Interior and Surface Dynamics of Terrestrial Bodies and their Implications for the Habitability

Noack, Lena; Breuer, D.

doi:10.1007/978-94-007-6546-7_12

Cited by 5 publications

(2 citation statements)

References 140 publications

(156 reference statements)

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“…6 refers to planets and moons in the Solar System. Mars, the moon and Venus were believed to be inhabited (see also review in Noack and Breuer 2013), until the area of space missions revolutionised the idea of life on other planets.…”

Section: Searching For Life Outside Of Earthmentioning

confidence: 99%

Water in Extrasolar Planets and Implications for Habitability

2017

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Exoplanet detection missions have found thousands of planets or planet candidates outside of the Solar System -some of which are in the habitable zone, where liquid water is possible at the surface. We give an overview of the recent progress in observations of water-rich exoplanets, detection of water in the atmosphere of gas giants and less-massive targets, and modelling of the interior and evolution of water layers in exoplanets. We summarise the possible habitability of water-rich planets and discuss the potential of future missions and telescopes towards the detection of water in the atmosphere of low-mass exoplanets or on their surface.

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Section: Searching For Life Outside Of Earthmentioning

confidence: 99%

Water in Extrasolar Planets and Implications for Habitability

2017

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“…Alternatively, silicate and metal planets can be locked in a geodynamical regime with very little or no surface mobility (a stagnant lid), among other possibilities (e.g., a heat-pipe regime; Moore & Webb 2013;Lourenco et al 2020). Whether a planet can sustain effective crustal recycling by processes such as plate tectonics is considered an important factor in determining its potential to host biological activity over geologic timescales (e.g., Parnell 2004;Noack & Breuer 2013;Mojzsis 2021). Evidently, the planet size affects thermal evolution and propensity toward plate tectonics (e.g., Valencia et al 2006;O'Neill et al 2007; Van Heck & Tackley 2011; Stamenković et al 2012;Stein et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Plausible Constraints on the Range of Bulk Terrestrial Exoplanet Compositions in the Solar Neighborhood

Spaargaren

Wang

Mojzsis

et al. 2023

ApJ

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Rocky planet compositions regulate planetary evolution by affecting core sizes, mantle properties, and melting behaviors. Yet, quantitative treatments of this aspect of exoplanet studies remain generally underexplored. We attempt to constrain the range of potential bulk terrestrial exoplanet compositions in the solar neighborhood (<200 pc). We circumscribe probable rocky exoplanet compositions based on a population analysis of stellar chemical abundances from the Hypatia and GALAH catalogs. We apply a devolatilization model to simulate compositions of hypothetical, terrestrial-type exoplanets in the habitable zones around Sun-like stars, considering elements O, S, Na, Si, Mg, Fe, Ni, Ca, and Al. We further apply core–mantle differentiation by assuming constant oxygen fugacity, and model the consequent mantle mineralogy with a Gibbs energy minimization algorithm. We report statistics on several compositional parameters and propose a reference set of (21) representative planet compositions for use as end-member compositions in imminent modeling and experimental studies. We find a strong correlation between stellar Fe/Mg and metallic-core sizes, which can vary from 18 to 35 wt%. Furthermore, stellar Mg/Si gives a first-order indication of mantle mineralogy, with high-Mg/Si stars leading to weaker, ferropericlase-rich mantles, and low-Mg/Si stars leading to mechanically stronger mantles. The element Na, which modulates crustal buoyancy and mantle clinopyroxene fraction, is affected by devolatilization the most. While we find that planetary mantles mostly consist of Fe/Mg silicates, the core sizes and relative abundances of common minerals can nevertheless vary significantly among exoplanets. These differences likely lead to different evolutionary pathways among rocky exoplanets in the solar neighborhood.

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Water in Extrasolar Planets and Implications for Habitability

Noack¹,

Snellen²,

Rauer³

2017

Space Sciences Series of ISSI

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Exoplanet detection missions have found thousands of planets or planet candidates outside of the Solar System-some of which are in the habitable zone, where liquid water is possible at the surface. We give an overview of the recent progress in observations of water-rich exoplanets, detection of water in the atmosphere of gas giants and less-massive targets, and modelling of the interior and evolution of water layers in exoplanets. We summarise the possible habitability of water-rich planets and discuss the potential of future missions and telescopes towards the detection of water in the atmosphere of low-mass exoplanets or on their surface.

show abstract

Interior and Surface Dynamics of Terrestrial Bodies and their Implications for the Habitability

Cited by 5 publications

References 140 publications

Water in Extrasolar Planets and Implications for Habitability

Water in Extrasolar Planets and Implications for Habitability

Plausible Constraints on the Range of Bulk Terrestrial Exoplanet Compositions in the Solar Neighborhood

Water in Extrasolar Planets and Implications for Habitability

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