Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
We present the discovery of a Jupiter-like planet, HD 73344 d ( ${m}_{d}=2.5{5}_{-0.46}^{+0.56}\,{M}_{J}$ , ${a}_{d}=6.7{0}_{-0.26}^{+0.25}$ au, ${e}_{d}=0.1{8}_{-0.12}^{+0.14}$ ) based on 27 yr radial velocity (RV) observations from ELODIE, Lick/Hamilton, SOPHIE, APF, and HIRES. HD 73344 also hosts...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-3881/ada60a |
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| author | Jingwen Zhang Lauren M. Weiss Daniel Huber Jerry W. Xuan Michael Bottom Benjamin J. Fulton Howard Isaacson Mason G. MacDougall Nicholas Saunders |
| author_facet | Jingwen Zhang Lauren M. Weiss Daniel Huber Jerry W. Xuan Michael Bottom Benjamin J. Fulton Howard Isaacson Mason G. MacDougall Nicholas Saunders |
| author_sort | Jingwen Zhang |
| collection | DOAJ |
| description | We present the discovery of a Jupiter-like planet, HD 73344 d ( ${m}_{d}=2.5{5}_{-0.46}^{+0.56}\,{M}_{J}$ , ${a}_{d}=6.7{0}_{-0.26}^{+0.25}$ au, ${e}_{d}=0.1{8}_{-0.12}^{+0.14}$ ) based on 27 yr radial velocity (RV) observations from ELODIE, Lick/Hamilton, SOPHIE, APF, and HIRES. HD 73344 also hosts a compact inner planetary system, including a transiting sub-Neptune, HD 73344 b ( P _b = 15.61 days, ${r}_{b}=2.8{8}_{-0.07}^{+0.08}\,{R}_{\oplus }$ ), and a nontransiting Saturn-mass planet ( P _c = 65.936 days, ${m}_{c}\,\sin \,{i}_{c}=0.36{7}_{-0.021}^{+0.022}\,{M}_{{\rm{J}}}$ ). By analyzing TESS light curves, we identified a stellar rotation period of 9.03 ± 1.3 days. Combining this with $v\,\sin \,{i}_{* }$ measurements from stellar spectra, we derived a stellar inclination of $63.{{6}^{\circ }}_{-16.5}^{+17.4}$ . Furthermore, by combining RVs and Hipparcos–Gaia astrometric acceleration, we characterized the three-dimensional orbit of the outer giant planet and constrained its mutual inclination relative to the innermost transiting planet to be 46° < Δ I _bd < 134° (1 σ ) and 20° < Δ I _bd < 160° (2 σ ), strongly disfavoring coplanar architectures. Our analytical calculations and N -body simulations reveal that the two inner planets are strongly coupled with each other and undergo nodal precession together around the orbital axis of the giant planet. During nodal precession, the orbital inclinations of inner planets oscillate with time and therefore become misaligned relative to the stellar spin axis. The formation of such systems suggests a history of planet–planet scattering or misalignment between the inner and outer components of protoplanetary disks. The upcoming release of Gaia Data Release 4 will uncover more systems similar to HD 73344, and enable the study of the flatness of exoplanet systems with a mixture of inner and outer planetary systems on a statistical level. |
| format | Article |
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| publishDate | 2025-01-01 |
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| spelling | doaj-art-9ecc467b70114960aa95dd50104419e12025-08-20T02:48:13ZengIOP PublishingThe Astronomical Journal1538-38812025-01-01169420010.3847/1538-3881/ada60aDiscovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344Jingwen Zhang0https://orcid.org/0000-0002-2696-2406Lauren M. Weiss1https://orcid.org/0000-0002-3725-3058Daniel Huber2https://orcid.org/0000-0001-8832-4488Jerry W. Xuan3https://orcid.org/0000-0002-6618-1137Michael Bottom4https://orcid.org/0000-0003-1341-5531Benjamin J. Fulton5https://orcid.org/0000-0003-3504-5316Howard Isaacson6https://orcid.org/0000-0002-0531-1073Mason G. MacDougall7https://orcid.org/0000-0003-2562-9043Nicholas Saunders8https://orcid.org/0000-0003-2657-3889Institute for Astronomy, University of Hawaii at Mānoa , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; jingwen7@hawaii.eduDepartment of Physics and Astronomy, University of Notre Dame , Notre Dame, IN 46556, USAInstitute for Astronomy, University of Hawaii at Mānoa , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; jingwen7@hawaii.edu; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney , Sydney, NSW 2006, AustraliaDepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USAInstitute for Astronomy, University of Hawaii at Mānoa , 640 N. Aohoku Place, Hilo, HI 96720, USANASA Exoplanet Science Institute/Caltech-IPAC , California Institute of Technology, Pasadena, CA 91125, USADepartment of Astronomy, University of California, Berkeley , 501 Campbell Hall, Berkeley, CA 94720, USADepartment of Physics & Astronomy, University of California, Los Angeles , Los Angeles, CA 90095, USAInstitute for Astronomy, University of Hawaii at Mānoa , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; jingwen7@hawaii.eduWe present the discovery of a Jupiter-like planet, HD 73344 d ( ${m}_{d}=2.5{5}_{-0.46}^{+0.56}\,{M}_{J}$ , ${a}_{d}=6.7{0}_{-0.26}^{+0.25}$ au, ${e}_{d}=0.1{8}_{-0.12}^{+0.14}$ ) based on 27 yr radial velocity (RV) observations from ELODIE, Lick/Hamilton, SOPHIE, APF, and HIRES. HD 73344 also hosts a compact inner planetary system, including a transiting sub-Neptune, HD 73344 b ( P _b = 15.61 days, ${r}_{b}=2.8{8}_{-0.07}^{+0.08}\,{R}_{\oplus }$ ), and a nontransiting Saturn-mass planet ( P _c = 65.936 days, ${m}_{c}\,\sin \,{i}_{c}=0.36{7}_{-0.021}^{+0.022}\,{M}_{{\rm{J}}}$ ). By analyzing TESS light curves, we identified a stellar rotation period of 9.03 ± 1.3 days. Combining this with $v\,\sin \,{i}_{* }$ measurements from stellar spectra, we derived a stellar inclination of $63.{{6}^{\circ }}_{-16.5}^{+17.4}$ . Furthermore, by combining RVs and Hipparcos–Gaia astrometric acceleration, we characterized the three-dimensional orbit of the outer giant planet and constrained its mutual inclination relative to the innermost transiting planet to be 46° < Δ I _bd < 134° (1 σ ) and 20° < Δ I _bd < 160° (2 σ ), strongly disfavoring coplanar architectures. Our analytical calculations and N -body simulations reveal that the two inner planets are strongly coupled with each other and undergo nodal precession together around the orbital axis of the giant planet. During nodal precession, the orbital inclinations of inner planets oscillate with time and therefore become misaligned relative to the stellar spin axis. The formation of such systems suggests a history of planet–planet scattering or misalignment between the inner and outer components of protoplanetary disks. The upcoming release of Gaia Data Release 4 will uncover more systems similar to HD 73344, and enable the study of the flatness of exoplanet systems with a mixture of inner and outer planetary systems on a statistical level.https://doi.org/10.3847/1538-3881/ada60aExtrasolar gaseous giant planetsRadial velocityGaiaSpace astrometryExoplanet dynamics |
| spellingShingle | Jingwen Zhang Lauren M. Weiss Daniel Huber Jerry W. Xuan Michael Bottom Benjamin J. Fulton Howard Isaacson Mason G. MacDougall Nicholas Saunders Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 The Astronomical Journal Extrasolar gaseous giant planets Radial velocity Gaia Space astrometry Exoplanet dynamics |
| title | Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 |
| title_full | Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 |
| title_fullStr | Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 |
| title_full_unstemmed | Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 |
| title_short | Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344 |
| title_sort | discovery of a jupiter analog misaligned to the inner planetary system in hd 73344 |
| topic | Extrasolar gaseous giant planets Radial velocity Gaia Space astrometry Exoplanet dynamics |
| url | https://doi.org/10.3847/1538-3881/ada60a |
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