A Rotational View of the Atmoshere Chapter 4

Total Page:16

File Type:pdf, Size:1020Kb

A Rotational View of the Atmoshere Chapter 4 A Rotational View of the Atmoshere Chapter 4 Paul A. Ullrich [email protected] Part 2: The Vorticity Equation Vorticity: Key Questions Question: How is positive / negative vorticity generated? Question: How do we describe the time rate of change of vorticity? Question: How do we describe conservation of vorticity? Is vorticity actually conserved following the fow? Question: What is the role of the Earth’s rotation? Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation Start from the scaled horizontal momentum equation in z coordinates, no viscosity: Du 1 @p = + fv Dt −⇢ @x Dv 1 @p = fu Dt −⇢ @y − Take derivatives on both sides and compute: @ Dv @ @v = + u v @ Dv @ Du @x Dt @x @t · r ✓ ◆ ✓ ◆ @x Dt − @y Dt @ Du @ @u ✓ ◆ ✓ ◆ = + u u @y Dt @y @t · r ✓ ◆ ✓ ◆ Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation @ @u @ @ 1 @p @ (u u)=+ (fv) −@y @t − @y · r @y ⇢ @x − @y ✓ ◆ @ @v @ @ 1 @p @ + + (u v)= (fu) @x @t @x · r −@x ⇢ @y − @x ✓ ◆ A rather long derivaon @⇣ @u @v + u ⇣ +(⇣ + f) + @t · r @x @y ✓ ◆ @w @v @w @u @f @ 1 @p @ 1 @p + + v = + @x @z − @y @z @y −@x ⇢ @y @y ⇢ @x ✓ ◆ ✓ ◆ ✓ ◆ Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation @⇣ @u @v + u ⇣ +(⇣ + f) + @t · r @x @y ✓ ◆ @w @v @w @u @f @ 1 @p @ 1 @p + + v = + @x @z − @y @z @y −@x ⇢ @y @y ⇢ @x ✓ ◆ ✓ ◆ ✓ ◆ Vorticity Equation D @w @v @w @u (⇣ + f)= (⇣ + f)( u) ( ↵ p) k Dt − rh · − @x @z − @y @z − r ⇥r · ✓ ◆ 1 With specifc volume ↵ = ⇢ Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation What are these terms? D @w @v @w @u (⇣ + f)= (⇣ + f)( u) ( ↵ p) k Dt − rh · − @x @z − @y @z − r ⇥r · ✓ ◆ Tilting or twisting Divergence term Solenoidal term term Rate of change of the absolute vorticity following the motion Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation Take a closer look at the divergence term… (⇣ + f)( u) − rh · Horizontal Absolute vorticity divergence • Remember that divergence is related to vertical motion (column integrated divergence gives the local vertical velocity) • We now see that it is also related to changes in vorticity… Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vertical Velocity Obtained from horizontal divergence Continuity Equation in @u @v @! + + =0 Pressure Coordinates @x @y @p ✓ ◆p ⇥u ⇥v dω = + dp − ⇥x ⇥y ✓ ◆p ω @ p=0 p=0 ⇥u ⇥v dω = + dp − ⇥x ⇥y Zω @ ps Zps ✓ ◆p p=0 ⇥u ⇥v ω(p = 0) ω(p )= + dp − s − ⇥x ⇥y Zps ✓ ◆p ps ω(p )= ( u)dp s − ⇥p · Zp=0 Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vorticity and Divergence Vertical wind is related to the divergence of the horizontal wind. (which requires an ageostrophic component to the wind) Changes in vorticity are partially driven by divergence of the horizontal wind. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vorticity and Divergence This fow feld is purely vortical (zero divergence) Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vorticity and Divergence This fow feld is purely divergent (zero vorticity) Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vorticity and Divergence Question: What is the effect of divergence on vorticity? We can think about this like angular momentum Paul Ullrich Introduction to Atmospheric Dynamics March 2014 A Spinning Skater Motion is in the (x,y) plane Axis of rotation is in the vertical plane Paul Ullrich Introduction to Atmospheric Dynamics March 2014 A Spinning Skater Motion is in the (x,y) plane Question: A skater that is spinning with a given radius then brings in her arms. What happens to her angular velocity? Paul Ullrich Introduction to Atmospheric Dynamics March 2014 A Spinning Skater Recall: Angular momentum Motion is in the is a conserved quantity. Its (x,y) plane magnitude is given by L = rm! | | Answer: Since her radius decreases, conservation of angular momentum says that her angular velocity must increase. Question: How is this like divergence? Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Vorticity and Divergence Question: What is the effect of divergence on vorticity? Answer: A divergent fow must lead to a decrease in angular velocity. A convergent fow must lead to an increase in angular velocity. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation Divergence term only D (⇣ + f)= (⇣ + f)( u) Dt − rh · Horizontal Absolute vorticity divergence Question: What happens to absolute vorticity when the fow is (a) Divergent? ( h u) > 0 r · (b) Convergent? ( u) < 0 rh · Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation What are these terms? D @w @v @w @u (⇣ + f)= (⇣ + f)( u) ( ↵ p) k Dt − rh · − @x @z − @y @z − r ⇥r · ✓ ◆ Tilting or twisting Divergence term Solenoidal term term Rate of change of the absolute vorticity following the motion Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting and Twisting Recall how relative vorticity is obtained: Relative velocity: u =(u, v, w) @w @v @u @w @v @u 3D vorticity vector: u = , , r⇥ @y − @z @z − @x @x − @y ✓ ◆ @v @u Relative vorticity: ⇣ = k ( u)= · r⇥ @x − @y ✓ ◆ Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting and Twisting Tilting or twisting term @w @v @w @u @x @z − @y @z ✓ ◆ Tilting represents the change in the vertical component of vorticity by tilting horizontal vorticity into the vertical. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting or twisting term @w @v @w @u @x @z − @y @z ✓ ◆ z Consider a long, thin cylinder of fuid aligned with the y-axis. y x Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting or twisting term @w @v @w @u @x @z − @y @z ✓ ◆ =0 > 0 z Initial axis of rotation Consider a long, thin cylinder of fuid aligned with the y-axis. y The fow satisfes v=0 and is sheared in the vertical so that the vorticity vector is along the y axis. x Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting or twisting term @w @v @w @u @x @z − @y @z ✓ ◆ =0 > 0 > 0 z Consider a long, thin The fow also satisfes cylinder of fuid dw/dy>0 leading to an aligned with the y-axis. upward tilting of the y cylindrical tube The fow satisfes v=0 and is sheared in the vertical so that the vorticity vector is along the y axis. x Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting and Twisting z Tilting or twisting term y @w @v @w @u @x @z − @y @z ✓ ◆ =0 > 0 > 0 x Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Tilting and Twisting Rotation in the (y,z) plane. Vorticity vector points along the x axis. As the wheel is turned there is a component of vorticity in the z plane. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation What are these terms? D @w @v @w @u (⇣ + f)= (⇣ + f)( u) ( ↵ p) k Dt − rh · − @x @z − @y @z − r ⇥r · ✓ ◆ Tilting or twisting Divergence term Solenoidal term term Rate of change of the absolute vorticity following the motion Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Solenoidal / Baroclinic Terms @ 1 @p @ 1 @p @↵ @p @↵ @p + = + −@x ⇢ @y @y ⇢ @x − @x @y @y @x ✓ ◆ ✓ ◆ The solenoidal / baroclinic terms capture changes in vorticity due to the alignment of surfaces of constant density and pressure. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Solenoidal / Baroclinic Terms Defnition: In a barotropic fuid density depends only on pressure. By the ideal gas law, this implies that surfaces of constant density are surfaces of constant pressure are surfaces of constant temperature. Defnition: In a baroclinic fuid density depends on pressure and temperature. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Solenoidal / Baroclinic Terms Barotropic: surfaces of constant density parallel to surfaces of constant pressure y ↵ p =0 p-2Δp r ⇥r ρ-2Δρ p-Δp ρ-Δρ ρ p A barotropic fuid does not x induce changes in vorticity Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Solenoidal / Baroclinic Terms Baroclinic: surfaces of constant density intersect surfaces of constant pressure y ↵ p =0 p-2Δp r ⇥r 6 ρ-2Δρ p-Δp ρ-Δρ ρ p A baroclinic fuid induces x a change in vorticity. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Solenoidal / Baroclinic Terms In the real atmosphere, the solenoidal terms are a primary driver of the development of low-level low pressure systems in the middle latitudes. This term is also important in understanding circulation around fronts. Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Aside: Baroclinic Fronts Note that this case has to do with the development of horizontal vorticity (perpendicular to x-z plane) z p-2Δp ρ-2Δρ p-Δp ρ-Δρ ρ p Cold air sinking Warm air rising x behind front ahead of front Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation What are these terms? D @w @v @w @u (⇣ + f)= (⇣ + f)( u) ( ↵ p) k Dt − rh · − @x @z − @y @z − r ⇥r · ✓ ◆ Tilting or twisting Divergence term Solenoidal term term Rate of change of the absolute vorticity following the motion Paul Ullrich Introduction to Atmospheric Dynamics March 2014 Advection of Vorticity D ⇥ ⇥ ⇥ ⇥ (ζ + f)= (ζ + f)+u (ζ + f)+v (ζ + f)+w (ζ + f) Dt ⇥t ⇥x ⇥y ⇥z @f @f @f =0 =0 =0 @t @x @z D @⇣ @f (⇣ + f)= + u ⇣ + v Dt @t · r @y Advection of Advection of relative vorticity planetary vorticity Paul Ullrich Introduction to Atmospheric Dynamics March 2014 The Vorticity Equation @⇣ @u @v + u ⇣ +(⇣ + f) + @t · r @x @y ✓ ◆ @w @v @w @u @f @ 1 @p @ 1 @p + + v = + @x @z − @y @z @y −@x ⇢ @y @y ⇢ @x
Recommended publications
  • Lecture 5: Saturn, Neptune, … A. P. Ingersoll [email protected] 1
    Lecture 5: Saturn, Neptune, … A. P. Ingersoll [email protected] 1. A lot a new material from the Cassini spacecraft, which has been in orbit around Saturn for four years. This talk will have a lot of pictures, not so much models. 2. Uranus on the left, Neptune on the right. Uranus spins on its side. The obliquity is 98 degrees, which means the poles receive more sunlight than the equator. It also means the sun is almost overhead at the pole during summer solstice. Despite these extreme changes in the distribution of sunlight, Uranus is a banded planet. The rotation dominates the winds and cloud structure. 3. Saturn is covered by a layer of clouds and haze, so it is hard to see the features. Storms are less frequent on Saturn than on Jupiter; it is not just that clouds and haze makes the storms less visible. Saturn is a less active planet. Nevertheless the winds are stronger than the winds of Jupiter. 4. The thickness of the atmosphere is inversely proportional to gravity. The zero of altitude is where the pressure is 100 mbar. Uranus and Neptune are so cold that CH forms clouds. The clouds of NH3 , NH4SH, and H2O form at much deeper levels and have not been detected. 5. Surprising fact: The winds increase as you move outward in the solar system. Why? My theory is that power/area is smaller, small‐scale turbulence is weaker, dissipation is less, and the winds are stronger. Jupiter looks more turbulent, and it has the smallest winds.
    [Show full text]
  • ATMOSPHERIC and OCEANIC FLUID DYNAMICS Fundamentals and Large-Scale Circulation
    ATMOSPHERIC AND OCEANIC FLUID DYNAMICS Fundamentals and Large-Scale Circulation Geoffrey K. Vallis Contents Preface xi Part I FUNDAMENTALS OF GEOPHYSICAL FLUID DYNAMICS 1 1 Equations of Motion 3 1.1 Time Derivatives for Fluids 3 1.2 The Mass Continuity Equation 7 1.3 The Momentum Equation 11 1.4 The Equation of State 14 1.5 The Thermodynamic Equation 16 1.6 Sound Waves 29 1.7 Compressible and Incompressible Flow 31 1.8 * More Thermodynamics of Liquids 33 1.9 The Energy Budget 39 1.10 An Introduction to Non-Dimensionalization and Scaling 43 2 Effects of Rotation and Stratification 51 2.1 Equations in a Rotating Frame 51 2.2 Equations of Motion in Spherical Coordinates 55 2.3 Cartesian Approximations: The Tangent Plane 66 2.4 The Boussinesq Approximation 68 2.5 The Anelastic Approximation 74 2.6 Changing Vertical Coordinate 78 2.7 Hydrostatic Balance 80 2.8 Geostrophic and Thermal Wind Balance 85 2.9 Static Instability and the Parcel Method 92 2.10 Gravity Waves 98 v vi Contents 2.11 * Acoustic-Gravity Waves in an Ideal Gas 100 2.12 The Ekman Layer 104 3 Shallow Water Systems and Isentropic Coordinates 123 3.1 Dynamics of a Single, Shallow Layer 123 3.2 Reduced Gravity Equations 129 3.3 Multi-Layer Shallow Water Equations 131 3.4 Geostrophic Balance and Thermal wind 134 3.5 Form Drag 135 3.6 Conservation Properties of Shallow Water Systems 136 3.7 Shallow Water Waves 140 3.8 Geostrophic Adjustment 144 3.9 Isentropic Coordinates 152 3.10 Available Potential Energy 155 4 Vorticity and Potential Vorticity 165 4.1 Vorticity and Circulation 165
    [Show full text]
  • Chapter 7 Balanced Flow
    Chapter 7 Balanced flow In Chapter 6 we derived the equations that govern the evolution of the at- mosphere and ocean, setting our discussion on a sound theoretical footing. However, these equations describe myriad phenomena, many of which are not central to our discussion of the large-scale circulation of the atmosphere and ocean. In this chapter, therefore, we focus on a subset of possible motions known as ‘balanced flows’ which are relevant to the general circulation. We have already seen that large-scale flow in the atmosphere and ocean is hydrostatically balanced in the vertical in the sense that gravitational and pressure gradient forces balance one another, rather than inducing accelera- tions. It turns out that the atmosphere and ocean are also close to balance in the horizontal, in the sense that Coriolis forces are balanced by horizon- tal pressure gradients in what is known as ‘geostrophic motion’ – from the Greek: ‘geo’ for ‘earth’, ‘strophe’ for ‘turning’. In this Chapter we describe how the rather peculiar and counter-intuitive properties of the geostrophic motion of a homogeneous fluid are encapsulated in the ‘Taylor-Proudman theorem’ which expresses in mathematical form the ‘stiffness’ imparted to a fluid by rotation. This stiffness property will be repeatedly applied in later chapters to come to some understanding of the large-scale circulation of the atmosphere and ocean. We go on to discuss how the Taylor-Proudman theo- rem is modified in a fluid in which the density is not homogeneous but varies from place to place, deriving the ‘thermal wind equation’. Finally we dis- cuss so-called ‘ageostrophic flow’ motion, which is not in geostrophic balance but is modified by friction in regions where the atmosphere and ocean rubs against solid boundaries or at the atmosphere-ocean interface.
    [Show full text]
  • Dynamics of Jupiter's Atmosphere
    6 Dynamics of Jupiter's Atmosphere Andrew P. Ingersoll California Institute of Technology Timothy E. Dowling University of Louisville P eter J. Gierasch Cornell University GlennS. Orton J et P ropulsion Laboratory, California Institute of Technology Peter L. Read Oxford. University Agustin Sanchez-Lavega Universidad del P ais Vasco, Spain Adam P. Showman University of A rizona Amy A. Simon-Miller NASA Goddard. Space Flight Center Ashwin R . V asavada J et Propulsion Laboratory, California Institute of Technology 6.1 INTRODUCTION occurs on both planets. On Earth, electrical charge separa­ tion is associated with falling ice and rain. On Jupiter, t he Giant planet atmospheres provided many of the surprises separation mechanism is still to be determined. and remarkable discoveries of planetary exploration during The winds of Jupiter are only 1/ 3 as strong as t hose t he past few decades. Studying Jupiter's atmosphere and of aturn and Neptune, and yet the other giant planets comparing it with Earth's gives us critical insight and a have less sunlight and less internal heat than Jupiter. Earth broad understanding of how atmospheres work that could probably has the weakest winds of any planet, although its not be obtained by studying Earth alone. absorbed solar power per unit area is largest. All the gi­ ant planets are banded. Even Uranus, whose rotation axis Jupiter has half a dozen eastward jet streams in each is tipped 98° relative to its orbit axis. exhibits banded hemisphere. On average, Earth has only one in each hemi­ cloud patterns and east- west (zonal) jets.
    [Show full text]
  • ATM 500: Atmospheric Dynamics End-Of-Semester Review, December 6 2017 Here, in Bullet Points, Are the Key Concepts from the Second Half of the Course
    ATM 500: Atmospheric Dynamics End-of-semester review, December 6 2017 Here, in bullet points, are the key concepts from the second half of the course. They are not meant to be self-contained notes! Refer back to your course notes for notation, derivations, and deeper discussion. Static stability The vertical variation of density in the environment determines whether a parcel, disturbed upward from an initial hydrostatic rest state, will accelerate away from its initial position, or oscillate about that position. For an incompressible or Boussinesq fluid, the buoyancy frequency is g dρ~ N 2 = − ρ~dz For a compressible ideal gas, the buoyancy frequency is g dθ~ N 2 = θ~dz (the expressions are different because density is not conserved in a small upward displacement of a compressible fluid, but potential temperature is conserved) Fluid is statically stable if N 2 > 0; otherwise it is statically unstable. Typical value for troposphere: N = 0:01 s−1, with corresponding oscillation period of 10 minutes. Dry adiabatic lapse rate g −1 Γd = = 9:8 K km cp The rate at which temperature decreases during adiabatic ascent (for which Dθ Dt = 0) \Dry" here means that there is no latent heating from condensation of water vapor. Static stability criteria for a dry atmosphere Environment is stable to dry con- vection if dθ~ dT~ > 0 or − < Γ dz dz d and otherwise unstable. 1 Buoyancy equation for Boussinesq fluid with background stratification Db0 + N 2w = 0 Dt where we have separated the full buoyancy into a mean vertical part ^b(z) and 0 2 d^b 2 everything else (b ), and N = dz .
    [Show full text]
  • A Diagnostic Model for Initial Winds in Primitive
    1 1 A DIAGNOSTIC MODEL FOR INITIAL WINDS IN PRIMITIVE EQUATIONS FORECASTS by Richard Asselin Department of Meteorology, Ph. D. ABSTRACT The set of primitive meteorologicai equations reduces to a single second order partial differential cquation when the accel- eration is replaced by the derivative of the geostrophic wind in the equation.of motion. From this equation a diagnostic three-dimensional wind field can be computed when the pressure distribution is known. Calculations for a barotropic atmosphere are performed fir st; the rotational part of the wind is found to be similar to that from the classical balance equation and the divergent part agrees well with synoptic experience. A forecast thus initialized contaills Lese; gravi- tational activity than one initialized with the non-divergent wind of the balance equation. With a five-level baroclinic atmosphere. the effects of mountains, surface drag, and release of latent heat are studi~d separately; the results arc consistent wlth classical concepts and other interesting features are revealed. T!;e diagnostic surfa:::e pres­ sure tendency is fo~nd to be in very good agreement with the observed pressure changes. A DIAGNOSTIC MODEL FOR INITIAL WINDS IN PRIMITIVE EQUATiONS FORECASTS by RI CHARD ASSE LIN . A the sis submitted to the Faculty of Graduate Studies and Re search in partial fulfillrnent of the requirernents for the degree of Doctor of Philosophy. Departrnent of Meteorology McGill Univer sity Montreal, Canada July. 1970 1971 A DL~GNOSTIC MODEL FOR INITIAL WINDS IN PRIMITIVE EQUATIONS FORECASTS by RI CHARD ASSE LIN . A thesis submitted ta the Faculty of Graduate Studies and Research in partial fulfillment of the requirements.
    [Show full text]
  • Ch4: Basics of Stratified Fluid ∂
    AOS611Ch.4, Z. Liu, 02/16/2016 1 Ch4: Basics of Stratified Fluid Sec. 4.1: Basic Equations Stratification will introduce new physics. We first derive the equations. Denoting rotation vector as Ω , gravity potential , u u,v, w, i x j y k z . The momentum equations are du 2Ω u p F . (4.1.1) dt The mass equation is d u 0 or u 0 (4.1.2) dt t The equation of state in general is p, T, S... (4.1.3) In the ocean, neglecting salinity, the equation of state is m 1T T0 (4.1.4) 1 where is the coefficient of thermal expansion and is a constant m T P reference density, which can be chosen as the average density. In the atmosphere, using the perfect gas, the equation of state is P (4.1.5) RT where R is the gas constant. The thermodynamic equation describes the internal energy change. For the ocean, which is incompressible, the thermodynamic equation is dT ~ C Q k 2T (4.1.6) p dt ~ where k is the thermal conductivity, Q is the heating rate per unit mass. This can be rewritten as dT J k 2T (4.1.6a) dt ~ Q k where J and k . Cp Cp Copyright 2014, Zhengyu Liu AOS611Ch.4, Z. Liu, 02/16/2016 2 The atmosphere is compressible, so the thermodynamic equation is dT 1 dp J k 2T (4.1.7) dt C p dt p 0 R , Define the potential temperature as T , where C we have p p p0 ln lnT ln lnT ln p const p d dT dp T p T p0 T d dT dp dT dp T p p p d p0 2 J k T (4.1.8) dt p T RT 1 where we have used (4.1.7) and the ideal gas law (4.1.5), such that .
    [Show full text]
  • Understanding Basic Concepts of Numerical Weather Prediction Using Single Level Atmospheric Model
    American Journal of Engineering Research (AJER) 2017 American Journal of Engineering Research (AJER) e-ISSN: 2320-0847 p-ISSN : 2320-0936 Volume-6, Issue-3, pp-57-62 www.ajer.org Research Paper Open Access Understanding Basic Concepts of Numerical Weather Prediction Using Single Level Atmospheric Model Ahmed Z. Abdulmajed, Kais J. Al-Jumaily Department of Atmospheric Sciences, College of Science, Al-Mustansiriyah University, Baghdad, Iraq ABSTRACT: Weather impacts all daily lives from a very hot summer day to a cold winter storm. Predicting these events and other weather phenomena has lead scientist to develop the most accurate way to forecast weather, numerical weather prediction. This system developed over the last 100 years has created more accurate and longer forecast periods, as well as, created a highly complex system of calculations designed to simulate atmospheric motions. This simulation requires the use of large computing systems for the computation but through the use of a simplified computer program one can gain a full understanding of the process of numerical weather prediction and the complexity of its parts. The aim of this research is to use a single level atmospheric model to understand some basic concepts of numerical weather prediction. Reference geopotential height of 5500 meters which represent the height of 500 mb pressure level was used as a single level. The model results showed that initial geopotential has two distinct centres of low and high geopotentials and the high centre is situated close to reference point. The results also indicated that the change in the time step interval of the integration does not affect the solution of shallow water equations and increasing the forecast length would result in the deformation in the geopotential patterns.
    [Show full text]
  • The Problem of the Professional Training of Meteorological Personnel of All Grades in the Less-Developed Countries
    WORLD METEOROLOGICAL ORGANIZATION TECHNICAL NOTE No. 50 THE PROBLEM OF THE PROFESSIONAL TRAINING OF METEOROLOGICAL PERSONNEL OF ALL GRADES IN THE LESS-DEVELOPED COUNTRIES PROFESSOR J. VAN MIEGHEM Consultant on Meteorological Training to the Secretary-General of WMO Reprinted in 1967 PRICE: Sw. fro 6.- I WMO· No. 132.TP. 59 I Secretariat of the World Meteorological Organization - Geneva - Switzerland 1963 NOTE The designations employed and the presentation of the material in this publication do not imply the expression of any opinion whatsoever on the part of the Secretariat of the World Meteorological Organization concerning the legal status of any country or territory or of its authorities, or concerning the delimitation of its frontiers. TABLE OF CONTENTS Foreword • .. .. .. .. .. .. .. .. .. .. .. .. • .. .. .. Summaries (English, French, Russian, Spanish). VII 1. Introduction .. .. .. 1 2. Collaboration with UNESCO and ICAO 1 3· Qualifications and recruitment of meteorological personnel 2 4. Equivalence of curricula and diplomas, standardization of Syllabi. 4 The diversity of personnel in a meteorological service and the need for uniform grading .. .. .. 5 6. Short-course training 7 7· Grading of meteorological personnel into four classes I duties devolving on each class and standards of knowledge required. 7 7.1 Class I meteorological personnel • 8 7.2 Class II meteorological personnel 8 7.3 Class III meteorological personnel 9 7.4 Class IV meteorological personnel 9 7.5 Syllabi of the courses • • • • • • . 9 7.6 Duration of meteorological courses 10 8. Plan for developing professional meteorological training 11 8.1 Fundamentals .. •• " •• • • •• • .. • • •••••• .. • 11 8.2 Instruction and tTaining of Class IV meteorological personnel 12 8.3 Instruction and training of Class III and Class II meteorological personnel.
    [Show full text]
  • Circulation and Vorticity
    Lecture 4: Circulation and Vorticity • Circulation •Bjerknes Circulation Theorem • Vorticity • Potential Vorticity • Conservation of Potential Vorticity ESS227 Prof. Jin-Yi Yu Measurement of Rotation • Circulation and vorticity are the two primary measures of rotation in a fluid. • Circul ati on, whi ch i s a scal ar i nt egral quantit y, i s a macroscopic measure of rotation for a finite area of the fluid. • Vorticity, however, is a vector field that gives a microscopic measure of the rotation at any point in the fluid. ESS227 Prof. Jin-Yi Yu Circulation • The circulation, C, about a closed contour in a fluid is defined as thliihe line integral eval uated dl along th e contour of fh the component of the velocity vector that is locally tangent to the contour. C > 0 Î Counterclockwise C < 0 Î Clockwise ESS227 Prof. Jin-Yi Yu Example • That circulation is a measure of rotation is demonstrated readily by considering a circular ring of fluid of radius R in solid-body rotation at angular velocity Ω about the z axis . • In this case, U = Ω × R, where R is the distance from the axis of rotation to the ring of fluid. Thus the circulation about the ring is given by: • In this case the circulation is just 2π times the angular momentum of the fluid ring about the axis of rotation. Alternatively, note that C/(πR2) = 2Ω so that the circulation divided by the area enclosed by the loop is just twice thlhe angular spee dfifhid of rotation of the ring. • Unlike angular momentum or angular velocity, circulation can be computed without reference to an axis of rotation; it can thus be used to characterize fluid rotation in situations where “angular velocity” is not defined easily.
    [Show full text]
  • Moist Versus Dry Barotropic Instability in a Shallow-Water Model of the Atmosphere with Moist Convection
    1234 JOURNAL OF THE ATMOSPHERIC SCIENCES VOLUME 68 Moist versus Dry Barotropic Instability in a Shallow-Water Model of the Atmosphere with Moist Convection JULIEN LAMBAERTS,GUILLAUME LAPEYRE, AND VLADIMIR ZEITLIN Laboratoire de Me´te´orologie Dynamique/IPSL, Ecole Normale Supe´rieure/CNRS/UPMC, Paris, France (Manuscript received 28 April 2010, in final form 6 January 2011) ABSTRACT Dynamical influence of moist convection upon development of the barotropic instability is studied in the rotating shallow-water model. First, an exhaustive linear ‘‘dry’’ stability analysis of the Bickley jet is per- formed, and the most unstable mode identified in this way is used to initialize simulations to compare the development and the saturation of the instability in dry and moist configurations. High-resolution numerical simulations with a well-balanced finite-volume scheme reveal substantial qualitative and quantitative dif- ferences in the evolution of dry and moist-convective instabilities. The moist effects affect both balanced and unbalanced components of the flow. The most important differences between dry and moist evolution are 1) the enhanced efficiency of the moist-convective instability, which manifests itself by the increase of the growth rate at the onset of precipitation, and by a stronger deviation of the end state from the initial one, measured with a number of different norms; 2) a pronounced cyclone–anticyclone asymmetry during the nonlinear evolution of the moist-convective instability, which leads to an additional, with respect to the dry case, geostrophic adjustment, and the modification of the end state; and 3) an enhanced ageostrophic activity in the precipitation zones but also in the nonprecipitating areas because of the secondary geostrophic adjustment.
    [Show full text]
  • An Introduction to Dynamic Meteorology.Pdf
    January 24, 2004 12:0 Elsevier/AID aid An Introduction to Dynamic Meteorology FOURTH EDITION January 24, 2004 12:0 Elsevier/AID aid This is Volume 88 in the INTERNATIONAL GEOPHYSICS SERIES A series of monographs and textbooks Edited by RENATADMOWSKA, JAMES R. HOLTON and H.THOMAS ROSSBY A complete list of books in this series appears at the end of this volume. January 24, 2004 12:0 Elsevier/AID aid AN INTRODUCTION TO DYNAMIC METEOROLOGY Fourth Edition JAMES R. HOLTON Department of Atmospheric Sciences University of Washington Seattle,Washington Amsterdam Boston Heidelberg London New York Oxford Paris San Diego San Francisco Singapore Sydney Tokyo January 24, 2004 12:0 Elsevier/AID aid Senior Editor, Earth Sciences Frank Cynar Editorial Coordinator Jennifer Helé Senior Marketing Manager Linda Beattie Cover Design Eric DeCicco Composition Integra Software Services Printer/Binder The Maple-Vail Manufacturing Group Cover printer Phoenix Color Corp Elsevier Academic Press 200 Wheeler Road, Burlington, MA 01803, USA 525 B Street, Suite 1900, San Diego, California 92101-4495, USA 84 Theobald’s Road, London WC1X 8RR, UK This book is printed on acid-free paper. Copyright c 2004, Elsevier Inc. All rights reserved. No part of this publication may be reproduced or transmitted in any form or by any means, electronic or mechanical, including photocopy, recording, or any information storage and retrieval system, without permission in writing from the publisher. Permissions may be sought directly from Elsevier’s Science & Technology Rights Department in
    [Show full text]