Equation of state for ε-iron at high pressures and temperatures

Belonoshko, Anatoly B.

doi:10.5488/cmp.13.23605

Cited by 17 publications

(14 citation statements)

References 30 publications

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“…Our model for the inner planet follows the model originally developed by Sotin et al (2007), and further improved by Grasset et al (2010), with some differences related to the assumed EOS iron, where we have used the most recent EOS developed by Belonoshko (2010). For the gas envelope, we have considered three models, one convective/isothermal model, one radiative/convective model, and a two-stream irradiated model following the model of Guillot (2010).…”

Section: Discussionmentioning

confidence: 99%

“…This EOS for Fe has been preferred to the one used by Sotin et al (2007), as it allows to reproduce high-precision volumetric experiments of iron under high pressure and temperature closely (see Belonoshko 2010). The adiabatic gradient is computed as…”

Section: Modelmentioning

confidence: 99%

“…In the case of the iron core, the value of the thermal expansion coefficient are directly computed from Belonoshko's EOS (Belonoshko 2010). Finally, we assume the water layer is isothermal.…”

Section: Modelmentioning

confidence: 99%

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On the radius of habitable planets

Alibert

2013

A&A

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Context. The conditions that a planet must fulfill to be habitable are not precisely known. However, it is comparatively easier to define conditions under which a planet is very likely not habitable. Finding such conditions is important as it can help select, in an ensemble of potentially observable planets, which ones should be observed in greater detail for characterization studies. Aims. Assuming, as in the Earth, that the presence of a C-cycle is a necessary condition for long-term habitability, we derive, as a function of the planetary mass, a radius above which a planet is likely not habitable. We compute the maximum radius a planet can have to fulfill two constraints: surface conditions compatible with the existence of liquid water, and no ice layer at the bottom of a putative global ocean. We demonstrate that, above a given radius, these two constraints cannot be met. Methods. We compute internal structure models of planets, using a five-layer model (core, inner mantle, outer mantle, ocean, and atmosphere), for different masses and composition of the planets (in particular, the Fe/Si ratio of the planet). Results. Our results show that for planets in the super-Earth mass range (1-12 M ⊕ ), the maximum that a planet, with a composition similar to that of the Earth, can have varies between 1.7 and 2.2 R ⊕ . This radius is reduced when considering planets with higher Fe/Si ratios and taking radiation into account when computing the gas envelope structure. Conclusions. These results can be used to infer, from radius and mass determinations using high-precision transit observations like those that will soon be performed by the CHaracterizing ExOPlanet Satellite (CHEOPS), which planets are very likely not habitable, and therefore which ones should be considered as best targets for further habitability studies.

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Section: Discussionmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

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On the radius of habitable planets

Alibert

2013

A&A

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“…2, b показаны барические зависимости второго q(P) и третьего z (P) параметров Грюнайзена. Оценки других авторов для q лежат в довольно широком ин-тервале: q = 0.69−1.7 -для ГЦК и ГПУ железа [3], 1.6 ± 0.6 -для ГЦК железа [15], 1.2−2.0 -для ГЦК и ГПУ железа [18], q = (−0.978)−(+0.489) -для ГПУ железа [19].…”

Section: результаты расчетовunclassified

"Изменение" Решеточных Свойств И Температуры Плавления Гранецентрированной Кубической Структуры Железа При Сжатии

Магомедов¹

2017

Журнал Технической Физики

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“…Finally, we used the EOS derived by Belonoshko (2010) for pure Fe, which is similar to the Mie-Gruneisen-Debye EOS, but with a different thermal pressure term:…”

Section: Equations Of Statementioning

confidence: 99%

Constraining the volatile fraction of planets from transit observations

Alibert

2016

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Context. The determination of the abundance of volatiles in extrasolar planets is very important as it can provide constraints on transport in protoplanetary disks and on the formation location of planets. However, constraining the internal structure of low-mass planets from transit measurements is known to be a degenerate problem. Aims. Using planetary structure and evolution models, we show how observations of transiting planets can be used to constrain their internal composition, in particular the amount of volatiles in the planetary interior, and consequently the amount of gas (defined in this paper to be only H and He) that the planet harbors. We first explore planets that are located close enough to their star to have lost their gas envelope. We then concentrate on planets at larger distances and show that the observation of transiting planets at different evolutionary ages can provide statistical information on their internal composition, in particular on their volatile fraction. Methods. We computed the evolution of low-mass planets (super-Earths to Neptune-like) for different fractions of volatiles and gas. We used a four-layer model (core, silicate mantle, icy mantle, and gas envelope) and computed the internal structure of planets for different luminosities. With this internal structure model, we computed the internal and gravitational energy of planets, which was then used to derive the time evolution of the planet. Since the total energy of a planet depends on its heat capacity and density distribution and therefore on its composition, planets with different ice fractions have different evolution tracks. Results. We show for low-mass gas-poor planets that are located close to their central star that assuming evaporation has efficiently removed the entire gas envelope, it is possible to constrain the volatile fraction of close-in transiting planets. We illustrate this method on the example of 55 Cnc e and show that under the assumption of the absence of gas, the measured mass and radius imply at least 20% of volatiles in the interior. For planets at larger distances, we show that the observation of transiting planets at different evolutionary ages can be used to set statistical constraints on the volatile content of planets. Conclusions. These results can be used in the context of future missions like PLATO to better understand the internal composition of planets, and based on this, their formation process and potential habitability.

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Equation of state for ε-iron at high pressures and temperatures

Cited by 17 publications

References 30 publications

On the radius of habitable planets

On the radius of habitable planets

"Изменение" Решеточных Свойств И Температуры Плавления Гранецентрированной Кубической Структуры Железа При Сжатии

Constraining the volatile fraction of planets from transit observations

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