Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Blanchet, Luc; Hébrard, G.; Larrouturou, François

doi:10.1051/0004-6361/201935705

Cited by 19 publications

(10 citation statements)

References 35 publications

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“…Final outlook -We expect to open up a new field aimed towards probing fundamental physics from astrometric data for minor planets in the inner and outer Solar System. More generally, alongside seminal works [66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82][83][84][85], we have only just begun exploring the full potential of connections between microscopic new physics and macroscopic planetary observations, from near (NEOs) to far (exoplanets) celestial objects.…”

Section: Etno Tno Jt H M Neomentioning

confidence: 99%

“…In this Letter, we provide the first proof-of-principle study using asteroid precessions and astrometric data to probe new ultralight particles. Previously, planets, exoplanets, and Kuiper Belt Objects (KBOs) were used to test GR and/or search for dark sector particles [66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82][83][84][85], yet the potential of probing new physics using asteroids remains mostly unharvested. Thanks to advances in radar and optical astrometry, the motion of asteroids, especially those classified as Near-Earth Objects (NEOs), is tracked much more precisely than KBOs and exoplanets.…”

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confidence: 99%

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Asteroid astrometry as a fifth-force and ultralight dark sector probe

Tsai¹,

Wu²,

Vagnozzi³

et al. 2021

Preprint

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We study for the first time the possibility of probing long-range fifth forces utilizing asteroid astrometric data, via the fifth force-induced orbital precession. We examine nine Near-Earth Object (NEO) asteroids whose orbital trajectories are accurately determined via optical and radar astrometry. Focusing on a Yukawa-type potential mediated by a new gauge field (dark photon) or a baryon-coupled scalar, we estimate the sensitivity reach for the fifth-force coupling strength and mediator mass in the mass range m 10 −21 − 10 −15 eV. Our estimated sensitivity is comparable to leading limits from torsion balance experiments, potentially exceeding these in a specific mass range. The fifth forced-induced precession increases with the orbital semi-major axis in the small m limit, motivating the study of objects further away from the Sun. We discuss future exciting prospects for extending our study to more than a million asteroids (including NEOs, main-belt asteroids, Hildas, and Jupiter Trojans), as well as trans-Neptunian objects and exoplanets.

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Section: Etno Tno Jt H M Neomentioning

confidence: 99%

mentioning

confidence: 99%

Asteroid astrometry as a fifth-force and ultralight dark sector probe

Tsai¹,

Wu²,

Vagnozzi³

et al. 2021

Preprint

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\dot{ω}

for HD 80606 b could be easily measured.…”

Section: Orbital Precessionmentioning

confidence: 99%

The HD 217107 planetary system: Twenty years of radial velocity measurements

et al. 2020

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The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence of a longer‐period companion, HD 217107 c. Interestingly, both the short‐period planet (Pb ∼ 7.13 d) and long‐period planet (Pc ∼ 5059 d) have significantly eccentric orbits (eb ∼ 0.13 and ec ∼ 0.40). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities. We confirm and refine the previously reported orbit of the long‐period companion. HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting the precession of the planetary orbit due to general relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, ω, is predicted to change at the level of ∼0.8∘ century−1. Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be ω˙<65.9∘ century−1. We discuss the limitations of detecting the subtle effects of precession in exoplanet orbits using RV data.

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“…Transit observations, with their sharp features that can be precisely timed, may provide a better opportunity for measuring orbital precession in exoplanet systems. For example, Blanchet, HÃľbrard, & Larrouturou (2019) proposed that, given future transit data TABLE 3 HD 217107 System Best-fit Orbital and Derived Parameters. The Maximum Likelihood values are given for each instrument's RV "jitter" term since we define those to be >0, and the posteriors are therefore non-Gaussian.…”

Section: Orbital Precessionmentioning

confidence: 99%

The HD 217107 Planetary System: Twenty Years of Radial Velocity Measurements

Giovinazzi,

Blake,

Eastman

et al. 2020

Preprint

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The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence for a longer-period companion, HD 217107 c. Interestingly, both the short-period planet ( b ∼ 7.13 d) and long-period planet ( c ∼ 5059 d) have significantly eccentric orbits ( b ∼ 0.13 and c ∼ 0.40). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities.We confirm and refine the previously reported orbit of the long-period companion.HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting precession of the planetary orbit due to General Relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, , is predicted to change at the level of ∼0.8 • century −1 . Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be ̇ < 65.9 • century −1 . We discuss the limitations of detecting the subtle effects of precession in exoplanet orbits using RV data.

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Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Cited by 19 publications

References 35 publications

Asteroid astrometry as a fifth-force and ultralight dark sector probe

Asteroid astrometry as a fifth-force and ultralight dark sector probe

The HD 217107 planetary system: Twenty years of radial velocity measurements

The HD 217107 Planetary System: Twenty Years of Radial Velocity Measurements

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