Machine-learning inference of the interior structure of low-mass exoplanets

Baumeister, Philipp; Padovan, Sebastiano; Tosi, Nicola; Montavon, Grégoire; Nettelmann, Nadine; MacKenzie, Jasmine; Godolt, M.

doi:10.5194/egusphere-egu2020-7520

Cited by 3 publications

(5 citation statements)

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“…GJ 367b is more consistent with pure iron and an interior similar to Mercury. (B) The predicted relative thicknesses of each interior layer of GJ 367b from the neural network model (32). The core is assumed to be a liquid a Fe-FeS alloy.…”

Section: Figs S1 To S10mentioning

confidence: 99%

“…The effect of a different prior for the light gas layer (e.g. logarithmic sampling instead of linear), has minor effects on the resulting distributions, especially for the core and silicate layers (32), which dominate the interior structure of GJ 367b. The core and silicate layers use standard equations of state (EoS) (115), the ice layer is modelled using the EoS of water ice VII.…”

Section: Simultaneous Analysis Of the Tess Photometry And Harps Rv Measurementsmentioning

confidence: 99%

“…Ice and gas could be present if the object formed far from the parent star and reached its current position via migration (117) or eccentricity excitation (118). This method has been used (32) to compare the inferred interior structure of the Earth to the core and mantle thickness from the Preliminary Reference Earth Model (PREM) (119). The values between two models agree within the uncertainties but the peak of the MDN distribution does not align with the core values from PREM, which was attributed to the large degeneracy in the interior model.…”

Section: Simultaneous Analysis Of the Tess Photometry And Harps Rv Measurementsmentioning

confidence: 99%

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GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

Lam

Csizmadia

Astudillo-Defru

et al. 2021

Science

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Ultra-short-period (USP) exoplanets have orbital periods shorter than one day. Precise masses and radii of USPs could provide constraints on their unknown formation and evolution processes. We report the detection and characterization of the USP planet GJ 367b using high precision photometry and radial velocity observations. GJ 367b orbits a bright (V-band magnitude = 10.2), nearby, red (M-type) dwarf star every 7.7 hours. GJ 367b has a radius of 0.718 ± 0.054 Earth-radii, a mass of 0.546 ± 0.078 Earth-masses, making it a sub-Earth. The corresponding bulk density is 8.106 ± 2.165 g cm -3 , close to that of iron. An interior structure model predicts the planet has an iron core radius fraction of 86 ± 5%, similar to Mercury's interior. Main Text:Red dwarf stars of spectral type M (M dwarfs) are cool stars with effective temperatures (Teff) below ~4000 K (1). They have masses and radii less than around ~60% of the Sun's and are the most abundant type of stars in the solar neighborhood (2-4). It has been estimated that M dwarfs host an average of 2.5 ± 0.2 small planets [planet radius Rp < 4 Earth-radius (R⊕)] with periods less than 100 days (5). Due to the small stellar radius, the transit signal produced

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Section: Figs S1 To S10mentioning

confidence: 99%

Section: Simultaneous Analysis Of the Tess Photometry And Harps Rv Measurementsmentioning

confidence: 99%

Section: Simultaneous Analysis Of the Tess Photometry And Harps Rv Measurementsmentioning

confidence: 99%

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GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

Lam

Csizmadia

Astudillo-Defru

et al. 2021

Science

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“…These EoSs differ in whether or not they take temperature dependence into account. Baumeister et al (2018) performed an extensive parameter study to model the internal structure of a large number of subneptunian exoplanets of different compositions, ranging from super-Earths consisting only of a metallic core and silicate mantle to subneptunes with ice and gas layers. They found that for the rocky interior of an exoplanet, the choice of EoS has little effect on characterizing the planet's internal structure, and that for Earth-like planets, a simple isothermal EoS such as the third-order isothermal Birch-Murnaghan EoS is sufficient to accurately model their interiors.…”

Section: The Modelmentioning

confidence: 99%

Relation between Mass and Radius of Exoplanets Distinguished by their Density

Betzler

Miranda

2023

Res. Astron. Astrophys.

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The formation of the solar system has been studied since the 18th century and received a boost in 1995 with the discovery of the first exoplanet, 51 Pegasi b. The investigations increased the number of confirmed planets to about 5,300 to date. The possible internal structure and composition of these planets can be inferred from the relationship between planet mass and radius, M-R. We have analyzed the M-R relation of a selected sample of iron-rock and ice-gas planets using a fractal approach to their densities. The application of fractal theory is particularly useful to define the physical meaning of the proportionality constant and the exponent in an empirical M-R power law in exoplanets, but this does not necessarily mean that they have an internal fractal structure. The M-R relations based on this sample are M$=(1.46 \pm 0.08) \text{R}^{2.6 \pm 0.2}$ for the rocky population ($3.6 \leq \rho \leq 14.3$ g/cm$^3$), with $1.5 \leq \text{M} \leq 39$ M$_{\Earth}$, and M $=(0.27 \pm 0.04) \text{R}^{2.7 \pm 0.2}$ for ice-gas planets ($0.3 \leq \rho \leq 2.1$ g/cm$^3$) with $5.1 \leq \text{M} \leq 639$ M$_{\Earth}$ (or $\simeq 2 \text{M}_{\text{J}}$) and orbital periods greater than 10 days. Both M-R relations have in their density range a great predictive power for the determination of the mass of exoplanets and even for the largest icy moons of the solar system. The average fractal dimension of these planets is D$=2.6 \pm 0.1$, indicating that these objects likely have a similar degree of heterogeneity in their densities and a nearly similar composition \textcolor{red}{in each sample}. The M-R diagram shows a ``gap'' between ice-gas and iron-rock planets. This gap is a direct consequence of the density range of these two samples. We empirically propose an upper mass limit of about 100 M$_{\Earth}$, so that an M-R relation for an ice-gas planets in a narrow density range is defined by M $\propto$ R$^{3}$.

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“…Baumeister et al. (2020) used MDNs to predict the distribution of the possible interior structures of extrasolar planets for given mass and radius.…”

Section: Introductionmentioning

confidence: 99%

Toward Constraining Mars' Thermal Evolution Using Machine Learning

Agarwal

Tosi

Kessel

et al. 2021

Earth and Space Science

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• Mixture Density Networks provide a probabilistic framework for inverting observables to infer parameters of Mars' interior evolution. 10 • Reference viscosity, crustal enrichment in heat-producing elements and initial mantle 11 temperature can be well constrained. 12 • Activation energy of diffusion creep can be weakly constrained; constraining activation 13 volume requires new observational signatures.

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Machine-learning inference of the interior structure of low-mass exoplanets

Cited by 3 publications

References 0 publications

GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star

Relation between Mass and Radius of Exoplanets Distinguished by their Density

Toward Constraining Mars' Thermal Evolution Using Machine Learning

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