Internal structure of massive terrestrial planets

Valencia, Diana; O’Connell, Richard J.; Sasselov, Dimitar

doi:10.1016/j.icarus.2005.11.021

Cited by 502 publications

(516 citation statements)

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“…The corresponding population of low mass planets was previously detected in radial velocity (RV) surveys (Mayor & Udry 2008;Howard et al 2009), but notably has no analog in our own solar system. The composition of these objects is not yet well understood; theoretical models predict that some of these intermediate size planets may be predominantly rocky and others may have a large fractional composition of volatiles or a substantial hydrogen envelope (Léger et al 2004;Valencia et al 2006;Fortney et al 2007;Seager et al 2007;Zeng & Sasselov 2013). There is presently only a small number of such planets observed to transit and having published mass estimates with a precision better than 20%, while less precise mass estimates are generally not sufficient to distinguish between a rocky compositional model and one that is volatile-rich.…”

Section: Introductionmentioning

confidence: 99%

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

Gettel

Charbonneau

Dressing

et al. 2016

ApJ

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Kepler-454 (KOI-273) is a relatively bright (V = 11.69 mag), Sun-like star that hosts a transiting planet candidate in a 10.6 day orbit. From spectroscopy, we estimate the stellar temperature to be 5687±50 K, its metallicity to be [m/H] = 0.32±0.08, and the projected rotational velocity to be v sin i<2.4 km s −1 . We combine these values with a study of the asteroseismic frequencies from short cadence Kepler data to estimate the stellar mass to be M 1.028 0.03 0.04 -+  , the radius to be 1.066±0.012 R e , and the age to be 5.25 1.39Gyr. We estimate the radius of the 10.6 day planet as 2.37±0.13 R ⊕ . Using 63 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 36 observations made with the HIRES spectrograph at the Keck Observatory, we measure the mass of this planet to be 6.8±1.4 M ⊕ . We also detect two additional nontransiting companions, a planet with a minimum mass of 4.46±0.12 M J in a nearly circular 524 day orbit and a massive companion with a period >10 years and mass >12.1 M J . The 12 exoplanets with radii <2.7 R ⊕ and precise mass measurements appear to fall into two populations, with those <1.6 R ⊕ following an Earth-like composition curve and larger planets requiring a significant fraction of volatiles. With a density of 2.76±0.73 g cm −3 , Kepler-454b lies near the mass transition between these two populations and requires the presence of volatiles and/or H/He gas.

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Section: Introductionmentioning

confidence: 99%

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

Gettel

Charbonneau

Dressing

et al. 2016

ApJ

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“…Guillot et al 2005;Fortney et al 2007). Objects lighter than ten Earth masses are even more enigmatic, as they can be explained in different ways (Valencia et al 2006(Valencia et al , 2007Sotin et al 2007;Seager et al 2007;Adams et al 2008;Grasset et al 2009). …”

Section: Overviewmentioning

confidence: 99%

Spectroscopy of planetary atmospheres in our Galaxy

Tinetti

Encrenaz

Coustenis

2013

Astron Astrophys Rev

128

111

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About 20 years after the discovery of the first extrasolar planet, the number of planets known has grown by three orders of magnitude, and continues to increase at neck breaking pace. For most of these planets we have little information, except for the fact that they exist and possess an address in our Galaxy. For about one third of them, we know how much they weigh, their size and their orbital parameters. For less than 20, we start to have some clues about their atmospheric temperature and composition. How do we make progress from here?We are still far from the completion of a hypothetical Hertzsprung-Russell diagram for planets comparable to what we have for stars, and today we do not even know whether such classification will ever be possible or even meaningful for planetary objects. But one thing is clear: planetary parameters such as mass, radius and temperature alone do not explain the diversity revealed by current observations. The chemical composition of these planets is needed to trace back their formation history and evolution, as happened for the planets in our Solar System. As in situ measurements are and will remain off-limits for exoplanets, to study their chemical composition we will have to rely on remote sensing spectroscopic observations of their gaseous envelopes.

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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) …”

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“…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.…”

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“…Seu modeloé constituído por cinco camadas: no centro, um núcleo rico em ferro fluido, consistindo de uma mistura de F e e F eS, com 80 % de ferro puro; um manto inferior de silicato constituído por uma mistura de silicatos a altas pressões, rico em ferro e magnésio; um manto superior composto por olivina e enstatita; uma camada de gelo a alta pressão; e uma hidrosfera, onde aáguaé encontrada na forma líquida ou na forma de gelo. A relação massa-raio proviniente deste modelo concorda com os valores encontrados por Valencia et al (2006):…”

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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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Internal structure of massive terrestrial planets

Cited by 502 publications

References 26 publications

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

The Kepler-454 System: A Small, Not-Rocky Inner Planet, a Jovian World, and a Distant Companion

Spectroscopy of planetary atmospheres in our Galaxy

Exoplanetas, Extremófilos e Habitabilidade

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