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Donald M. Hunten

NOVEMBER 1973 D O N A L D M. H U N T E N 1481The Escape of Light Gases from Planetary Atmospheres DONALD M. I-IuNTEN Kitt Peak National Observatory, Tucson, Ariz. 85717(Manuscript received 11 May 1973, in revised form 16 July 1973)ABSTRACT The Jeans-Spitzer treatment of atmospheric escape by evaporation must be supplemented, for a mixtureof gases, by a discussion of the mutual

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L. V. Berkner and L. C. Marshall

VOL. 23, NO. 2 JOURNAL OF THE ATMOSPHERIC SCIENCES MARCH 1966Limitation on Oxygen Concentration in a Primitive Planetary Atmosphere~ L. Vo BERKNER AND L. C. MARSHALLSouthwest Center for Advanced Studies, Dallas, Texas(Manuscript received 23 August 1965, in revised form 27 September 1965)ABSTRACT The absorption of ultraviolet radiation across the dissociative band (1500-2100 .~) is computed for thethree component

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Stephen I. Thomson and Michael E. McIntyre

. Fluid Mech. , 181 , 527 – 565 , doi: 10.1017/S0022112087002209 . Pierrehumbert , R. T. , 2010 : Principles of Planetary Climate. Cambridge University Press, 652 pp . Porco , C. C. , and Coauthors , 2003 : Cassini imaging of Jupiter’s atmosphere, satellites, and rings . Science , 299 , 1541 – 1547 , doi: 10.1126/science.1079462 . Read , P. L. , P. J. Gierasch , B. J. Conrath , A. Simon-Miller , T. Fouchet , and Y. H. Yamazaki , 2006 : Mapping potential

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Y. T. Chiu and J. M. Straus

Ma-1974 Y.T. CHIU AND J. M. STRAUS 1109The Structure of Planetary Waves in the Auroral Region Upper Atmosphere~ Y. T. Catu ^t~r) J. M. STItAUSSpace Physics Laboratory, The Aerospace Corporation, El Segundo, Calif. 90245(Manuscript received 26 September 1973, in revised form 30 January 1974)ABSTRACT Invoking recent satellite observations of the planetary-scale variations of auroral

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by applying the well-1B. A. A. 8. Nottingham Report, p. 682, 1893..--established laws of the kinetic theory to the problem, and hispaper On the escape of gases from planetary atmospheresaccording to the kinetic theory appeared in the Astrophys-ical Journal for January, 1900. Contemporaneous with thepublication of this paper Dr. (3. H. Bryan read a paper on theIC Kinetic theory of planetary atmospheres before the RoyalSociety. This paper apIfeared in the Transactions of theRoyal Society, London

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G. E. Hunt and I. P. Grant

SEPTEMBER 1969 G. E. H U N T A N D I. P. G RAN T 963Discrete Space Theory of Radiative Transfer and its Application to Problems in Planetary Atmospheres G. E. HUNT AND L P. GRANTScience l~esearch Council, Atlas Computer Laboratory, Chilton, Didcot, Berkshire, England (Marmscript received 9 May 1969, in revised form 13 June ~969)ABSTRACT The classical methods that have been devised to

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. INTRODUCTIONThe vertical motions at the earth's surface associatedwith horizontal adow over the mountain ranges are ofimportance both for their direct effect on local climate (e.g.,adiaba:ic warming and cooling with accompanyingcloud aud precipitation formation) and for their indirecteffect on planetary climate by the forcing of stationarywave systems (e.g., Charney and Eliassen 1949). Thisvertical motion is given bywhere V is the vector horizontal wind of which u is theeastward component and v is the

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David M. Romps

1. Introduction To motivate the study of the entropy budget, consider first an enclosed, dry atmosphere. For an enclosed atmosphere in a steady state, the sum of all the entropy sources must be zero (here, “sources” is shorthand for sources and sinks). In the case of an enclosed, dry atmosphere, all of the entropy sources are simply heat sources divided by the temperature. For example, possible heat sources include radiation ( Q ), conduction of heat (− ∇ · J , where J is the conductive

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Raj K. Rai, Larry K. Berg, Branko Kosović, Sue Ellen Haupt, Jeffrey D. Mirocha, Brandon L. Ennis, and Caroline Draxl


Coupled mesoscale–microscale simulations are required to provide time-varying weather-dependent inflow and forcing for large-eddy simulations under general flow conditions. Such coupling necessarily spans a wide range of spatial scales (i.e., ~10 m to ~10 km). Herein, we use simulations that involve multiple nested domains with horizontal grid spacings in the terra incognita (i.e., km) that may affect simulated conditions in both the outer and inner domains. We examine the impact on simulated wind speed and turbulence associated with forcing provided by a terrain with grid spacing in the terra incognita. We perform a suite of simulations that use combinations of varying horizontal grid spacings and turbulence parameterization/modeling using the Weather Research and Forecasting (WRF) Model using a combination of planetary boundary layer (PBL) and large-eddy simulation subgrid-scale (LES-SGS) models. The results are analyzed in terms of spectral energy, turbulence kinetic energy, and proper orthogonal decomposition (POD) energy. The results show that the output from the microscale domain depends on the type of turbulence model (e.g., PBL or LES-SGS model) used for a given horizontal grid spacing but is independent of the horizontal grid spacing and turbulence modeling of the parent domain. Simulation using a single domain produced less POD energy in the first few modes compared to a coupled simulation (one-way nesting) for similar horizontal grid spacing, which highlights that coupled simulations are required to accurately pass the mesoscale features into the microscale domain.

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H. L. Kuo

1973 H. L. KUO 53Planetary Boundary Layer Flow of a Stable Atmosphere Over the Globe H. L. KuoDept. of the Geophysical Sciences, The Uni*ersity of Chicago 60637(Manuscript received 19 April 1972, in revised form 18 September 1972)ABSTRACT When the temperature and pressure perturbations are taken into consideration in the boundary layerequations, the stable

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