Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391
We present the discoveries of two giant plants orbiting the red-giant-branch star HD 112570 and the red-clump star HD 154391, based on the radial-velocity (RV) measurements from the Xinglong station and Okayama Astrophysical Observatory. Spectroscopic and asteroseismic analyses suggest that HD 11257...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad11de |
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| author | Guang-Yao Xiao Huan-Yu Teng Jianzhao Zhou Bun’ei Sato Yu-Juan Liu Shaolan Bi Takuya Takarada Masayuki Kuzuhara Marc Hon Liang Wang Masashi Omiya Hiroki Harakawa Fei Zhao Gang Zhao Eiji Kambe Hideyuki Izumiura Hiroyasu Ando Kunio Noguchi Wei Wang Meng Zhai Nan Song Chengqun Yang Tanda Li Timothy D. Brandt Michitoshi Yoshida Yoichi Itoh Eiichiro Kokubo |
| author_facet | Guang-Yao Xiao Huan-Yu Teng Jianzhao Zhou Bun’ei Sato Yu-Juan Liu Shaolan Bi Takuya Takarada Masayuki Kuzuhara Marc Hon Liang Wang Masashi Omiya Hiroki Harakawa Fei Zhao Gang Zhao Eiji Kambe Hideyuki Izumiura Hiroyasu Ando Kunio Noguchi Wei Wang Meng Zhai Nan Song Chengqun Yang Tanda Li Timothy D. Brandt Michitoshi Yoshida Yoichi Itoh Eiichiro Kokubo |
| author_sort | Guang-Yao Xiao |
| collection | DOAJ |
| description | We present the discoveries of two giant plants orbiting the red-giant-branch star HD 112570 and the red-clump star HD 154391, based on the radial-velocity (RV) measurements from the Xinglong station and Okayama Astrophysical Observatory. Spectroscopic and asteroseismic analyses suggest that HD 112570 has a mass of 1.15 ± 0.12 M _☉ , a radius of 9.85 ± 0.23 R _☉ , a metallicity [Fe/H] of −0.46 ± 0.1, and $\mathrm{log}\,g$ of 2.47 ± 0.1. With the joint analysis of RV and Hipparcos-Gaia astrometry, we obtain a dynamical mass of ${M}_{{\rm{p}}}={3.42}_{-0.84}^{+1.4}\ {M}_{\mathrm{Jup}}$ , a period of $P={2615}_{-77}^{+85}$ days, and a moderate eccentricity of $e={0.20}_{-0.14}^{+0.16}$ for the Jovian planet HD 112570 b. For HD 154391, it has a mass of 2.07 ± 0.03 M _☉ , a radius of 8.56 ± 0.05 R _☉ , a metallicity [Fe/H] of 0.07 ± 0.1, and $\mathrm{log}\,g$ of 2.86 ± 0.1. The super-Jupiter HD 154391 b has a mass of ${M}_{{\rm{p}}}={9.1}_{-1.9}^{+2.8}\ {M}_{\mathrm{Jup}}$ , a period of $P={5163}_{-57}^{+60}$ days, and an eccentricity of $e={0.20}_{-0.04}^{+0.04}$ . We found that HD 154391 b has one of the longest orbital periods among those ever discovered orbiting evolved stars, which may provide a valuable case in our understanding of planetary formation at wider orbits. Moreover, while a mass gap at 4 M _Jup seems to be present in the population of giant stars, there appear to be no significant differences in the distribution of metallicity among giant planets with masses above or below this threshold. Finally, the origin of the abnormal accumulation near 2 au for planets around large evolved stars ( R _⋆ > 21 R _☉ ), remains unclear. |
| first_indexed | 2024-03-08T14:28:51Z |
| format | Article |
| id | doaj.art-2fddf3752d464a048cb25d515ceb9460 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-08T14:28:51Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-2fddf3752d464a048cb25d515ceb94602024-01-12T13:37:04ZengIOP PublishingThe Astronomical Journal1538-38812024-01-0116725910.3847/1538-3881/ad11deTwo Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391Guang-Yao Xiao0https://orcid.org/0000-0001-6753-4611Huan-Yu Teng1https://orcid.org/0000-0003-3860-6297Jianzhao Zhou2https://orcid.org/0009-0004-9024-9666Bun’ei Sato3https://orcid.org/0000-0001-8033-5633Yu-Juan Liu4https://orcid.org/0009-0008-3430-1027Shaolan Bi5Takuya Takarada6Masayuki Kuzuhara7Marc Hon8https://orcid.org/0000-0003-2400-6960Liang Wang9Masashi Omiya10Hiroki Harakawa11https://orcid.org/0000-0002-7972-0216Fei Zhao12Gang Zhao13Eiji Kambe14Hideyuki Izumiura15Hiroyasu Ando16Kunio Noguchi17Wei Wang18https://orcid.org/0000-0002-9702-4441Meng Zhai19Nan Song20Chengqun Yang21Tanda Li22https://orcid.org/0000-0001-6396-2563Timothy D. Brandt23https://orcid.org/0000-0003-2630-8073Michitoshi Yoshida24https://orcid.org/0000-0002-9948-1646Yoichi Itoh25Eiichiro Kokubo26CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cn; Department of Earth and Planetary Sciences, School of Science, Tokyo Institute of Technology , 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of China; Department of Astronomy, Beijing Normal University , Beijing 100875, People's Republic of ChinaDepartment of Earth and Planetary Sciences, School of Science, Tokyo Institute of Technology , 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of China; Department of Astronomy, Beijing Normal University , Beijing 100875, People's Republic of ChinaAstrobiology Center, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanAstrobiology Center, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USANational Astronomical Observatories, Nanjing Institute of Astronomical Optics & Technology , Chinese Academy of Sciences, Nanjing 210042, People's Republic of China; CAS Key Laboratory of Astronomical Optics & Technology, Nanjing Institute of Astronomical Optics & Technology , Chinese Academy of Sciences, Nanjing 210042, People's Republic of ChinaAstrobiology Center, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 650 North A’ohoku Place, Hilo, HI 96720, USACAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 650 North A’ohoku Place, Hilo, HI 96720, USAOkayama Branch Office, Subaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences , Kamogata, Asakuchi, Okayama 719-0232, JapanNational Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China lyj@bao.ac.cnChina Science and Technology Museum , Beijing 100101, People's Republic of ChinaShanghai Astronomical Observatory , 80 Nandan Road, Shanghai 200030, People's Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of China; Department of Astronomy, Beijing Normal University , Beijing 100875, People's Republic of China; School of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, UKDepartment of Physics, University of California , Santa Barbara, Santa Barbara, CA 93106, USANational Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo , 407-2, Nishigaichi, Sayo, Hyogo 679-5313, JapanThe Graduate University for Advanced Studies (SOKENDAI) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanWe present the discoveries of two giant plants orbiting the red-giant-branch star HD 112570 and the red-clump star HD 154391, based on the radial-velocity (RV) measurements from the Xinglong station and Okayama Astrophysical Observatory. Spectroscopic and asteroseismic analyses suggest that HD 112570 has a mass of 1.15 ± 0.12 M _☉ , a radius of 9.85 ± 0.23 R _☉ , a metallicity [Fe/H] of −0.46 ± 0.1, and $\mathrm{log}\,g$ of 2.47 ± 0.1. With the joint analysis of RV and Hipparcos-Gaia astrometry, we obtain a dynamical mass of ${M}_{{\rm{p}}}={3.42}_{-0.84}^{+1.4}\ {M}_{\mathrm{Jup}}$ , a period of $P={2615}_{-77}^{+85}$ days, and a moderate eccentricity of $e={0.20}_{-0.14}^{+0.16}$ for the Jovian planet HD 112570 b. For HD 154391, it has a mass of 2.07 ± 0.03 M _☉ , a radius of 8.56 ± 0.05 R _☉ , a metallicity [Fe/H] of 0.07 ± 0.1, and $\mathrm{log}\,g$ of 2.86 ± 0.1. The super-Jupiter HD 154391 b has a mass of ${M}_{{\rm{p}}}={9.1}_{-1.9}^{+2.8}\ {M}_{\mathrm{Jup}}$ , a period of $P={5163}_{-57}^{+60}$ days, and an eccentricity of $e={0.20}_{-0.04}^{+0.04}$ . We found that HD 154391 b has one of the longest orbital periods among those ever discovered orbiting evolved stars, which may provide a valuable case in our understanding of planetary formation at wider orbits. Moreover, while a mass gap at 4 M _Jup seems to be present in the population of giant stars, there appear to be no significant differences in the distribution of metallicity among giant planets with masses above or below this threshold. Finally, the origin of the abnormal accumulation near 2 au for planets around large evolved stars ( R _⋆ > 21 R _☉ ), remains unclear.https://doi.org/10.3847/1538-3881/ad11deExoplanet astronomyEvolved starsRadial velocityPlanet formation |
| spellingShingle | Guang-Yao Xiao Huan-Yu Teng Jianzhao Zhou Bun’ei Sato Yu-Juan Liu Shaolan Bi Takuya Takarada Masayuki Kuzuhara Marc Hon Liang Wang Masashi Omiya Hiroki Harakawa Fei Zhao Gang Zhao Eiji Kambe Hideyuki Izumiura Hiroyasu Ando Kunio Noguchi Wei Wang Meng Zhai Nan Song Chengqun Yang Tanda Li Timothy D. Brandt Michitoshi Yoshida Yoichi Itoh Eiichiro Kokubo Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 The Astronomical Journal Exoplanet astronomy Evolved stars Radial velocity Planet formation |
| title | Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 |
| title_full | Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 |
| title_fullStr | Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 |
| title_full_unstemmed | Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 |
| title_short | Two Long-period Giant Planets around Two Giant Stars: HD 112570 and HD 154391 |
| title_sort | two long period giant planets around two giant stars hd 112570 and hd 154391 |
| topic | Exoplanet astronomy Evolved stars Radial velocity Planet formation |
| url | https://doi.org/10.3847/1538-3881/ad11de |
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