Exoplanets & Exomoons

Revisiting Planetary Systems in Okayama Planet Search Program: A New Long-period planet, RV Astrometry Joint Analysis, And Multiplicity-metallicity Trend Around Evolved Stars

By Keith Cowing
Status Report
astro-ph.EP
August 11, 2023
Filed under , , , , , , , , , , , , , , , , ,
Revisiting Planetary Systems in Okayama Planet Search Program: A New Long-period planet, RV Astrometry Joint Analysis, And Multiplicity-metallicity Trend Around Evolved Stars
HR diagram of the 32 OPSP planet-harboring stars in this study. The stars included in Takeda et al. (2008) are marked by circles, while other stars are marked by squares. The colored lines represent evolutionary tracks for solar-metallicity stars of masses between 1.0 M⊙ and 3.0 M⊙. — astro-ph.EP

In this study, we revisit 32 planetary systems around evolved stars observed within the framework of the Okayama Planet Search Program and its collaborative framework of the EAPS-Net to search for additional companions and investigate the properties of stars and giant planets in multiple-planet systems.

With our latest radial velocities obtained from Okayama Astrophysical Observatory (OAO), we confirm an additional giant planet in the wide orbit of 75 Cet system (Pc=2051.62+45.98−40.47 d, Mcsini=0.912+0.088−0.090 MJ, and ac=3.929+0.052−0.058 au), along with five stars exhibiting long-term radial velocity accelerations, which indicates massive companions in the wide orbits. We have also found that the radial velocity variations of several planet-harboring stars may indicate additional planet candidates, stellar activities, or other understudied sources. These stars include ϵ Tau, 11 Com, 24 Boo, 41 Lyn, 14 And, HD 32518, and ω Ser.

We further constrain the orbital configuration of the HD 5608, HD 14067, HD 120084, and HD 175679 systems by combining radial velocities with astrometry, as their host central stars exhibit significant astrometric accelerations. For other systems, we simply refine their orbital parameters. Moreover, our study indicates that the OPSP planet-harboring stars are more metal-poor compared to the currently known planet-harboring stars, and this is likely due to the B−V color upper limit at 1.0 for star selection in the beginning of the survey.

Finally, by investigating the less-massive giant planets (<5MJ) around currently known planet-harboring evolved stars, we have found that metallicity positively correlates with the multiplicity and total planet mass of the system, which can be evidence for the core-accretion planet formation model.

Huan-Yu Teng, Bun’ei Sato, Masayuki Kuzuhara, Takuya Takarada, Masashi Omiya, Hiroki Harakawa, Hideyuki Izumiura, Eiji Kambe, Mesut Yilmaz, Ilfan Bikmaev, Selim O. Selam, Timothy D. Brandt, Guang-Yao Xiao, Michitoshi Yoshida, Yoichi Itoh, Hiroyasu Ando, Eiichiro Kokubo, Shigeru Ida

Comments: 49 figures, 4 tables, accepted by PASJ, RV data will be available online as supplementary after the publication
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2308.05343 [astro-ph.EP] (or arXiv:2308.05343v1 [astro-ph.EP] for this version)
Submission history
From: Huan-Yu Teng
[v1] Thu, 10 Aug 2023 05:12:59 UTC (6,749 KB)
https://arxiv.org/abs/2308.05343
Astrobiology,

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻