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| Main Authors: | , , , , , |
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| Format: | Preprint |
| Published: |
2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2507.19954 |
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| _version_ | 1866912502831382528 |
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| author | Koenigsberger, G. Schmutz, W. Pilachowski, C. Mejia-Nava, A. R. Sikorski, D. Cordero, M. |
| author_facet | Koenigsberger, G. Schmutz, W. Pilachowski, C. Mejia-Nava, A. R. Sikorski, D. Cordero, M. |
| contents | We determine the surface lithium abundance of the eclipsing binary components in V 505 Per (HIP 10961), A(Li)=2.65+/-0.07 and 2.35+/-0.1, which supports the rather unexpected conclusion that their surface Li abundances differ. We find effective temperatures 6600 K + 6550 K (~150 K higher than previously reported), which place the stars at the hot limit of the Lithium Dip, thus aleviating the previously suggested discrepancy with cluster stars of similar ages and temperatures. These temperatures are also more consistent with the system's Gaia spectral energy distribution. Our iron abundances, [Fe/H]=-0.15+\-0.07 and -0.25+\-0.1, agree with predictions of the higher temperatures deduced from our spectra and from evolutionary tracks. The surface rotation rate implied by our line profiles, 12.5+\-1 km/s, is smaller than the synchronous rotation rate, a curious result given the circular orbit and the age of the system. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_19954 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Lithium in V505 Per Koenigsberger, G. Schmutz, W. Pilachowski, C. Mejia-Nava, A. R. Sikorski, D. Cordero, M. Solar and Stellar Astrophysics We determine the surface lithium abundance of the eclipsing binary components in V 505 Per (HIP 10961), A(Li)=2.65+/-0.07 and 2.35+/-0.1, which supports the rather unexpected conclusion that their surface Li abundances differ. We find effective temperatures 6600 K + 6550 K (~150 K higher than previously reported), which place the stars at the hot limit of the Lithium Dip, thus aleviating the previously suggested discrepancy with cluster stars of similar ages and temperatures. These temperatures are also more consistent with the system's Gaia spectral energy distribution. Our iron abundances, [Fe/H]=-0.15+\-0.07 and -0.25+\-0.1, agree with predictions of the higher temperatures deduced from our spectra and from evolutionary tracks. The surface rotation rate implied by our line profiles, 12.5+\-1 km/s, is smaller than the synchronous rotation rate, a curious result given the circular orbit and the age of the system. |
| title | Lithium in V505 Per |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.19954 |