Radial velocity variability fractions of different types of hot subdwarf stars
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866912160770162688 |
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| author | He, Ruijie Meng, Xiangcun Lei, Zhenxin Yan, Huahui Lan, Shunyi |
| author_facet | He, Ruijie Meng, Xiangcun Lei, Zhenxin Yan, Huahui Lan, Shunyi |
| contents | Different types of hot subdwarfs may have different origins, which will cause them to present different radial velocity (RV) variability properties. Only 6$\pm$4% of our single-lined He-rich hot subdwarfs that only show spectroscopic features of hot subdwarfs are found to be RV variable, which is lower than the fraction of single-lined He-poor sdB stars (31$\pm$3%). Single-lined sdB stars with effective temperatures ($T_{\rm eff}$) $\sim$ 25,000 $-$ 33,000 K show an RV-variability fraction of 34$\pm$5%, while lower RV-variability fractions are observed for single-lined sdB stars cooler than about 25,000 K (11$\pm$4%), single-lined sdB/OB stars with $T_{\rm eff}$ $\sim$ 33,000 $-$ 40,000 K and surface gravities about 5.7 $-$ 6.0 (13$\pm$3%), as well as single-lined sdO/B stars with $T_{\rm eff}$ $\sim$ 45,000 $-$ 70,000 K (10$\pm$7%). Single-lined hot subdwarfs with $T_{\rm eff}$ $\sim$ 35,000 $-$ 45,000 K located above the extreme horizontal branch (EHB) show a similar RV-variability fraction of 34$\pm$9% as single-lined sdB stars at about 25,000 $-$ 33,000 K. The largest RV-variability fraction of 51$\pm$8% is found in single-lined hot subdwarfs below the canonical EHB. The detected RV-variability fraction of our composite hot subdwarfs with an infrared excess in their spectral energy distributions is 9$\pm$3%, which is lower than that fraction of single-lined hot subdwarfs. Since the average RV uncertainty we measured in the LAMOST spectra is about 7.0 km/s, the lower detected RV-variability fraction for composite hot subdwarfs is expected because the RV amplitudes associated with long-period systems are lower. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_13963 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Radial velocity variability fractions of different types of hot subdwarf stars He, Ruijie Meng, Xiangcun Lei, Zhenxin Yan, Huahui Lan, Shunyi Solar and Stellar Astrophysics Different types of hot subdwarfs may have different origins, which will cause them to present different radial velocity (RV) variability properties. Only 6$\pm$4% of our single-lined He-rich hot subdwarfs that only show spectroscopic features of hot subdwarfs are found to be RV variable, which is lower than the fraction of single-lined He-poor sdB stars (31$\pm$3%). Single-lined sdB stars with effective temperatures ($T_{\rm eff}$) $\sim$ 25,000 $-$ 33,000 K show an RV-variability fraction of 34$\pm$5%, while lower RV-variability fractions are observed for single-lined sdB stars cooler than about 25,000 K (11$\pm$4%), single-lined sdB/OB stars with $T_{\rm eff}$ $\sim$ 33,000 $-$ 40,000 K and surface gravities about 5.7 $-$ 6.0 (13$\pm$3%), as well as single-lined sdO/B stars with $T_{\rm eff}$ $\sim$ 45,000 $-$ 70,000 K (10$\pm$7%). Single-lined hot subdwarfs with $T_{\rm eff}$ $\sim$ 35,000 $-$ 45,000 K located above the extreme horizontal branch (EHB) show a similar RV-variability fraction of 34$\pm$9% as single-lined sdB stars at about 25,000 $-$ 33,000 K. The largest RV-variability fraction of 51$\pm$8% is found in single-lined hot subdwarfs below the canonical EHB. The detected RV-variability fraction of our composite hot subdwarfs with an infrared excess in their spectral energy distributions is 9$\pm$3%, which is lower than that fraction of single-lined hot subdwarfs. Since the average RV uncertainty we measured in the LAMOST spectra is about 7.0 km/s, the lower detected RV-variability fraction for composite hot subdwarfs is expected because the RV amplitudes associated with long-period systems are lower. |
| title | Radial velocity variability fractions of different types of hot subdwarf stars |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2412.13963 |