Phase equilibria in the system CO2-H2O I: New equilibrium relations at low temperatures

Longhi, J.

doi:10.1016/j.gca.2004.07.007

Cited by 43 publications

(32 citation statements)

References 23 publications

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“…Indeed, contrary to most other clathrateforming molecules, the sublimation vapor pressure curve for pure CO 2 ice (Giauque & Egan 1937;Fray & Schmitt 2009) lies just above the dissociation pressure curve of CO 2 clathrate hydrate in equilibrium with CO 2 gas + H 2 O ice. The different low-temperature extrapolations of these curves place the solid CO 2 /H 2 O ice/CO 2 clathrate/CO 2 gas quadruple point between 120 and 135 K (Miller & Smythe 1970;Longhi 2005). The crossing of the curves is more probably around 131 ± 2 K. Our estimate is 130.2 K using Clausius-Clapeyron laws based on the first experimental determinations of these curves (Giauque & Egan 1937;Miller & Smythe 1970) and critical reviews of the ice vapor pressures (Fray & Schmitt 2009) and clathrate hydrate dissociation pressures (Fray et al 2009) leads to a value of 132.5 ± 1 K.…”

Section: Phase Diagramsmentioning

confidence: 98%

Carbon dioxide clathrate hydrate FTIR spectrum

Dartois¹,

Schmitt

2009

A&A

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Section: Phase Diagramsmentioning

confidence: 98%

Carbon dioxide clathrate hydrate FTIR spectrum

Dartois¹,

Schmitt

2009

A&A

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“…Secondly, pressure and temperature conditions expected at the bottom of the ice layer are in the stability field of CO 2 clathrate hydrate (Sloan 1998;Longhi 2005), therefore CO 2 should rapidly interact with H 2 O molecules to form clathrate hydrate. Clathrate hydrates are non-stoichiometric compounds consisting of hydrogen-bonded H 2 O molecules forming cage-like structures in which guest gas molecules, such as CO 2 , can be trapped (Sloan 1998).…”

Section: The Fate Of Buried Comentioning

confidence: 99%

Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets

Turbet

Bolmont

Leconte

et al. 2018

A&A

171

268

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TRAPPIST-1 planets are invaluable for the study of comparative planetary science outside our Solar System and possibly habitability. Both Time Transit Variations (TTV) of the planets and the compact, resonant architecture of the system suggest that TRAPPIST-1 planets could be endowed with various volatiles today. First, we derive from N-body simulations possible planetary evolution scenarios, and show that all the planets are likely in synchronous rotation. We then use a versatile 3-D Global Climate Model (GCM) to explore the possible climates of cool planets around cool stars, with a focus on the TRAPPIST-1 system. We look at the conditions required for cool planets to prevent possible volatile species to be lost permanently by surface condensation, irreversible burying or photochemical destruction. We also explore the resilience of the same volatiles (when in condensed phase) to a runaway greenhouse process. We find that background atmospheres made of N 2 , CO or O 2 are rather resistant to atmospheric collapse. However, even if TRAPPIST-1 planets were able to sustain a thick background atmosphere by surviving early X/UV radiation and stellar wind atmospheric erosion, it is difficult for them to accumulate significant greenhouse gases like CO 2 , CH 4 or NH 3 . CO 2 can easily condense on the permanent nightside, forming CO 2 ice glaciers that would flow toward the substellar region. A complete CO 2 ice surface cover is theoretically possible on TRAPPIST-1g and h only, but CO 2 ices should be gravitationally unstable and get buried beneath the water ice shell in geologically short timescales. Given TRAPPIST-1 planets large EUV irradiation (at least ∼ 10 3 × Titan's flux), CH 4 and NH 3 are photodissociated rapidly and are thus hard to accumulate in the atmosphere. Photochemical hazes could then sedimentate and form a surface layer of tholins that would progressively thicken over the age of the TRAPPIST-1 system. Regarding habitability, we confirm that few bars of CO 2 would suffice to warm the surface of TRAPPIST-1f and g above the melting point of water. We also show that TRAPPIST-1e is a remarkable candidate for surface habitability. If the planet is today synchronous and abundant in water, then it should always sustain surface liquid water at least in the substellar region, whatever the atmosphere considered.

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“…Moreover, inclusions with liquid phase CO 2 at room temperature need to be cooled down to separate the liquid and vapor CO 2 phases in order to obtain T h . Inclusions with high CO 2 densities (i.e., >0.9 g/cm 3 ) will form CO 2 clathrate at low temperatures (Longhi, 2005;Sun and Duan, 2005), which will affect the accuracy of CO 2 density values derived from T h measurements. However, the micro-Raman density determinations can be applied to fluid inclusions slightly larger than the spatial resolution of Raman spectroscopy ($1 lm) with Table 6 The variation of CO 2 Fermi diad split for (a) natural CO 2 -rich carbonic-aqueous fluid inclusion and ( 11.…”

Section: D-q Relation In Co 2 Mixturesmentioning

confidence: 99%