| author_facet | Takeda, Yoichi |
| contents | A spectroscopic study was carried out for the double-line A-type eclipsing binary system RR Lyn A+B based on the disentangled spectra, with an aim of clarifying the differences in photospheric chemical compositions between the components, where T_eff (effective temperature) and v_t (microturbulence) were determined from Fe lines. The resulting abundances of 30 elements revealed the following characteristics. (1) The brighter/hotter A shows metal-rich trends of classical Am stars; i.e., heavier elements generally show overabundances tending to increase towards higher Z (atomic number) with exceptionally large deficit of Sc, while light elements such as CNO show underabundances. (2) Meanwhile, the abundances of fainter/cooler B are closer to the solar composition ([X/H]~0 for intermediate Z elements such as Fe group) though [X/H] does exhibit a slightly increasing tendency with Z, which suggests that B is a kind of marginal Am star with almost normal metallicity. This consequence is in contrast to the results of previous studies, which reported B to be of metal-deficient nature similar to lambda Boo stars. Such distinctions of chemical abundances between A and B may serve as a key to understanding the condition for the emergence of Am phenomenon. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_20047 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Atmospheric parameters and chemical abundances of the A-type eclipsing binary system RR Lyncis A and B Takeda, Yoichi Solar and Stellar Astrophysics A spectroscopic study was carried out for the double-line A-type eclipsing binary system RR Lyn A+B based on the disentangled spectra, with an aim of clarifying the differences in photospheric chemical compositions between the components, where T_eff (effective temperature) and v_t (microturbulence) were determined from Fe lines. The resulting abundances of 30 elements revealed the following characteristics. (1) The brighter/hotter A shows metal-rich trends of classical Am stars; i.e., heavier elements generally show overabundances tending to increase towards higher Z (atomic number) with exceptionally large deficit of Sc, while light elements such as CNO show underabundances. (2) Meanwhile, the abundances of fainter/cooler B are closer to the solar composition ([X/H]~0 for intermediate Z elements such as Fe group) though [X/H] does exhibit a slightly increasing tendency with Z, which suggests that B is a kind of marginal Am star with almost normal metallicity. This consequence is in contrast to the results of previous studies, which reported B to be of metal-deficient nature similar to lambda Boo stars. Such distinctions of chemical abundances between A and B may serve as a key to understanding the condition for the emergence of Am phenomenon. |
| title | Atmospheric parameters and chemical abundances of the A-type eclipsing binary system RR Lyncis A and B |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2509.20047 |