Unraveling Year-Long Radial Velocity Variations in Red Clump Region -- I: Comprehensive analysis of a K0 Giant star, 2 Draconis
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2026
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| author | Srisuchinwong, Udomlerd Zhou, Jianzhao Teng, Huan-Yu Xiao, Guang-Yao Sato, Bun'ei Takarada, Takuya Omiya, Masashi Harakawa, Hiroki Kambe, Eiji Izumiura, Hideyuki Yoshida, Michitoshi Itoh, Yoichi Ando, Hiroyasu Kokubo, Eiichiro Hon, Marc Liu, Yujuan Zhao, Fei Wang, Wei Zhai, Meng Bi, Shaolan Zhao, Gang |
| author_facet | Srisuchinwong, Udomlerd Zhou, Jianzhao Teng, Huan-Yu Xiao, Guang-Yao Sato, Bun'ei Takarada, Takuya Omiya, Masashi Harakawa, Hiroki Kambe, Eiji Izumiura, Hideyuki Yoshida, Michitoshi Itoh, Yoichi Ando, Hiroyasu Kokubo, Eiichiro Hon, Marc Liu, Yujuan Zhao, Fei Wang, Wei Zhai, Meng Bi, Shaolan Zhao, Gang |
| contents | Slow-rotating evolved stars frequently exhibit radial velocity (RV) variations on annual timescales, complicated by instrumental systematics and aliasing in the one-year regime. Here we investigate the origin of the near-yearly periodicity in 2 Dra, a star located in the red-clump region, assessing possible causes between stellar activity, instrumental profile (IP) effects, sampling alias, and planetary companions. We applied two independent approaches: (1) constraining diagnostic signals and performing a correlation analysis ($r$) between period-confined signals, and (2) evaluating phase stability by partitioning Keplerian fits. These methods enabled us to examine the physical connections and phase coherence among stellar activity indicators, RV measurements, and IP diagnostics. Our analysis suggests a stellar rotation period of $\simeq270\text{--}320$\,d for 2~Dra. The 340-d RV signal does not appear to originate from stellar activity in this chromospherically quiet star ($|r| \lesssim 0.33$), nor from instrumental systematics near the annual period ($|r| \lesssim 0.1$). This conclusion is supported by contrasting phase behavior: the RV and stellar activity phases remain stable, whereas the IP phases do not. We therefore propose that the 340-d variation likely arises from either small-amplitude intrinsic variability or a tentative gas giant companion with potential weak activity-induced modulation. The case of 2~Dra provides a framework for distinguishing the origins of $\sim$1-yr RV variations in other evolved stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_08164 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Unraveling Year-Long Radial Velocity Variations in Red Clump Region -- I: Comprehensive analysis of a K0 Giant star, 2 Draconis Srisuchinwong, Udomlerd Zhou, Jianzhao Teng, Huan-Yu Xiao, Guang-Yao Sato, Bun'ei Takarada, Takuya Omiya, Masashi Harakawa, Hiroki Kambe, Eiji Izumiura, Hideyuki Yoshida, Michitoshi Itoh, Yoichi Ando, Hiroyasu Kokubo, Eiichiro Hon, Marc Liu, Yujuan Zhao, Fei Wang, Wei Zhai, Meng Bi, Shaolan Zhao, Gang Solar and Stellar Astrophysics Earth and Planetary Astrophysics Slow-rotating evolved stars frequently exhibit radial velocity (RV) variations on annual timescales, complicated by instrumental systematics and aliasing in the one-year regime. Here we investigate the origin of the near-yearly periodicity in 2 Dra, a star located in the red-clump region, assessing possible causes between stellar activity, instrumental profile (IP) effects, sampling alias, and planetary companions. We applied two independent approaches: (1) constraining diagnostic signals and performing a correlation analysis ($r$) between period-confined signals, and (2) evaluating phase stability by partitioning Keplerian fits. These methods enabled us to examine the physical connections and phase coherence among stellar activity indicators, RV measurements, and IP diagnostics. Our analysis suggests a stellar rotation period of $\simeq270\text{--}320$\,d for 2~Dra. The 340-d RV signal does not appear to originate from stellar activity in this chromospherically quiet star ($|r| \lesssim 0.33$), nor from instrumental systematics near the annual period ($|r| \lesssim 0.1$). This conclusion is supported by contrasting phase behavior: the RV and stellar activity phases remain stable, whereas the IP phases do not. We therefore propose that the 340-d variation likely arises from either small-amplitude intrinsic variability or a tentative gas giant companion with potential weak activity-induced modulation. The case of 2~Dra provides a framework for distinguishing the origins of $\sim$1-yr RV variations in other evolved stars. |
| title | Unraveling Year-Long Radial Velocity Variations in Red Clump Region -- I: Comprehensive analysis of a K0 Giant star, 2 Draconis |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2601.08164 |