Parameterization of radiative heating and cooling rates in the stratosphere of Jupiter

Kuroda, Takeshi; Medvedev, Alexander S.; Hartogh, P.

doi:10.1016/j.icarus.2014.08.001

Cited by 17 publications

(46 citation statements)

References 46 publications

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“…( 2) where P is the photospheric pressure, g is gravity, c p is the specific heat at constant pressure, σ is Stefan-Boltzmann constant, and T is temperature. Inserting appropriate values for Jupiter (P ∼ 0.5 bar, c p = 1.3 × 10 4 J kg −1 K −1 , g = 23 m s −1 and T = 130 K) yields τ rad ≈ 6 × 10 7 s. This is similar to values estimated from sophisticated radiative transfer calculations, which indicate that τ rad ranges between 10 8 and 10 7 s from 1 bar to 1 mbar (Kuroda et al 2014;Li et al 2018). At the higher temperatures of brown dwarfs, however, the above scaling predicts much shorter radiative time constants in the range ∼10 4 -10 5 s (see Robinson & Marley 2014).…”

Section: Modelsupporting

confidence: 77%

Atmospheric Circulation of Brown Dwarfs and Jupiter- and Saturn-like Planets: Zonal Jets, Long-term Variability, and QBO-type Oscillations

Showman

Tan²,

Zhang

2019

ApJ

125

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Brown dwarfs and directly imaged giant planets exhibit significant evidence for active atmospheric circulation, which induces a large-scale patchiness in the cloud structure that evolves significantly over time, as evidenced by infrared light curves and Doppler maps. These observations raise critical questions about the fundamental nature of the circulation, its time variability, and the overall relationship to the circulation on Jupiter and Saturn. Jupiter and Saturn themselves exhibit numerous robust zonal (east-west) jet streams at the cloud level; moreover, both planets exhibit long-term stratospheric oscillations involving perturbations of zonal wind and temperature that propagate downward over time on timescales of ∼4 years (Jupiter) and ∼15 years (Saturn). These oscillations, dubbed the Quasi Quadrennial Oscillation (QQO) for Jupiter and the Semi-Annual Oscillation (SAO) on Saturn, are thought to be analogous to the Quasi-Biennial Oscillation (QBO) on Earth, which is driven by upward propagation of equatorial waves from the troposphere. To investigate these issues, we here present global, three-dimensional, high-resolution numerical simulations of the flow in the stratified atmosphere-overlying the convective interior-of brown dwarfs and Jupiter-like planets. The effect of interior convection is parameterized by inducing small-scale, randomly varying perturbations in the radiative-convective boundary at the base of the model. Radiative damping is represented using an idealized Newtonian cooling scheme. In the simulations, the convective perturbations generate atmospheric waves and turbulence that interact with the rotation to produce numerous zonal jets. Moreover, the equatorial stratosphere exhibits stacked eastward and westward jets that migrate downward over time, exactly as occurs in the terrestrial QBO, Jovian QQO, and Saturnian SAO. This is the first demonstration of a QBO-like phenomenon in 3D numerical simulations of a giant planet.

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Section: Modelsupporting

confidence: 77%

Atmospheric Circulation of Brown Dwarfs and Jupiter- and Saturn-like Planets: Zonal Jets, Long-term Variability, and QBO-type Oscillations

Showman

Tan²,

Zhang

2019

ApJ

125

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“…The entire solar and infrared spectra are divided into 15 bands according to the absorption bands for CH4, C2H2 and C2H6. The wavenumber range and the dominant absorber in each band is described in Kuroda, Medvedev [9], with spectral resolution of 0.01 cm -1 . We have considered the absorptions and emissions by CH4, C2H2, C2H6, NH3, PH3 and the collision-induced absorptions by H2-H2 and H2-He [15].…”

Section: Heating Rates and Radiative Time Constants On Giant Planetsmentioning

confidence: 99%

A high-performance atmospheric radiation package: With applications to the radiative energy budgets of giant planets

Zhang

et al. 2018

Journal of Quantitative Spectroscopy and Radiative Transfer

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A High-performance Atmospheric Radiation Package (HARP) is developed for studying multiplescattering planetary atmospheres. HARP is an open-source program written in C++ that utilizes high-level data structure and parallel-computing algorithms. It is generic in three aspects. First, the construction of the model atmospheric profile is generic. The program can either take in an atmospheric profile or construct an adiabatic thermal and compositional profile, taking into account the clouds and latent heat release due to condensation. Second, the calculation of opacity is generic, based on line-by-line molecular transitions and tabulated continuum data, along with a table of correlated-k opacity provided as an option to speed up the calculation of energy fluxes. Third, the selection of the solver for the radiative transfer equation is generic.The solver is not hardwired in the program. Instead, based on the purpose, a variety of radiative transfer solvers can be chosen to couple with the atmosphere model and the opacity model.We use the program to investigate the radiative heating and cooling rates of all four giant planets in the Solar System. Our Jupiter's result is consistent with previous publications. Saturn has nearly perfect balance between the heating rate and cooling rate. Uranus has the least radiative fluxes because of the lack of CH4 and its photochemical products. Both Uranus and Neptune suffer from a severe energy deficit in their stratospheres. Possible ways to resolve this issue are discussed. Finally, we recalculate the radiative time constants of all four giant planet atmospheres and find that the traditional values from (Conrath BJ, Gierasch PJ, Leroy SS. Temperature and Circulation in the Stratosphere of the Outer Planets. Icar. 1990;83:255-81) are significantly overestimated.

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“…В годы возле широких минимумов СА (1964-1966, 1975-1977.5, 1984.7-1987.5, 1995.8-1997.5, 2006- То есть в 1963-1995 гг. корреляция межу изменениями фактора A J , солнечной активностью и мо- 30 Видьмаченко А.П.…”

Section: активность процессов в атмосфереunclassified

“…Одна из гипотез прямого воздействия опирается на особенности процесса фазовых переходов для разных химических элементов в атмосферах планет (например, воды в атмосфере Земли, метана и аммиака и их производных в атмосферах Юпитера и Сатурна [30,35,74,87,100,111]). Поэтому проявление солнечной активности в атмосферах следует искать, прежде всего, в тех длинах волн, где проявляется образующаяся в атмосферах планет-гигантов дымка из активных для данной атмосферы составляющих (продукты фотолиза метана, аммиака и пр.).…”

Section: воздействие излучения солнца на атмосферуunclassified

Periodic changes of the activity of processes in Jupiter's atmosphere

Vidmachenko

2016

AstSR

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Главная астрономическая обсерватория НАН Украины Вариации йовимагнитной широты Земли на Юпитере будут предпочтительными при солнечно-обусловленных изменениях отражательных свойств облаков и дымки. Из-за наличия эксцентриситета орбиты (e =0,04845) северное полушарие получает на 21% больший приток солнечной энергии к атмосфере, поскольку в близкий к летнему солнцестоянию момент Юпитер находится в перигелии. Результаты наших исследований показали, что отношение яркости северной и южной тропических и умеренных поясов является наглядным фактором фотометрической активности процессов в атмосфере Юпитере. Полученное из анализа наблюдательных данных за период с 1962 по 2015 год существование цикличности в изменении фактора активности полушарий планеты с периодом около 11,86 лет говорит о наличии сезонной перестройки физических параметров атмосферы Юпитера. ПЕРIОДИЧНI ЗМIНИ АКТИВНОСТI ПРОЦЕСIВ В АТМОСФЕРI ЮПIТЕРА, Вiдьмаченко А.П.-Варiацiї йовiмагнiтної широти Землi на Юпiтерi є кращими для сонячно-обумовлених змiн вiдбивних властивостей хмар i надхмарового туману. Через наявнiсть ексцентриситету орбiти (e =0,048450) пiвнiчна пiвкуля отримує на 21% бiльший приплив сонячної енергiї до атмосфери, оскiльки в близький до лiтнього сонцестояння момент Юпiтер знаходиться в перигелiї. Результати наших дослiджень показали, що вiдношення яскравостi пiвнiчної i пiвденної тропiчних i помiрних поясiв є наочним фактором фотометричної активностi атмосферних процесiв на Юпiтерi. Отримане з аналiзу спостережних даних за перiод з 1962 по 2015 рiк iснування циклiчностi у змiнi фактора активностi пiвкуль планети з перiодом близько 11,86 рокiв говорить про iснування сезонної перебудови фiзичних параметрiв атмосфери Юпiтера.

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Parameterization of radiative heating and cooling rates in the stratosphere of Jupiter

Cited by 17 publications

References 46 publications

Atmospheric Circulation of Brown Dwarfs and Jupiter- and Saturn-like Planets: Zonal Jets, Long-term Variability, and QBO-type Oscillations

Atmospheric Circulation of Brown Dwarfs and Jupiter- and Saturn-like Planets: Zonal Jets, Long-term Variability, and QBO-type Oscillations

A high-performance atmospheric radiation package: With applications to the radiative energy budgets of giant planets

Periodic changes of the activity of processes in Jupiter's atmosphere

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