Hidden water in magma ocean exoplanets

Dorn, Caroline; Lichtenberg, Tim

doi:10.48550/arxiv.2110.15069

Cited by 3 publications

(4 citation statements)

References 104 publications

(145 reference statements)

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“…More complex models, including a lighter core compositions (i.e. a Ca/Al enriched core), the modelling of water steam envelopes, or wet-melt solid interiors related to deep water reservoirs (Dorn & Lichtenberg 2021), could be an interesting step forward in the understanding of the planet structure and composi- tion. The low density of TOI-561 b could also be related to the fact that the host star is a metal-poor, thick-disk star.…”

Section: Discussionmentioning

confidence: 99%

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Lacedelli,

Wilson,

Malavolta

et al. 2022

Preprint

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We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (𝑃 = 0.45 d, 𝑅 = 1.42 R ⊕ , 𝑀 = 2.0 M ⊕ ), c (𝑃 = 10.78 d, 𝑅 = 2.91 R ⊕ , 𝑀 = 5.4 M ⊕ ), d (𝑃 = 25.7 d, 𝑅 = 2.82 R ⊕ , 𝑀 = 13.2 M ⊕ ) and e (𝑃 = 77 d, 𝑅 = 2.55 R ⊕ , 𝑀 = 12.6 R ⊕ ). Moreover, we identify an additional, long-period signal (> 450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (𝜌 b = 3.8 ± 0.5 g cm −3 ) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.

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Section: Discussionmentioning

confidence: 99%

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Lacedelli,

Wilson,

Malavolta

et al. 2022

Preprint

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“…Although mineral water capacities are sensitive to temperature, we can assume that the initial potential temperature of a mantle having just crystallised from the primordial magma ocean is equal to its shallow solidus temperature. Further, this newly-solid mantle could easily have inherited a water concentration near its saturation value (Tikoo & Elkins-Tanton 2017;Dorn & Lichtenberg 2021;Bower et al 2021;Miyazaki & Korenaga 2022). Therefore the mantle water capacity of a young planet provides a deterministic initial condition to its actual water content.…”

Section: Discussionmentioning

confidence: 99%

“…The water budget of a planet's mantle may be set early on, shortly after its formation. Models of magma ocean crystallisation have suggested that primordial mantles may inherit large inventories of water, from formation at near-water saturated conditions (Tikoo & Elkins-Tanton 2017;Dorn & Lichtenberg 2021;Bower et al 2021;Miyazaki & Korenaga 2022). Thus, the solubility of water in hot, newly-solidified, mantles likely provides the initial condition for subsequent water cycling-a particularly important bound for stagnant lid planets, which may lack an efficient return flux of volatiles to the mantle (e.g., Foley & Smye 2018).…”

Section: Introductionmentioning

confidence: 99%

Mantle mineralogy limits to rocky planet water inventories

Guimond¹,

Shorttle²,

Rudge³

2022

Preprint

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Nominally anhydrous minerals in rocky planet mantles can sequester oceans of water as a whole, giving a constraint on bulk water inventories. Here we predict mantle water capacities from the thermodynamically-limited solubility of water in their constituent minerals. We report the variability of mantle water capacity due to (i) host star refractory element abundances that set mineralogy, (ii) realistic mantle temperature scenarios, and (iii) planet mass. We find that planets large enough to stabilise perovskite almost unfailingly have a dry lower mantle, topped by a high-watercapacity transition zone which may act as a bottleneck for water transport within the planet's interior. Because the pressure of the ringwoodite-perovskite phase boundary defining the lower mantle is roughly insensitive to planet mass, the relative contribution of the upper mantle reservoir will diminish with increasing planet mass. Large rocky planets therefore have disproportionately small mantle water capacities. In practice, our results would represent initial water concentration profiles in planetary mantles where their primordial magma oceans are water-saturated. We suggest that a considerable proportion of massive rocky planets' accreted water budgets would form surface oceans or atmospheric water vapour immediately after magma ocean solidification, possibly diminishing the likelihood of these planets hosting land. This work is a step towards understanding planetary deep water cycling, thermal evolution as mediated by rheology and melting, and the frequency of waterworlds.

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“…These planets are exposed to extreme stellar irradiation that leads to surface temperatures hot enough to prevent the planet from cooling and creating a crust (Boukaré et al, 2022;Henning et al, 2018), exposing the silicate mantle directly to the atmosphere. Furthermore, since the atmosphere is a direct product of the outgassing from the magma ocean and is in equilibrium with it, the atmospheric compositions of these planets are directly influenced by the interior composition (Dorn & Lichtenberg, 2021;Ito et al, 2015;Kite et al, 2016Kite et al, , 2020Miguel et al, 2011;Nguyen et al, 2020). This provides a unique opportunity to derive interior properties from atmospheric observations.…”

Section: Introductionmentioning

confidence: 99%

LavAtmos: An open‐source chemical equilibrium vaporization code for lava worlds

Buchem

Miguel

Zilinskas

et al. 2023

Meteorit & Planetary Scien

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To date, over 500 short‐period rocky planets with equilibrium temperatures above 1500 K have been discovered. Such planets are expected to support magma oceans, providing a direct interface between the interior and the atmosphere. This provides a unique opportunity to gain insight into their interior compositions through atmospheric observations. A key process in doing such work is the vapor outgassing from the lava surface. LavAtmos is an open‐source code that calculates the equilibrium chemical composition of vapor above a dry melt for a given composition and temperature. Results show that the produced output is in good agreement with the partial pressures obtained from experimental laboratory data as well as with other similar codes from literature. LavAtmos allows for the modeling of vaporization of a wide range of different mantle compositions of hot rocky exoplanets. In combination with atmospheric chemistry codes, this enables the characterization of interior compositions through atmospheric signatures.

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Hidden water in magma ocean exoplanets

Cited by 3 publications

References 104 publications

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

Mantle mineralogy limits to rocky planet water inventories

LavAtmos: An open‐source chemical equilibrium vaporization code for lava worlds

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