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Understanding Eddy Field in the Arctic Ocean from High-Resolution Satellite Observations Igor Kozlov1, A
Abstract ID: 21849 Understanding eddy field in the Arctic Ocean from high-resolution satellite observations Igor Kozlov1, A. Artamonova1, L. Petrenko1, E. Plotnikov1, G. Manucharyan2, A. Kubryakov1 1Marine Hydrophysical Institute of RAS, Russia; 2School of Oceanography, University of Washington, USA Highlights: - Eddies are ubiquitous in the Arctic Ocean even in the presence of sea ice; - Eddies range in size between 0.5 and 100 km and their orbital velocities can reach up to 0.75 m/s. - High-resolution SAR data resolve complex MIZ dynamics down to submesoscales [O(1 km)]. Fig 1. Eddy detection Fig 2. Spatial statistics Fig 3. Dynamics EGU2020 OS1.11: Changes in the Arctic Ocean, sea ice and subarctic seas systems: Observations, Models and Perspectives 1 Abstract ID: 21849 Motivation • The Arctic Ocean is a host to major ocean circulation systems, many of which generate eddies transporting water masses and tracers over long distances from their formation sites. • Comprehensive observations of eddy characteristics are currently not available and are limited to spatially and temporally sparse in situ observations. • Relatively small Rossby radii of just 2-10 km in the Arctic Ocean (Nurser and Bacon, 2014) also mean that most of the state-of-art hydrodynamic models are not eddy-resolving • The aim of this study is therefore to fill existing gaps in eddy observations in the Arctic Ocean. • To address it, we use high-resolution spaceborne SAR measurements to detect eddies over the ice-free regions and in the marginal ice zones (MIZ). EGU20 -OS1.11 – Kozlov et al., Understanding eddy field in the Arctic Ocean from high-resolution satellite observations 2 Abstract ID: 21849 Methods • We use multi-mission high-resolution spaceborne synthetic aperture radar (SAR) data to detect eddies over open ocean and marginal ice zones (MIZ) of Fram Strait and Beaufort Gyre regions. -
Rossby Number Similarity of Atmospheric RANS Using Limited
https://doi.org/10.5194/wes-2019-74 Preprint. Discussion started: 21 October 2019 c Author(s) 2019. CC BY 4.0 License. Rossby number similarity of atmospheric RANS using limited length scale turbulence closures extended to unstable stratification Maarten Paul van der Laan1, Mark Kelly1, Rogier Floors1, and Alfredo Peña1 1Technical University of Denmark, DTU Wind Energy, Risø Campus, Frederiksborgvej 399, 4000 Roskilde, Denmark Correspondence: Maarten Paul van der Laan ([email protected]) Abstract. The design of wind turbines and wind farms can be improved by increasing the accuracy of the inflow models repre- senting the atmospheric boundary layer. In this work we employ one-dimensional Reynolds-averaged Navier-Stokes (RANS) simulations of the idealized atmospheric boundary layer (ABL), using turbulence closures with a length scale limiter. These models can represent the mean effects of surface roughness, Coriolis force, limited ABL depth, and neutral and stable atmo- 5 spheric conditions using four input parameters: the roughness length, the Coriolis parameter, a maximum turbulence length, and the geostrophic wind speed. We find a new model-based Rossby similarity, which reduces the four input parameters to two Rossby numbers with different length scales. In addition, we extend the limited length scale turbulence models to treat the mean effect of unstable stratification in steady-state simulations. The original and extended turbulence models are compared with historical measurements of meteorological quantities and profiles of the atmospheric boundary layer for different atmospheric 10 stabilities. 1 Introduction Wind turbines operate in the turbulent atmospheric boundary layer (ABL) but are designed with simplified inflow conditions that represent analytic wind profiles of the atmospheric surface layer (ASL). -
The General Circulation of the Atmosphere and Climate Change
12.812: THE GENERAL CIRCULATION OF THE ATMOSPHERE AND CLIMATE CHANGE Paul O'Gorman April 9, 2010 Contents 1 Introduction 7 1.1 Lorenz's view . 7 1.2 The general circulation: 1735 (Hadley) . 7 1.3 The general circulation: 1857 (Thompson) . 7 1.4 The general circulation: 1980-2001 (ERA40) . 7 1.5 The general circulation: recent trends (1980-2005) . 8 1.6 Course aim . 8 2 Some mathematical machinery 9 2.1 Transient and Stationary eddies . 9 2.2 The Dynamical Equations . 12 2.2.1 Coordinates . 12 2.2.2 Continuity equation . 12 2.2.3 Momentum equations (in p coordinates) . 13 2.2.4 Thermodynamic equation . 14 2.2.5 Water vapor . 14 1 Contents 3 Observed mean state of the atmosphere 15 3.1 Mass . 15 3.1.1 Geopotential height at 1000 hPa . 15 3.1.2 Zonal mean SLP . 17 3.1.3 Seasonal cycle of mass . 17 3.2 Thermal structure . 18 3.2.1 Insolation: daily-mean and TOA . 18 3.2.2 Surface air temperature . 18 3.2.3 Latitude-σ plots of temperature . 18 3.2.4 Potential temperature . 21 3.2.5 Static stability . 21 3.2.6 Effects of moisture . 24 3.2.7 Moist static stability . 24 3.2.8 Meridional temperature gradient . 25 3.2.9 Temperature variability . 26 3.2.10 Theories for the thermal structure . 26 3.3 Mean state of the circulation . 26 3.3.1 Surface winds and geopotential height . 27 3.3.2 Upper-level flow . 27 3.3.3 200 hPa u (CDC) . -
Navier-Stokes Equation
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Vorticity Production Through Rotation, Shear, and Baroclinicity
A&A 528, A145 (2011) Astronomy DOI: 10.1051/0004-6361/201015661 & c ESO 2011 Astrophysics Vorticity production through rotation, shear, and baroclinicity F. Del Sordo1,2 and A. Brandenburg1,2 1 Nordita, AlbaNova University Center, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden e-mail: [email protected] 2 Department of Astronomy, AlbaNova University Center, Stockholm University, 10691 Stockholm, Sweden Received 31 August 2010 / Accepted 14 February 2011 ABSTRACT Context. In the absence of rotation and shear, and under the assumption of constant temperature or specific entropy, purely potential forcing by localized expansion waves is known to produce irrotational flows that have no vorticity. Aims. Here we study the production of vorticity under idealized conditions when there is rotation, shear, or baroclinicity, to address the problem of vorticity generation in the interstellar medium in a systematic fashion. Methods. We use three-dimensional periodic box numerical simulations to investigate the various effects in isolation. Results. We find that for slow rotation, vorticity production in an isothermal gas is small in the sense that the ratio of the root-mean- square values of vorticity and velocity is small compared with the wavenumber of the energy-carrying motions. For Coriolis numbers above a certain level, vorticity production saturates at a value where the aforementioned ratio becomes comparable with the wavenum- ber of the energy-carrying motions. Shear also raises the vorticity production, but no saturation is found. When the assumption of isothermality is dropped, there is significant vorticity production by the baroclinic term once the turbulence becomes supersonic. In galaxies, shear and rotation are estimated to be insufficient to produce significant amounts of vorticity, leaving therefore only the baroclinic term as the most favorable candidate. -
Rotating Fluids
26 Rotating fluids The conductor of a carousel knows about fictitious forces. Moving from horse to horse while collecting tickets, he not only has to fight the centrifugal force trying to kick him off, but also has to deal with the dizzying sideways Coriolis force. On a typical carousel with a five meter radius and turning once every six seconds, the centrifugal force is strongest at the rim where it amounts to about 50% of gravity. Walking across the carousel at a normal speed of one meter per second, the conductor experiences a Coriolis force of about 20% of gravity. Provided the carousel turns anticlockwise seen from above, as most carousels seem to do, the Coriolis force always pulls the conductor off his course to the right. The conductor seems to prefer to move from horse to horse against the rotation, and this is quite understandable, since the Coriolis force then counteracts the centrifugal force. The whole world is a carousel, and not only in the metaphorical sense. The centrifugal force on Earth acts like a cylindrical antigravity field, reducing gravity at the equator by 0.3%. This is hardly a worry, unless you have to adjust Olympic records for geographic latitude. The Coriolis force is even less noticeable at Olympic speeds. You have to move as fast as a jet aircraft for it to amount to 0.3% of a percent of gravity. Weather systems and sea currents are so huge and move so slowly compared to Earth’s local rotation speed that the weak Coriolis force can become a major player in their dynamics. -
Atmosphere-Ocean Dynamics
1 80 o N o E 75 o N 30 o o E 70 N 20 o 65 N o a) E 10 oN 30o o 60 o o W 20 W 10 W 0 Atmosphere-Ocean Dynamics J. H. LaCasce Dept. of Geosciences University of Oslo LAST REVISED August 28, 2018 2 Contents 1 Equations 9 1.1 Derivatives ................................. 9 1.2 Continuityequation............................. 11 1.3 Momentumequations............................ 13 1.4 Equationsofstate.............................. 21 1.5 Thermodynamic equations . 22 1.6 Exercises .................................. 30 2 Basic balances 33 2.1 Hydrostaticbalance............................. 33 2.2 Horizontal momentum balances . 39 2.2.1 Geostrophicflow .......................... 41 2.2.2 Cyclostrophic flow . 44 2.2.3 Inertialflow............................. 46 2.2.4 Gradientwind............................ 47 2.3 The f-plane and β-plane approximations . 50 2.4 Incompressibility .............................. 52 2.4.1 The Boussinesq approximation . 52 2.4.2 Pressurecoordinates . 53 2.5 Thermalwind................................ 57 2.6 Summary of synoptic scale balances . 63 2.7 Exercises .................................. 64 3 Shallow water flows 67 3.1 Fundamentals ................................ 67 3.1.1 Assumptions ............................ 67 3.1.2 Shallow water equations . 70 3.2 Materialconservedquantities. 72 3.2.1 Volume ............................... 72 3.2.2 Vorticity............................... 73 3.2.3 Kelvin’s theorem . 75 3.2.4 Potential vorticity . 76 3.3 Integral conserved quantities . 77 3.3.1 Mass ................................ 77 3 4 CONTENTS 3.3.2 Circulation ............................. 78 3.3.3 Energy ............................... 79 3.4 Linearshallowwaterequations . 80 3.5 Gravitywaves................................ 82 3.6 Gravity waves with rotation . 87 3.7 Steadyflow ................................. 91 3.8 Geostrophicadjustment. 91 3.9 Kelvinwaves ................................ 95 3.10 EquatorialKelvinwaves . -
Surface Circulation2016
OCN 201 Surface Circulation Excess heat in equatorial regions requires redistribution toward the poles 1 In the Northern hemisphere, Coriolis force deflects movement to the right In the Southern hemisphere, Coriolis force deflects movement to the left Combination of atmospheric cells and Coriolis force yield the wind belts Wind belts drive ocean circulation 2 Surface circulation is one of the main transporters of “excess” heat from the tropics to northern latitudes Gulf Stream http://earthobservatory.nasa.gov/Newsroom/NewImages/Images/gulf_stream_modis_lrg.gif 3 How fast ( in miles per hour) do you think western boundary currents like the Gulf Stream are? A 1 B 2 C 4 D 8 E More! 4 mph = C Path of ocean currents affects agriculture and habitability of regions ~62 ˚N Mean Jan Faeroe temp 40 ˚F Islands ~61˚N Mean Jan Anchorage temp 13˚F Alaska 4 Average surface water temperature (N hemisphere winter) Surface currents are driven by winds, not thermohaline processes 5 Surface currents are shallow, in the upper few hundred metres of the ocean Clockwise gyres in North Atlantic and North Pacific Anti-clockwise gyres in South Atlantic and South Pacific How long do you think it takes for a trip around the North Pacific gyre? A 6 months B 1 year C 10 years D 20 years E 50 years D= ~ 20 years 6 Maximum in surface water salinity shows the gyres excess evaporation over precipitation results in higher surface water salinity Gyres are underneath, and driven by, the bands of Trade Winds and Westerlies 7 Which wind belt is Hawaii in? A Westerlies B Trade -
Intro to Tidal Theory
Introduction to Tidal Theory Ruth Farre (BSc. Cert. Nat. Sci.) South African Navy Hydrographic Office, Private Bag X1, Tokai, 7966 1. INTRODUCTION Tides: The periodic vertical movement of water on the Earth’s Surface (Admiralty Manual of Navigation) Tides are very often neglected or taken for granted, “they are just the sea advancing and retreating once or twice a day.” The Ancient Greeks and Romans weren’t particularly concerned with the tides at all, since in the Mediterranean they are almost imperceptible. It was this ignorance of tides that led to the loss of Caesar’s war galleys on the English shores, he failed to pull them up high enough to avoid the returning tide. In the beginning tides were explained by all sorts of legends. One ascribed the tides to the breathing cycle of a giant whale. In the late 10 th century, the Arabs had already begun to relate the timing of the tides to the cycles of the moon. However a scientific explanation for the tidal phenomenon had to wait for Sir Isaac Newton and his universal theory of gravitation which was published in 1687. He described in his “ Principia Mathematica ” how the tides arose from the gravitational attraction of the moon and the sun on the earth. He also showed why there are two tides for each lunar transit, the reason why spring and neap tides occurred, why diurnal tides are largest when the moon was furthest from the plane of the equator and why the equinoxial tides are larger in general than those at the solstices. -
Mesoscale and Submesoscale Physical-Biological Interactions
Chapter 4. MESOSCALE AND SUBMESOSCALE PHYSICAL–BIOLOGICAL INTERACTIONS GLENN FLIERL Massachusetts Institute of Technology DENNIS J. MCGILLICUDDY Woods Hole Oceanographic Institution Contents 1. Introduction 2. Eulerian versus Lagrangian Models 3. Biological Dynamics 4. Review of Eddy Dynamics 5. Rossby Waves and Biological Dynamics 6. Isolated Vortices 7. Eddy Transport, Stirring, and Mixing 8. Instabilities and Generation of Eddies 9. Near-Surface/ Deep-Ocean Interaction 10. Concluding Remarks References 1. Introduction In the 1960s and 1970s, physical oceanographers realized that mesoscale eddy flows were an order of magnitude stronger than the mean currents, that such variability is ubiquitous, and that the transport of momentum and heat by transient motions signif- icantly altered the general circulation of the ocean (see Robinson, 1983). Evidence that eddies can also profoundly alter the distributions and the dynamics of the biota began to accumulate during the latter part of this period (e.g., Angel and Fasham, 1983). As biological measurement technologies continue to improve and interdisci- plinary field studies to progress, we are developing a clearer picture of the spatial and temporal structure of biological variability and its association with the mesoscale and submesoscale band (corresponding to length scales of ten to hundreds of kilometers The Sea, Volume 12, edited by Allan R. Robinson, James J. McCarthy, and Brian J. Rothschild ISBN 0-471-18901-4 2002 John Wiley & Sons, Inc., New York 113 114 GLENN FLIERL AND DENNIS J. MCGILLICUDDY and time scales of days to years). In addition, biophysical modelling now provides a valuable tool for examining the ways in which populations react to these flows. -
Atmospheric Circulation of Terrestrial Exoplanets
Atmospheric Circulation of Terrestrial Exoplanets Adam P. Showman University of Arizona Robin D. Wordsworth University of Chicago Timothy M. Merlis Princeton University Yohai Kaspi Weizmann Institute of Science The investigation of planets around other stars began with the study of gas giants, but is now extending to the discovery and characterization of super-Earths and terrestrial planets. Motivated by this observational tide, we survey the basic dynamical principles governing the atmospheric circulation of terrestrial exoplanets, and discuss the interaction of their circulation with the hydrological cycle and global-scale climate feedbacks. Terrestrial exoplanets occupy a wide range of physical and dynamical conditions, only a small fraction of which have yet been explored in detail. Our approach is to lay out the fundamental dynamical principles governing the atmospheric circulation on terrestrial planets—broadly defined—and show how they can provide a foundation for understanding the atmospheric behavior of these worlds. We first sur- vey basic atmospheric dynamics, including the role of geostrophy, baroclinic instabilities, and jets in the strongly rotating regime (the “extratropics”) and the role of the Hadley circulation, wave adjustment of the thermal structure, and the tendency toward equatorial superrotation in the slowly rotating regime (the “tropics”). We then survey key elements of the hydrological cycle, including the factors that control precipitation, humidity, and cloudiness. Next, we summarize key mechanisms by which the circulation affects the global-mean climate, and hence planetary habitability. In particular, we discuss the runaway greenhouse, transitions to snowball states, atmospheric collapse, and the links between atmospheric circulation and CO2 weathering rates. We finish by summarizing the key questions and challenges for this emerging field in the future. -
Coriolis Effect
Project ATMOSPHERE This guide is one of a series produced by Project ATMOSPHERE, an initiative of the American Meteorological Society. Project ATMOSPHERE has created and trained a network of resource agents who provide nationwide leadership in precollege atmospheric environment education. To support these agents in their teacher training, Project ATMOSPHERE develops and produces teacher’s guides and other educational materials. For further information, and additional background on the American Meteorological Society’s Education Program, please contact: American Meteorological Society Education Program 1200 New York Ave., NW, Ste. 500 Washington, DC 20005-3928 www.ametsoc.org/amsedu This material is based upon work initially supported by the National Science Foundation under Grant No. TPE-9340055. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of the National Science Foundation. © 2012 American Meteorological Society (Permission is hereby granted for the reproduction of materials contained in this publication for non-commercial use in schools on the condition their source is acknowledged.) 2 Foreword This guide has been prepared to introduce fundamental understandings about the guide topic. This guide is organized as follows: Introduction This is a narrative summary of background information to introduce the topic. Basic Understandings Basic understandings are statements of principles, concepts, and information. The basic understandings represent material to be mastered by the learner, and can be especially helpful in devising learning activities in writing learning objectives and test items. They are numbered so they can be keyed with activities, objectives and test items. Activities These are related investigations.