On the potentially dramatic history of the super-Earth ρ 55 Cancri e

Hansen, Bradley M. S.; Zink, Jon K.

doi:10.1093/mnras/stv916

Cited by 42 publications

(20 citation statements)

References 73 publications

(107 reference statements)

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“…In the first channel, planets form in the disk, and in some cases, angular momentum exchange between the planets and the protoplanetary disk can produce inward migration (e.g., Lin and Papaloizou 1986;Masset and Papaloizou 2003). In the second channel, planets also formed in the disk, but dynamical interactions between multiple planets or a stellar companion greatly affect the final orbital configuration of the system, through a variety of mechanisms such as planetplanet scattering (e.g., Rasio and Ford 1996a), EKL (see below), or secular chaos (Lithwick and Wu 2012;Hansen and Zink 2015). The role of planet or stellar dynamical interactions is motivated by the presence of substantial eccentricities amongst the more distant Jovian population, and the discovery of high obliquities (misalignments between planetary orbital and host star spin directions, e.g., Albrecht et al 2012b).…”

Section: Planetary Systemsmentioning

confidence: 99%

The Eccentric Kozai-Lidov Effect and Its Applications

Naoz

2016

Annu. Rev. Astron. Astrophys.

634

564

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The hierarchical triple body approximation has useful applications to a variety of systems from planetary and stellar scales to supermassive black holes. In this approximation, the energy of each orbit is separately conserved and therefore the two semi-major axes are constants. On timescales much larger than the orbital periods, the orbits exchange angular momentum which leads to eccentricity and orientation (i.e., inclination) oscillations. The orbits' eccentricity can reach extreme values leading to a nearly radial motion, which can further evolve into short orbit periods and merging binaries. Furthermore, the orbits' mutual inclination may change dramatically from pure prograde to pure retrograde leading to misalignment and a wide range of inclinations. This dynamical behavior is coined as the "eccentric Kozai-Lidov" mechanism. The behavior of such a system is exciting, rich and chaotic in nature. Furthermore, these dynamics are accessible from a large part of the triple body parameter space and can be applied to diverse range of astrophysical settings and used to gain insights to many puzzles.Comment: 60 pages 25 figures, to appear in Annual Review of Astronomy and Astrophysics, comments welcom

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Section: Planetary Systemsmentioning

confidence: 99%

The Eccentric Kozai-Lidov Effect and Its Applications

Naoz

2016

Annu. Rev. Astron. Astrophys.

634

564

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“…One clue about the formation history of 55 Cnc e is the fact that it transits whereas the outer planet (P∼4800 days) is claimed, on the basis of HST astrometry, to be inclined to the line of sight by 30 degrees (McArthur et al 2004). Hansen & Zink (2015) showed that if 55 Cnc e formed slightly beyond its current orbitand migrated inwards through tidal dissipation, it would have crossed a pair of secular resonances in the system, which could have boosted its inclination and/or eccentricity. This would increase the tidal heating and potentially devolatilize the planet or drive it to Roche lobe overflow.…”

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confidence: 99%

Mass Constraints of the Wasp-47 Planetary System From Radial Velocities

Sinukoff

Howard

Petigura

et al. 2017

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We report precise radial velocity (RV) measurements of WASP-47, a G star that hosts three transiting planets in close proximity (a hot Jupiter, a super-Earth, and a Neptune-sized planet) and a non-transiting planet at 1.4 au. Through a joint analysis of previously published RVs and our own Keck-HIRES RVs, we significantly improve the planet mass and bulk density measurements. For the super-Earth WASP-47e (P=0.79 days), we measure a mass of  9.11 1.17 M ⊕ , and a bulk density of  7.63 1.90 g cm −3 , consistent with a rocky composition. For the hot Jupiter WASP-47b (P=4.2 days), we measure a mass of  356 12 M ⊕ (1.12 ± 0.04 M Jup ) and constrain its eccentricity to <0.021 at 3σ confidence. For the Neptune-size planet WASP-47d (P=9.0 days), we measure a mass of  12.75 2.70 M ⊕ and a bulk density of  1.36 0.42 g cm −3 , suggesting that it has a thick H/He envelope. For the outer non-transiting planet, we measure a minimum mass of  411 18 M ⊕ (1.29 ± 0.06 M Jup ), an orbital period of  595.7 5.0days, and an orbital eccentricity of  0.27 0.04. Our new measurements are consistent with but two to four times more precise than previous mass measurements.

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“…Gravitational scattering due to overdensities caused by other planets in the vicinity (e.g. Hansen & Zink 2015).…”

Section: Limitations Of Our Modelmentioning

confidence: 99%

The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and H₂ Envelope’s Sizes

Modirrousta-Galian

Locci

Micela

2020

ApJ

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Several models have been introduced in order to explain the radius distribution in exoplanet radii observed by Fulton et al. (2017) with one peak at ∼ 1.3R ⊕ the other at ∼ 2.4R ⊕ and the minimum at ∼ 1.75R ⊕ . In this paper we focus on the hypothesis that the exoplanet size distribution is caused by stellar XUV-induced atmospheric loss. We evolve 10 6 synthetic exoplanets by exposing them to XUV irradiation from synthetic ZAMS stars. For each planet we set a different interior composition which ranged from 100 wt% Fe (very dense) through 100 wt% MgSiO 3 (average density) and to 100 wt% H 2 O ice (low density) with varying hydrogen envelop sizes which varied from 0 wt% (a negligible envelop) to 100 wt% (a negligible core). Our simulations were able to replicate the bimodal distribution in exoplanet radii. We argue that in order to reproduce the distribution by Fulton et al. (2017) it is mandatory for there to be a paucity of exoplanets with masses above ∼ 8M ⊕ . Furthermore, our bestfit result predicts an initial flat distribution in exoplanet occurrence for M P 8M ⊕ with a strong deficiency for planets with 3M ⊕ . Our results are consistent with the ∼ 1.3R ⊕ radius peak mostly encompassing denuded exoplanets whilst the ∼ 2.4R ⊕ radius peak mainly comprising exoplanets with large hydrogen envelops.

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On the potentially dramatic history of the super-Earth ρ 55 Cancri e

Cited by 42 publications

References 73 publications

The Eccentric Kozai-Lidov Effect and Its Applications

The Eccentric Kozai-Lidov Effect and Its Applications

Mass Constraints of the Wasp-47 Planetary System From Radial Velocities

The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and H₂ Envelope’s Sizes

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On the potentially dramatic history of the super-Earth ρ 55 Cancri e

Cited by 42 publications

References 73 publications

The Eccentric Kozai-Lidov Effect and Its Applications

The Eccentric Kozai-Lidov Effect and Its Applications

Mass Constraints of the Wasp-47 Planetary System From Radial Velocities

The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and H2 Envelope’s Sizes

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The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and H₂ Envelope’s Sizes