Mass–radius curve for extrasolar Earth-like planets and ocean planets

Sotin, C.; Grasset, O.; Mocquet, A.

doi:10.1016/j.icarus.2007.04.006

Cited by 397 publications

(565 citation statements)

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“…Two end-member models of tidal theory have been applied to exoplanets and the bodies of our solar system: one assumes the energy dissipation gives a constant phase lag in For these calculations we used the stellar mass-radius relationship from Bayless and Orosz (2006), the mass-luminosity relationship from Reid and Hawley (2000), and the terrestrial mass-radius relationship from Sotin et al (2007). the periodic distortion (CPL), and the other assumes a constant time lag (CTL) (Greenberg, 2009).…”

Section: Tidal Heatingmentioning

confidence: 99%

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

et al. 2013

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Traditionally, stellar radiation has been the only heat source considered capable of determining global climate on long timescales. Here, we show that terrestrial exoplanets orbiting low-mass stars may be tidally heated at highenough levels to induce a runaway greenhouse for a long-enough duration for all the hydrogen to escape. Without hydrogen, the planet no longer has water and cannot support life. We call these planets ''Tidal Venuses'' and the phenomenon a ''tidal greenhouse.'' Tidal effects also circularize the orbit, which decreases tidal heating. Hence, some planets may form with large eccentricity, with its accompanying large tidal heating, and lose their water, but eventually settle into nearly circular orbits (i.e., with negligible tidal heating) in the habitable zone (HZ). However, these planets are not habitable, as past tidal heating desiccated them, and hence should not be ranked highly for detailed follow-up observations aimed at detecting biosignatures. We simulated the evolution of hypothetical planetary systems in a quasi-continuous parameter distribution and found that we could constrain the history of the system by statistical arguments. Planets orbiting stars with masses < 0.3 M Sun may be in danger of desiccation via tidal heating. We have applied these concepts to Gl 667C c, a *4.5 M Earth planet orbiting a 0.3 M Sun star at 0.12 AU. We found that it probably did not lose its water via tidal heating, as orbital stability is unlikely for the high eccentricities required for the tidal greenhouse. As the inner edge of the HZ is defined by the onset of a runaway or moist greenhouse powered by radiation, our results represent a fundamental revision to the HZ for noncircular orbits. In the appendices we review (a) the moist and runaway greenhouses, (b) hydrogen escape, (c) stellar mass-radius and mass-luminosity relations, (d) terrestrial planet mass-radius relations, and (e) linear tidal theories.

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Section: Tidal Heatingmentioning

confidence: 99%

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

et al. 2013

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“…Há dois modelos análogos aos modelos terrestres que darão suporte a esta pesquisa (Valencia et al, 2006;Sotin et al, 2007), pois fornecem uma boa estimativa da razão massa-raio para alguns tipos de exoplanetas. Valencia et al (2006) …”

Section: Entretanto Com Técnicas Mais Avançadas E Os Lançamentos Da unclassified

“…Paralelamente aos estudos realizados por Valencia et al (2006), Sotin et al (2007) desenvolveram um modelo para caracterizar exoplanetas do tipo terrestre baseado em planetas rochosos e objetos (satélite e planetas) localizados além da snow line do Sistema Solar. Eles levaram em consideração na contrução de seu modelo parâmetros como a distância da estrela, o conteúdo de magnésio no manto, a fração de massa deágua e a massa total do planeta.…”

Section: Entretanto Com Técnicas Mais Avançadas E Os Lançamentos Da unclassified

“…Certamente devem ter sido formados em regiões mais externas dos sistemas planetários onde a condensação dá agua pode ocorrer e, ao passar por um processo migratório, atingido regiões mais internas. O modelo desenvolvido por Sotin et al (2007) permite uma simulação satisfatória da estrutura interna de planetas oceânicos, levando a uma relação massa-raio igual a:…”

Section: Planetas Extrasolares Oceânicosunclassified

“…Cálculos baseados em simulações mostram que exoplanetas contendo 50 % de massa emágua possuem seus raios com valores 25 % maiores do que os raios de planetas com composição semelhanteà terrestre (Sotin et al, 2007). , 2002).…”

Section: Planetas Extrasolares Oceânicosunclassified

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Exoplanetas, Extremófilos e Habitabilidade

Bernardes¹

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O principal objetivo do trabalhoé estimar a possibilidade de sobrevivência de microorganismos extremófilos na superfície de exoplanetas conhecidos, assim como na superfície de seus eventuais satélites naturais. Foi utilizado um modelo que simula a atmosfera terrestre primordial, composta principalmente por nitrogênio,água e dióxido de carbono. E em se tratando de extremófilos, esses cálculos não foram limitadosà Zona Habitável dos sistemas planetários, pois esse conceito foi estendido para uma região mais ampla, a "Zona Extremófila", onde a vida pode existir. Extremófilos são micro-organismos terrestres que vivem sob condições extremas de temperatura, nível de radiação, umidade, pressão, salinidade, pH, etc. . . Eles são candidatos naturais para habitarem meios ditos extraterrestres onde tais condições são eventualmente encontradas. Alguns exemplos desses ambientes em nosso sistema solar são: Marte, Titã (satélite de Saturno) e Europa (satélite de Júpiter).Há algumas centenas de planetas orbitando outras estrelas (exoplanetas) e a maioria deles são gigantes gasosos, em particular Hot Jupiters. A temperatura superficial de um planeta depende fortemente de seu albedo, de sua distância orbital, de condições geodinâmicas intrínsecas, além do tipo espectral de sua estrela hospedeira. A estimativa dessa temperatura foi obtida considerando o ciclo silicato-carbono e um balanço de energia global, que contribuiram para se obter estimativas da pressão parcial atmosférica devido ao CO 2 e da temperatura média, na superfície dos planetas e/ou de seus satélites hipotéticos.Os eventuais satélites naturais de planetas gigantes podem abrigar vida e essa possibilidade foi testada através da análise das condições de estabilidade orbital desses corpos celestes.Os resultados deste trabalho deverão fornecer subsídios para a hipótese da panspermia. AbstractThe main objective of this study is to estimate the chance of survival of microorganisms (extremophiles) on the surface of known exoplanets, as well as on the surface of its potential natural satellites. We used a model that simulates the primordial atmosphere composed by, primarily, nitrogen, water and carbon dioxide. And when it comes to extremophiles, these calculations were not limited to the Habitable Zone of planetary systems, since this concept was extended to a wider region, the "Extremophile Zone", where life can exist. Extremophiles are terrestrial microorganisms living under extreme conditions of temperature, light level, humidity, pressure, salinity, pH, etc ... They are natural candidates for living in habitats considered extraterrestrials where such conditions are encountered eventually. Examples of such environments in our solar system are: Mars, Titan (moon of Saturn) and Europe (satellite of Jupiter).There are hundreds of planets orbiting other stars (exoplanets) and most of them are gas giants, particularly Hot Jupiters. The surface temperature of a planet/moon depends heavily on its albedo, its orbital distance, of geodynamic conditions intrinsic, in addition to ...

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Thermal conductivity of H₂O‐CH₃OH mixtures at high pressures: Implications for the dynamics of icy super‐Earths outer shells

Hsieh

Deschamps

2015

JGR Planets

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Thermal conductivity of H 2 O-volatile mixtures at extreme pressure-temperature conditions is a key factor to determine the heat flux and profile of the interior temperature in icy bodies. We use time domain thermoreflectance and stimulated Brillouin scattering combined with diamond anvil cells to study the thermal conductivity and sound velocity of water (H 2 O)-methanol (CH 3 OH) mixtures to pressures as high as 12 GPa. Compared to pure H 2 O, the presence of 5-20 wt % CH 3 OH significantly reduces the thermal conductivity and sound velocity when the mixture becomes ice VI-CH 3 OH and ice VII-CH 3 OH phases at high pressures, indicating that the heat transfer is hindered within the icy body. We then apply these results to model the heat transfer through the icy mantles of super-Earths, assuming that these mantles are animated by thermal convection. Our calculations indicate that the decrease of thermal conductivity due to the presence of 10 wt % CH 3 OH induces a twofold decrease of the power transported by convection.

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Mass–radius curve for extrasolar Earth-like planets and ocean planets

Cited by 397 publications

References 56 publications

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

Exoplanetas, Extremófilos e Habitabilidade

Thermal conductivity of H₂O‐CH₃OH mixtures at high pressures: Implications for the dynamics of icy super‐Earths outer shells

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Mass–radius curve for extrasolar Earth-like planets and ocean planets

Cited by 397 publications

References 56 publications

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

Exoplanetas, Extremófilos e Habitabilidade

Thermal conductivity of H2O‐CH3OH mixtures at high pressures: Implications for the dynamics of icy super‐Earths outer shells

Contact Info

Product

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Thermal conductivity of H₂O‐CH₃OH mixtures at high pressures: Implications for the dynamics of icy super‐Earths outer shells