The circulation pattern and day-night heat transport in the atmosphere of a synchronously rotating aquaplanet: Dependence on planetary rotation rate

Noda, S.; Ishiwatari, Masaki; Nakajima, Kensuke; Takahashi, Yoshiyuki O.; Takehiro, Shin‐ichi; Onishi, Masanori; Hashimoto, George L.; Kuramoto, Kiyoshi; Hayashi, Yoshiyuki

doi:10.1016/j.icarus.2016.09.004

Cited by 84 publications

(104 citation statements)

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“…Using a present-day Earth GCM, Edson et al (2011) noted that this definition requires that slow rotators must have a rotational period of ∼ 5 days or greater, for an Earth-size planet in synchronous orbit around a Gdwarf star. Other studies using more idealized GCMs (Carone et al 2014(Carone et al , 2015(Carone et al , 2016Noda et al 2017) have found comparable values for this limit on slow rotators. All planets in our set of simulations have a rotation period greater than 5 days, except for planets orbiting a 2600 K host star.…”

Section: Slow Rotatorsmentioning

confidence: 64%

“…4). Rapid rotators tend to show banded cloud formation beneath the substellar point Kopparapu et al 2016) and a mean zonal circulation that only partially reaches from day to night side (Haqq-Misra & Kopparapu 2015; Kopparapu et al 2017) Rapid rotators are comparable to the 'Type-IV' circulation regime described by Noda et al (2017), with some dynamical features that resemble present-day Earth.…”

Section: Rapid Rotatorsmentioning

confidence: 99%

“…Atmospheric dynamics on a slow rotator are broadly characterized by a thermally-direct circulation with heating and rising air on the day side, cooling and descending air on the night side, and the strength of the circulation limited by frictional dissipation in the boundary layer (Koll & Abbot 2016). Slow rotators are equivalent to the 'Type-I' circulation regime described by Noda et al (2017), where the thermally-direct day-night circulation is the primary characteristic of the planet's large-scale dynamics.…”

Section: Slow Rotatorsmentioning

confidence: 99%

“…But subsequent investigations with simplified climate models (Haberle et al 1996) and general circulation models (GCMs) (Joshi et al 1997;Joshi 2003;Merlis & Scheider 2010;Edson et al 2011;Showman et al 2010Showman et al , 2013Leconte et al 2013;Yang et al 2013Cullum et al 2014;Hu & Yang 2014;Carone et al 2014Carone et al , 2015Carone et al , 2016Wordsworth 2015;Way et al 2016;Kopparapu et al 2016Kopparapu et al , 2017Noda et al 2017;Fujii et al 2017) have demonstrated that energy transport from the day to night hemisphere is generally sufficient to avoid atmospheric collapse across a wide range of atmospheric compositions and rotation periods.…”

Section: Introductionmentioning

confidence: 99%

“…Further analysis has revealed common patterns in the large-scale dynamics of synchronously rotating terrestrial planets, most notably a transition between circulation regimes as a planet's rotation period decreases and the Rossby deformation radius approaches planetary radius (Merlis & Scheider 2010;Edson et al 2011;Showman et al 2010Showman et al , 2013Leconte et al 2013;Yang et al 2013Haqq-Misra & Kopparapu 2015;Carone et al 2014Carone et al , 2015Carone et al , 2016Noda et al 2017). For an Earthsize synchronously rotating planet, this transition occurs at a rotation period of ∼5 days (Edson et al 2011;Carone et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Demarcating Circulation Regimes of Synchronously Rotating Terrestrial Planets within the Habitable Zone

Haqq-Misra

Wolf

Joshi

et al. 2018

ApJ

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We investigate the atmospheric dynamics of terrestrial planets in synchronous rotation within the habitable zone of low-mass stars using the Community Atmosphere Model (CAM). The surface temperature contrast between day and night hemispheres decreases with an increase in incident stellar flux, which is opposite the trend seen on gas giants. We define three dynamical regimes in terms of the equatorial Rossby deformation radius and the Rhines length. The slow rotation regime has a mean zonal circulation that spans from day to night side, with both the Rossby deformation radius and the Rhines length exceeding planetary radius, which occurs for planets around stars with effective temperatures of 3300 K to 4500 K (rotation period > 20 days). Rapid rotators have a mean zonal circulation that partially spans a hemisphere and with banded cloud formation beneath the substellar point, with the Rossby deformation radius is less than planetary radius, which occurs for planets orbiting stars with effective temperatures of less than 3000 K (rotation period < 5 days). In between is the Rhines rotation regime, which retains a thermally-direct circulation from day to night side but also features midlatitude turbulence-driven zonal jets. Rhines rotators occur for planets around stars in the range of 3000 K to 3300 K (rotation period ∼ 5 to 20 days), where the Rhines length is greater than planetary radius but the Rossby deformation radius is less than planetary radius. The dynamical state can be observationally inferred from comparing the morphology of the thermal emission phase curves of synchronously rotating planets.

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