Ocean Dynamics and the Inner Edge of the Habitable Zone for Tidally Locked Terrestrial Planets

Yang, Jun; Abbot, Dorian S.; Koll, Daniel D. B.; Hu, Yongyun; Showman, Adam P.

doi:10.3847/1538-4357/aaf1a8

Cited by 73 publications

(76 citation statements)

References 76 publications

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“…All the experiments are started from an ice-free state. Tests showed that the final equilibrium states do not depend on the initial state 83 . For tidally locked planets, there is nearly no climate bistability or hysteresis 28 .…”

Section: Continents Can Influence the Open Ocean Area For Example Amentioning

confidence: 99%

“…1 except that the ratio of orbital period to rotation period is 3:2, rather than 1:1 (Supplementary Table 2 41,71 . We have modified the model to simulate the climates of tidally locked terrestrial planets in the habitable zone of low-mass stars 17,20,83,84 . The model includes four components-atmosphere, ocean, sea ice, and land, and one coupler is used to connect them.…”

Section: Continents Can Influence the Open Ocean Area For Example Amentioning

confidence: 99%

“…Supplementary Information for the paper "Transition from Eyeball to Snowball Driven by Sea-ice Drift on Tidally Locked Terrestrial Planets" by Jun Yang et al, 2019 Contents:…”

Section: Planetary Properties Supplementarymentioning

confidence: 99%

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Transition from eyeball to snowball driven by sea-ice drift on tidally locked terrestrial planets

Yang

Zeng

2019

Nat Astron

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Tidally locked terrestrial planets around low-mass stars are the prime targets for future atmospheric characterizations of potentially habitable systems 1 , especially the three nearby ones-Proxima b 2 , TRAPPIST-1e 3 , and LHS 1140b 4 . Previous studies suggest that if these planets have surface ocean they would be in an eyeball-like climate state 5-10 : ice-free in the vicinity of the substellar point and ice-covered in the rest regions. However, an important component of the climate system-sea ice dynamics has not been well studied in previous studies. A fundamental question is: would the open ocean be stable against a globally ice-covered snowball state? Here we show that sea-ice drift cools the ocean's surface when the ice flows to the warmer substellar region and melts through absorbing heat from the ocean and the overlying air. As a result, the open ocean shrinks and can even disappear when atmospheric greenhouse gases are not much more abundant than on Earth, turning the planet into a snowball state. This occurs for both synchronous rotation and spinorbit resonances (such as 3:2). These results suggest that sea-ice drift strongly reduces the open ocean area and can significantly impact the habitability of tidally locked planets.

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Section: Continents Can Influence the Open Ocean Area For Example Amentioning

confidence: 99%

Section: Continents Can Influence the Open Ocean Area For Example Amentioning

confidence: 99%

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Transition from eyeball to snowball driven by sea-ice drift on tidally locked terrestrial planets

Yang

Zeng

2019

Nat Astron

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“…Such a scenario is discussed by Yang et al [2014] (see also Menou, 2013;Leconte et al, 2013;Turbet et al, 2016), but ROCKE-3D both lacks a dynamic land ice model that accounts for the glacial flow that could possibly replenish the dayside with water (to some degree) and the duration of simulation time necessary to largely evacuate the Pacific Ocean is well beyond reasonable simulation run durations. The tidally-locked/sun-synchronous 365x simulations produce familiar patterns [Yang et al, 2013;2014b;2019a;2019b;Kopparapu et al, 2017;Fauchez et al, 2019] of a very thick sub-stellar cloud, primarily composed of ice particles at high altitudes (Figure 3 ), that is not perfectly round but instead modulated by the presence of continents and a dynamical ocean transporting heat poleward.…”

Section: Simulated Climate and Atmospheric Dynamicsmentioning

confidence: 99%

“…Wordsworth et al, 2011; Abe et al, 2011; Pierrehumbert, 2011; Selsis et al, 2011; Leconte et al, 2013; Wang et al,. 2014; Yang et al, 2014a, 2014b; Shields et al, 2013, 2016; Koll & Abbot, 2015; Wordsworth et al, 2015; Pierrehumbert & Ding, 2016; Bolmont et al, 2016; Way et al, 2016, 2018; Popp et al, 2016; Wolf et al, 2017; Kopparapu et al, 2017; Turbet et al, 2016; 2017; Boutle et al, 2017; Fujii et al, 2017; HaqqMisra et al, 2018; Kodama et al, 2018; Del Genio et al, 2019; Jansen et al, 2019Yang et al, 2019a). However, the climate of planets depend on many parameters, including the total stellar irradiation, the atmospheric composition, the volatile inventory, the planetary rotation rate, the surface properties, and the presence of clouds or hazes [Forget & Leconte, 2014].…”

Section: Introductionmentioning

confidence: 99%

The Impact of Planetary Rotation Rate on the Reflectance and Thermal Emission Spectrum of Terrestrial Exoplanets around Sunlike Stars

Guzewich

Lustig‐Yaeger

Davis

et al. 2020

ApJ

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Robust atmospheric and radiative transfer modeling will be required to properly interpret reflected light and thermal emission spectra of terrestrial exoplanets. This will help break observational degeneracies between the numerous atmospheric, planetary, and stellar factors that drive planetary climate. Here we simulate the climates of Earth-like worlds around the Sun with increasingly slow rotation periods, from Earth-like to fully Sun-synchronous, using the ROCKE-3D general circulation model. We then provide these results as input to the Spectral Planet Model (SPM), which employs the SMART radiative transfer model to simulate the spectra of a planet as it would be observed from a future space-based telescope. We find that the primary observable effects of slowing planetary rotation rate are the altered cloud distributions, altitudes, and opacities which subsequently drive many changes to the spectra by altering the absorption band depths of biologically-relevant gas species (e.g., H2O, O2, and O3). We also identify a potentially diagnostic feature of synchronously rotating worlds in mid-infrared H2O absorption/emission lines.

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Superrotation in Planetary Atmospheres

et al. 2020

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Superrotation is a dynamical regime where the atmosphere circulates around the planet in the direction of planetary rotation with excess angular momentum in the equatorial region. Superrotation is known to exist in the atmospheres of Venus, Titan, Jupiter, and Saturn in the solar system. Some of the exoplanets also exhibit superrotation. Our understanding of superrotation in a framework of circulation regimes of the atmospheres of terrestrial planets is in progress thanks to the development of numerical models; a global instability involving planetary-scale waves seems to play a key role, and the dynamical state depends on the Rossby number, a measure of the relative importance of the inertial and Coriolis forces, and the thermal inertia of the atmosphere. Recent general circulation models of Venus's and Titan's atmospheres demonstrated the importance of horizontal waves in the angular momentum transport in these atmospheres and also an additional contribution of thermal tides in Venus's atmosphere. The atmospheres of Jupiter and Saturn also exhibit strong superrotation. Recent gravity data suggests that these superrotational flows extend deep into the planet, yet currently no single mechanism has been identified as driving this superrotation. Moreover, atmospheric circulation models of tidally locked, strongly Understanding the Diversity of Planetary Atmospheres Edited by François Forget,

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Ocean Dynamics and the Inner Edge of the Habitable Zone for Tidally Locked Terrestrial Planets

Cited by 73 publications

References 76 publications

Transition from eyeball to snowball driven by sea-ice drift on tidally locked terrestrial planets

Transition from eyeball to snowball driven by sea-ice drift on tidally locked terrestrial planets

The Impact of Planetary Rotation Rate on the Reflectance and Thermal Emission Spectrum of Terrestrial Exoplanets around Sunlike Stars

Superrotation in Planetary Atmospheres

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