Observation and Parameterization of Broadband Sea Surface Albedo

Huang, Chuan Jiang; Chen, Siyu; Xue, Yuting; Guo, Jing

doi:10.1029/2018jc014444

Cited by 16 publications

(6 citation statements)

References 37 publications

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“…The sea surface albedo is another key parameter in climate systems. Based on about 5 months of in-situ observations, Huang et al (2019) found that albedo increases with the increase of winds or surface waves and decreased with increasing water vapor pressure at the sea surface, which is a process by means of which surface waves impact on air-sea heat fluxes. Li et al (2021) demonstrated another important wave-coupled mechanisms, this time in polar regions.…”

Section: Air-sea Heat Fluxmentioning

confidence: 99%

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Ocean Waves in Large‐Scale Air‐Sea Weather and Climate Systems

Babanin

2023

JGR Oceans

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Ocean surface gravity waves are mechanical water waves propagating along the sea interface, with heights from centimeters to more than 10 m. They are one of the most significant dynamic processes in the upper ocean which have received a lot of attention in the fluid mechanics and ocean science community, starting from Stokes (1847) and peaking about half a century ago (e.g., see Yuan and Huang (2012) for a review). When moderate-to-strong wind blows over the sea surface, most of the energy and momentum are first transported to surface waves, to support their growth (e.g., Kudryavtsev & Makin, 2001), before those are passed to the ocean through wave breaking and wave-turbulence interactions (Babanin, 2011). That is, the waves are the "sink" of the energy and momentum flux for the low atmosphere and the "source" for the upper ocean, and play an important role in redistribution of the air-sea energy and momentum fluxes at the space-time scale of the storms. Moreover, such energy and momentum balance is not quite dependent on the instantaneous and local wind, because the waves are integral of the wind over large scales. Furthermore, in large areas dominated by swells, the waves can be unrelated to the local wind altogether, and in fact can be responsible for generating the local winds (e.g., Hanley et al., 2010).

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Section: Air-sea Heat Fluxmentioning

confidence: 99%

“…Based on about 5 months of in‐situ observations, Huang et al. (2019) found that albedo increases with the increase of winds or surface waves and decreased with increasing water vapor pressure at the sea surface, which is a process by means of which surface waves impact on air‐sea heat fluxes. Li et al.…”

Section: Air‐sea Heat Fluxmentioning

confidence: 99%

Ocean Waves in Large‐Scale Air‐Sea Weather and Climate Systems

Babanin

2023

JGR Oceans

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“…This behavior is caused by the transition from a completely and continuously glaciated northern ocean, and a mostly open ocean. Oceans have a very low albedo even compared to Martian regolith (∼0.05 6 versus 0.215; see, e.g., Huang et al 2019, for data on the former), thus they contribute to warm up the planet. Since the ocean fraction is highest in the C0GN model, their effect is strongest.…”

Section: Dependence On Obliquitymentioning

confidence: 99%

Seasonal Thaws under Mid- to Low-pressure Atmospheres on Early Mars

Simonetti,

Vladilo,

Ivanovski

et al. 2023

ApJ

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Despite decades of scientific research on the subject, the climate of the first 1.5 Gyr of Mars' history has not been fully understood yet. Especially challenging is the need to reconcile the presence of liquid water for extended periods of time on the Martian surface with the comparatively low insolation received by the planet, a problem which is known as the Faint Young Sun paradox. In this paper, we use the Earth-like planet surface-temperature model (or ESTM), a latitudinal energy-balance model with enhanced prescriptions for meridional heat diffusion, and the radiative-transfer code EOS to investigate how seasonal variations of temperature can give rise to local conditions which are conducive to liquid-water runoffs. We include the effects of the Martian dichotomy, a northern ocean with either 150 or 550 m of global equivalent layer, and simplified CO2 or H2O clouds. We find that 1.3–2.0 bar CO2-dominated atmospheres can produce seasonal thaws due to inefficient heat redistribution, provided that the eccentricity and the obliquity of the planet are sufficiently different from zero. We also studied the impact of different values for the argument of perihelion. When local favorable conditions exist, they nearly always persist for >15% of the Martian year. These results are obtained without the need for additional greenhouse gases (e.g., H2, CH4) or transient heat-injecting phenomena (e.g., asteroid impacts, volcanic eruptions). A moderate amount (0.1%–1%) of CH4 significantly widens the parameter space region in which seasonal thaws are possible.

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“…The surface reflectivity of the oceans is modelled using empirical laws that take into account its dependence on 𝑍 and the fact that the water surface is not smooth. We compared previous algorithms published in the literature (Briegleb et al 1986;Enomoto 2007) with a recent set of measurements obtained at different values of 𝑍 (Huang et al 2019). The observational data (red dots in Fig.…”

Section: Ocean Albedomentioning

confidence: 99%

EOS-ESTM: a flexible climate model for habitable exoplanets

Biasiotti

Simonetti

Vladilo

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Rocky planets with temperate conditions provide the best chance for discovering habitable worlds and life outside the Solar System. In the last decades, new instrumental facilities and large observational campaigns have been driven by the quest for habitable worlds. Climate models aimed at studying the habitability of rocky planets are essential tools to pay off these technological and observational endeavours. In this context, we present EOS-ESTM, a fast and flexible model aimed at exploring the impact on habitability of multiple climate factors, including those unconstrained by observations. EOS-ESTM is built on ESTM, a seasonal-latitudinal energy balance model featuring an advanced treatment of the meridional and vertical transport. The novel features of EOS-ESTM include: (1) parameterizations for simulating the climate impact of oceans, land, ice, and clouds as a function of temperature and stellar zenith distance; (2) a procedure (EOS) for calculating the radiative transfer in atmospheres with terrestrial and non-terrestrial compositions illuminated by solar- and non-solar-type stars. By feeding EOS-ESTM with Earth’s stellar, orbital and planetary parameters we derive a reference model that satisfies a large number of observational constraints of the Earth’s climate system. Validation tests of non-terrestrial conditions yield predictions that are in line with comparable results obtained with a hierarchy of climate models. The application of EOS-ESTM to planetary atmospheres in maximum greenhouse conditions demonstrates the possibility of tracking the snowball transition at the outer edge of the HZ for a variety of planetary parameters, paving the road for multi-parametric studies of the HZ.

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Observation and Parameterization of Broadband Sea Surface Albedo

Cited by 16 publications

References 37 publications

Ocean Waves in Large‐Scale Air‐Sea Weather and Climate Systems

Ocean Waves in Large‐Scale Air‐Sea Weather and Climate Systems

Seasonal Thaws under Mid- to Low-pressure Atmospheres on Early Mars

EOS-ESTM: a flexible climate model for habitable exoplanets

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