Outgassing on stagnant-lid super-Earths

Dorn, Caroline; Noack, Lena; Rozel, Antoine

doi:10.1051/0004-6361/201731513

Cited by 90 publications

(150 citation statements)

References 95 publications

Supporting

Mentioning

139

Contrasting

Unclassified

Order By: Relevance

“…Stagnant lid planets still experience volcanism, which can release a significant amount of CO 2 to the atmosphere, as estimated in previous studies for Mars (e.g. Pollack et al 1987;O'Neill et al 2007;Grott et al 2011), a hypothetical stagnant lid Earth (Tosi et al 2017), and super-Earths (Noack et al 2017;Dorn et al 2018). Moreover, burial of carbonated crust under lava flows could lead to metamorphic decarbonation of this crust, providing an additional CO 2 source to the atmosphere, or recycling of surface CO 2 back into the mantle (e.g.…”

mentioning

confidence: 77%

Habitability of Earth-like Stagnant Lid Planets: Climate Evolution and Recovery from Snowball States

Foley

2019

ApJ

View full text Add to dashboard Cite

Coupled models of mantle thermal evolution, volcanism, outgassing, weathering, and climate evolution for Earth-like (in terms of size and composition) stagnant lid planets are used to assess their prospects for habitability. The results indicate that planetary CO 2 budgets ranging from ≈ 3 orders of magnitude lower than Earth's to ≈ 1 order of magnitude larger, and radiogenic heating budgets as large or larger than Earth's, allow for habitable climates lasting 1-5 Gyrs. The ability of stagnant lid planets to recover from potential snowball states is also explored; recovery is found to depend on whether atmosphere-ocean chemical exchange is possible. For a "hard" snowball with no exchange, recovery is unlikely, as most CO 2 outgassing takes place via metamorphic decarbonation of the crust, which occurs below the ice layer. However, for a "soft" snowball where there is exchange between atmosphere and ocean, planets can readily recover. For both hard and soft snowball states, there is a minimum CO 2 budget needed for recovery; below this limit any snowball state would be permanent. Thus there is the possibility for hysteresis in stagnant lid planet climate evolution, where planets with low CO 2 budgets that start off in a snowball climate will be permanently stuck in this state, while otherwise identical planets that start with a temperate climate will be capable of maintaining this climate for 1 Gyrs or more. Finally, the model results have important implications for future exoplanet missions, as they can guide observations to planets most likely to possess habitable climates.Subject headings: astrobiology -planets and satellites: physical evolutionplanets and satellites: terrestrial planets IntroductionDetermining the factors that allow long-lived, habitable climates to develop on rocky planets is a critical goal for astrobiology, especially in light of the large number of exoplanets

show abstract

mentioning

confidence: 77%

Habitability of Earth-like Stagnant Lid Planets: Climate Evolution and Recovery from Snowball States

Foley

2019

ApJ

View full text Add to dashboard Cite

show abstract

“…However, the amount of outgasing also depends on the mass of the planet. The highest level is expected for planets with masses between 2-3 M⊕ (Dorn et al 2018 (Brown & Chaffee 1945;Brown et al 1975;Brown 1976;Brown &Shemansky 1982;Morgan & Pilcher 1982;Thomas 1993Thomas , 1996Küppers & Jockers 1995, 1997Kupo et al 1976).…”

Section: Introductionmentioning

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

View full text Add to dashboard Cite

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.

show abstract

“…Habitable zone (HZ) small-radius exoplanets are common (Burke et al 2015;Dressing & Charbonneau 2015). What fraction of them are habitable?…”

mentioning

confidence: 99%

Habitability of Exoplanet Waterworlds

Kite

Ford

2018

ApJ

View full text Add to dashboard Cite

Many habitable zone (HZ) exoplanets are expected to form with water mass fractions higher than that of the Earth. For rocky exoplanets with 10-1000× Earth's H 2 O but without H 2 , we model the multi-Gyr evolution of ocean temperature and chemistry, taking into account C partitioning, high-pressure ice phases, and atmosphere-lithosphere exchange. Within our model, for Sun-like stars, we find that:(1) the duration of habitable surface water is strongly affected by ocean chemistry; (2) possible ocean pH spans a wide range; (3) surprisingly, many waterworlds retain habitable surface water for >1 Gyr, and (contrary to previous claims) this longevity does not necessarily involve geochemical cycling.The key to this cycle-independent planetary habitability is that C exchange between the convecting mantle and the water ocean is curtailed by seafloor pressure on waterworlds, so the planet is stuck with the ocean mass and ocean cations that it acquires during the first 1% of its history. In our model, the sum of positive charges leached from the planetary crust by early water-rock interactions is -coincidentally -often within an order of magnitude of the early-acquired atmosphere+ocean inorganic C inventory overlaps. As a result, p CO2 is frequently in the "sweet spot" (0.2-20 bar) for which the range of semimajor axis that permits surface liquid water is about as wide as it can be. Because the width of the HZ in semimajor axis defines (for Sun-like stars) the maximum possible time span of surface habitability, this effect allows for Gyr of habitability as the star brightens. We illustrate our findings by using the output of an ensemble of N -body simulations as input to our waterworld evolution code. Thus (for the first time in an end-to-end calculation) we show that chance variation of initial conditions, with no need for geochemical cycling, can yield multi-Gyr surface habitability on waterworlds.

show abstract

Outgassing on stagnant-lid super-Earths

Cited by 90 publications

References 95 publications

Habitability of Earth-like Stagnant Lid Planets: Climate Evolution and Recovery from Snowball States

Habitability of Earth-like Stagnant Lid Planets: Climate Evolution and Recovery from Snowball States

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

Habitability of Exoplanet Waterworlds

Contact Info

Product

Resources

About