Magma oceans and enhanced volcanism on TRAPPIST-1 planets due to induction heating

Kislyakova, K. G.; Noack, Lena; Johnstone, C. P.; Зайцев, В. В.; Fossati, L.; Lämmer, H.; Khodachenko, M. L.; Odert, P.; Güdel, M.

doi:10.1038/s41550-017-0284-0

Cited by 81 publications

(101 citation statements)

References 55 publications

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“…Close-in planets that are highly irradiated and experience strong tidal heating (e.g. Bolmont et al 2013) or induction heating due to the stellar magnetic field (Kislyakova et al 2017), might have largely molten interiors which reduces the bulk density similar to our calculated planetary interiors (Fig. 9).…”

Section: Mass-radiussupporting

confidence: 59%

Linking the evolution of terrestrial interiors and an early outgassed atmosphere to astrophysical observations

Bower¹,

Kitzmann²,

Wolf³

et al. 2019

Preprint

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Context.A terrestrial planet is molten during formation and may remain molten due to intense insolation or tidal forces. Observations favour the detection and characterisation of hot planets, potentially with large outgassed atmospheres. Aims. We aim to determine the radius of hot Earth-like planets with large outgassing atmospheres. Our goal is to explore the differences between molten and solid silicate planets on the mass-radius relationship and transmission and emission spectra.Methods. An interior-atmosphere model was combined with static structure calculations to track the evolving radius of a hot rocky planet that outgasses CO 2 and H 2 O. We generated synthetic emission and transmission spectra for CO 2 and H 2 O dominated atmospheres. Results. Atmospheres dominated by CO 2 suppress the outgassing of H 2 O to a greater extent than previously realised since previous studies applied an erroneous relationship between volatile mass and partial pressure. We therefore predict that more H 2 O can be retained by the interior during the later stages of magma ocean crystallisation. Formation of a surface lid can tie the outgassing of H 2 O to the efficiency of heat transport through the lid, rather than the radiative timescale of the atmosphere. Contraction of the mantle, as it cools from molten to solid, reduces the radius by around 5%, which can partly be offset by the addition of a relatively light species (e.g. H 2 O versus CO 2 ) to the atmosphere. Conclusions. A molten silicate mantle can increase the radius of a terrestrial planet by around 5% compared to its solid counterpart, or equivalently account for a 13% decrease in bulk density. An outgassing atmosphere can perturb the total radius, according to its composition, notably the abundance of light versus heavy volatile species. Atmospheres of terrestrial planets around M-stars that are dominated by CO 2 or H 2 O can be distinguished by observing facilities with extended wavelength coverage (e.g. JWST).

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Section: Mass-radiussupporting

confidence: 59%

Linking the evolution of terrestrial interiors and an early outgassed atmosphere to astrophysical observations

Bower¹,

Kitzmann²,

Wolf³

et al. 2019

Preprint

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“…Due to their slow evolution, M stars can keep high levels of XUV radiation in their HZs for a longer time in comparison to solar-like stars (West et al 2008), which can further enhance non-thermal losses. The atmospheres of planets orbiting active low mass M dwarfs may be replenished by extreme volcanic activity due to tidal or induction heating (Driscoll & Barnes 2015;Kislyakova et al 2017Kislyakova et al , 2018. A volcanically active planet would eject gases composed mainly of SO 2 , CO 2 , H 2 O, and S 2 .…”

Section: Atmosphere Parametersmentioning

confidence: 99%

Transit Lyman-α signatures of terrestrial planets in the habitable zones of M dwarfs

Kislyakova

Holmström

Odert

et al. 2019

A&A

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Aims. We modeled the transit signatures in the Lyman-alpha (Lyα) line of a putative Earth-sized planet orbiting in the habitable zone (HZ) of the M dwarf GJ 436. We estimated the transit depth in the Lyα line for an exo-Earth with three types of atmospheres: a hydrogen-dominated atmosphere, a nitrogen-dominated atmosphere, and a nitrogen-dominated atmosphere with an amount of hydrogen equal to that of the Earth. For all types of atmospheres, we calculated the in-transit absorption they would produce in the stellar Lyα line. We applied it to the out-of-transit Lyα observations of GJ 436 obtained by the Hubble Space Telescope and compared the calculated in-transit absorption with observational uncertainties to determine if it would be detectable. To validate the model, we also used our method to simulate the deep absorption signature observed during the transit of GJ 436b and showed that our model is capable of reproducing the observations. Methods. We used a direct simulation Monte Carlo (DSMC) code to model the planetary exospheres. The code includes several species and traces neutral particles and ions. It includes several ionization mechanisms, such as charge exchange with the stellar wind, photo-and electron impact ionization, and allows to trace particles collisions. At the lower boundary of the DSMC model we assumed an atmosphere density, temperature, and velocity obtained with a hydrodynamic model for the lower atmosphere. Results. We showed that for a small rocky Earth-like planet orbiting in the HZ of GJ 436 only the hydrogen-dominated atmosphere is marginally detectable with the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). Neither a pure nitrogen atmosphere nor a nitrogen-dominated atmosphere with an Earth-like hydrogen concentration in the upper atmosphere are detectable. We also showed that the Lyα observations of GJ 436b can be reproduced reasonably well assuming a hydrogendominated atmosphere, both in the blue and red wings of the Lyα line, which indicates that warm Neptune-like planets are a suitable target for Lyα observations. Terrestrial planets, on the other hand, can be observed in the Lyα line if they orbit very nearby stars, or if several observational visits are available.

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“…Another newly identified heating source for exoplanets is induction heating (Kislyakova et al 2017). Electromagnetic induction is the production of voltage across an electrical conductor if the magnetic field around it varies in time.…”

Section: ;mentioning

confidence: 99%

“…We have assumed the equilibrium temperature of HD3167 b at its surface as a boundary condition (see Table 2). We have used the procedure to calculate induction heating in a planet with a conductivity varying with depth, as described in Kislyakova et al (2017). In this model, induction equation is solved in every layer, and the conductivity values at the surface and in the planetary core are used as boundary conditions.…”

Section: ;mentioning

confidence: 99%

Searching for volcanic activity and a mercury-like exosphere of the super-Earth HD3167 b

Guenther

Kislyakova

2019

Monthly Notices of the Royal Astronomical Society

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HD3167 b is a transiting super-Earth that has a density which is consistent with a rocky composition. The planet is exposed to strong radiation, intense stellar wind, and likely strong tidal forces and induction heating. According to theory, planets that are so close to the star should have an atmosphere like Mercury but much more extended and denser. Other theories predict that such planets have a lava lake on their surfaces and exhibit an enormous volcanic activity. We have calculated the heating by electromagnetic induction to estimate if it can drive significant volcanic activity at HD3167 b and shown that for some magnetic fields the heating can be substantial. HD3167 is an ideal target to search for the exosphere of a planet, and signs of volcanic activity. We observed the planet in-and out-of transit with UVES in order to search for presence of lines originating from the exosphere of the planet such as the Na D 1,2 and CaII H&K lines as well as numerous [S II], [S III], and [O III] lines that are tracers of volcanic activity. We derived upper limits for the ratios of the line fluxes to the stellar flux. The upper limits that we derived are I p,λ /I * ,λ = 1.5 10 −3 for the CaII H&K lines, and I p,λ /I * ,λ = 7.2 10 −4 and I p,λ /I * ,λ = 3.3 10 −4 for the NaD 1,2 lines, respectively. The fact that our upper limits correspond to previous detections in 55 Cnc e shows that not all super-Earth show these lines all the time and that they might be variable.

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Magma oceans and enhanced volcanism on TRAPPIST-1 planets due to induction heating

Cited by 81 publications

References 55 publications

Linking the evolution of terrestrial interiors and an early outgassed atmosphere to astrophysical observations

Linking the evolution of terrestrial interiors and an early outgassed atmosphere to astrophysical observations

Transit Lyman-α signatures of terrestrial planets in the habitable zones of M dwarfs

Searching for volcanic activity and a mercury-like exosphere of the super-Earth HD3167 b

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