HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit

Errico, Adriana; Wittenmyer, Robert A.; Horner, Jonathan; Li, Zhexing; Brandt, G. Mirek; Kane, Stephen R.; Fetherolf, Tara; Holt, Timothy R.; Carter, Brad; Clark, Jake T.; Butler, R. Paul; Tinney, C. G.; Ballard, Sarah; Bowler, Brendan P.; Kielkopf, John F.; Liu, Hui-Gen; Plavchan, Peter; Shporer, Avi; Zhang, Hui; Wright, D. E.; Addison, Brett C.; Mengel, M. W.; Okumura, Jack

doi:10.3847/1538-3881/ac6589

“…The constraints of the astrometric nondetection require HAT-P-2 c to have an edge-on orbital inclination (i c = 90°± 16°), as any other configuration would produce a detectable astrometric signal. This is comparable to the result of Errico et al (2022), who determined the true mass of the long-period planet HD 83443 c from an astrometric nondetection. HAT-P-2 c's orbital inclination is consistent with HAT-P-2 b, which in turn has a low projected obliquity from the host star's rotational axis (Winn et al 2007;Albrecht et al 2012).…”

Section: Hat-p-2 Csupporting

confidence: 86%

Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c

de Beurs,

de Wit,

Venner

et al. 2023

AJ

5

0

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One possible formation mechanism for Hot Jupiters is that high-eccentricity gas giants experience tidal interactions with their host star that cause them to lose orbital energy and migrate inwards. We study these types of tidal interactions in an eccentric Hot Jupiter called HAT-P-2 b, which is a system where a long-period companion has been suggested and hints of orbital evolution were detected. Using 5 additional years of radial velocity (RV) measurements, we further investigate these phenomena. We investigated the long-period companion by jointly fitting RVs and Hipparcos-Gaia astrometry and confirmed this long-period companion, significantly narrowed down the range of possible periods ( P 2 = 8500 − 1500 + 2600 days), and determined that it must be a substellar object ( 10.7 − 2.2 + 5.2 M j). We also developed a modular pipeline to simultaneously model rapid orbital evolution and the long-period companion. We find that the rate and significance of evolution are highly dependent on the long-period companion modeling choices. In some cases the orbital rates of change reached de / dt = 3.28 − 1.72 + 1.75 × 10 − 3 yr−1, d ω/dt = 1.12° ± 0.22° yr−1, which corresponds to a ∼321 yr apsidal precession period. In other cases, the data is consistent with de/dt = 7.67 ± 18.6 × 10−4 yr−1, d ω/dt = 0.76° ± 0.24° yr−1. The most rapid changes found are significantly larger than the expected relativistic precession rate and could be caused by transient tidal planet–star interactions. To definitively determine the magnitude and significance of potential orbital evolution in HAT-P-2 b, we recommend further monitoring with RVs and precise transit and eclipse timings.

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“…In this way it is possible to remove the intrinsic uncertainty in the mass of the companion discovered by the radial velocity (RV) method, and determine its true mass rather than a minimum value. Recent, notable applications of this approach include: a) a preliminary astrometric mass for the super-Earth candidate orbiting at 1.5 au from the nearest star to the Sun, the M dwarf Proxima Centauri [33], which had been uncovered based on long-term RV time-series analysis [34]; b) true mass determinations for the long-period (5 ≤ P ≤ 20 yr) super-Jupiters (1.5 ≤ M p ≤ 10 M Jup ) 14 Her b [35] and HD 83443 c [36], orbiting solar-mass primaries.…”

Section: Dynamical Mass Measurementsmentioning

confidence: 99%

Gaia astrometry and exoplanetary science: DR2, (E)DR3, and beyond

Sozzetti¹

2024

Comptes Rendus. Physique

1

0

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I review the recent impact of Gaia astrometry in the exoplanet field, both in terms of characterization of the orbits and masses of planetary systems and the properties of their host stars. I then discuss the newly published results in the third major data release (DR3), that begin to tackle exoplanetary science based on Gaia data alone. I conclude with a perspective look at the expectations for major contributions to our understanding of exoplanet demographics from future Gaia data releases.Résumé. Je passe en revue l'impact récent de l'astrométrie fournie par la mission spatiale Gaia dans le domaine des exoplanètes, tant en termes de caractérisation des orbites et des masses des systèmes planétaires que des propriétés de leurs étoiles hôtes. Je discute ensuite des résultats récemment publiés dans la troisième livraison majeure des données (DR3), qui commencent à aborder la science des exoplanètes sur la base des seules données de Gaia. Je conclus par un regard prospectif sur les contributions majeures à notre compréhension de la démographie des exoplanètes, attendues à partir des futures publications de données Gaia.

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“…By comparing data from HIPPARCOS with the second data release from Gaia, Brandt (2018; which has since been updated to the Gaia Early Data Release 3, EDR3; see Brandt 2021) and Kervella et al (2019) have both separately released catalogs of stars exhibiting astrometric accelerations. These catalogs have been used for follow-up to efficiently find new brown dwarfs (Bowler et al 2021;Bonavita et al 2022;Kuzuhara et al 2022) and exoplanets (Errico et al 2022) and to dynamically characterize previously known systems (Brandt et al 2021;Feng et al 2021;Li et al 2021;Steiger et al 2021;Zeng et al 2021;Biller et al 2022;Dupuy et al 2022;Franson et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Weighing the Darkness. III. How Gaia Could, but Probably Will Not, Astrometrically Detect Free-floating Black Holes

Andrews

¹

2023

ApJ

2

0

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The gravitational pull of an unseen companion to a luminous star is well known to cause deviations to the parallax and proper motion of a star. In a previous paper in this series, we argue that the astrometric mission Gaia can identify long-period binaries by precisely measuring these arcs. An arc in a star’s path can also be caused by a flyby: a hyperbolic encounter with another massive object. We quantify the apparent acceleration over time induced by a companion star as a function of the impact parameter, velocity of interaction, and companion mass. In principle, Gaia could be used to astrometrically identify the contribution of massive compact halo objects to the local dark matter potential of the Milky Way. However, after quantifying their rate and Gaia’s sensitivity, we find that flybys are so rare that Gaia will probably never observe one. Therefore, every star in the Gaia database exhibiting astrometric acceleration is likely in a long-period binary with another object. Nevertheless, we show how intermediate-mass black holes, if they exist in the local stellar neighborhood, can induce anomalously large accelerations on stars.

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HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit

Cited by 6 publications

References 141 publications

Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c

Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c

Gaia astrometry and exoplanetary science: DR2, (E)DR3, and beyond

Weighing the Darkness. III. How Gaia Could, but Probably Will Not, Astrometrically Detect Free-floating Black Holes

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