Energy Literacy Essential Principles and Fundamental Concepts for Energy Education
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AST242 LECTURE NOTES PART 3 Contents 1. Viscous Flows 2 1.1. the Velocity Gradient Tensor 2 1.2. Viscous Stress Tensor 3 1.3. Na
AST242 LECTURE NOTES PART 3 Contents 1. Viscous flows 2 1.1. The velocity gradient tensor 2 1.2. Viscous stress tensor 3 1.3. Navier Stokes equation { diffusion 5 1.4. Viscosity to order of magnitude 6 1.5. Example using the viscous stress tensor: The force on a moving plate 6 1.6. Example using the Navier Stokes equation { Poiseuille flow or Flow in a capillary 7 1.7. Viscous Energy Dissipation 8 2. The Accretion disk 10 2.1. Accretion to order of magnitude 14 2.2. Hydrostatic equilibrium for an accretion disk 15 2.3. Shakura and Sunyaev's α-disk 17 2.4. Reynolds Number 17 2.5. Circumstellar disk heated by stellar radiation 18 2.6. Viscous Energy Dissipation 20 2.7. Accretion Luminosity 21 3. Vorticity and Rotation 24 3.1. Helmholtz Equation 25 3.2. Rate of Change of a vector element that is moving with the fluid 26 3.3. Kelvin Circulation Theorem 28 3.4. Vortex lines and vortex tubes 30 3.5. Vortex stretching and angular momentum 32 3.6. Bernoulli's constant in a wake 33 3.7. Diffusion of vorticity 34 3.8. Potential Flow and d'Alembert's paradox 34 3.9. Burger's vortex 36 4. Rotating Flows 38 4.1. Coriolis Force 38 4.2. Rossby and Ekman numbers 39 4.3. Geostrophic flows and the Taylor Proudman theorem 39 4.4. Two dimensional flows on the surface of a planet 41 1 2 AST242 LECTURE NOTES PART 3 4.5. Thermal winds? 42 5. -
Toolkit 1: Energy Units and Fundamentals of Quantitative Analysis
Energy & Society Energy Units and Fundamentals Toolkit 1: Energy Units and Fundamentals of Quantitative Analysis 1 Energy & Society Energy Units and Fundamentals Table of Contents 1. Key Concepts: Force, Work, Energy & Power 3 2. Orders of Magnitude & Scientific Notation 6 2.1. Orders of Magnitude 6 2.2. Scientific Notation 7 2.3. Rules for Calculations 7 2.3.1. Multiplication 8 2.3.2. Division 8 2.3.3. Exponentiation 8 2.3.4. Square Root 8 2.3.5. Addition & Subtraction 9 3. Linear versus Exponential Growth 10 3.1. Linear Growth 10 3.2. Exponential Growth 11 4. Uncertainty & Significant Figures 14 4.1. Uncertainty 14 4.2. Significant Figures 15 4.3. Exact Numbers 15 4.4. Identifying Significant Figures 16 4.5. Rules for Calculations 17 4.5.1. Addition & Subtraction 17 4.5.2. Multiplication, Division & Exponentiation 18 5. Unit Analysis 19 5.1. Commonly Used Energy & Non-energy Units 20 5.2. Form & Function 21 6. Sample Problems 22 6.1. Scientific Notation 22 6.2. Linear & Exponential Growth 22 6.3. Significant Figures 23 6.4. Unit Conversions 23 7. Answers to Sample Problems 24 7.1. Scientific Notation 24 7.2. Linear & Exponential Growth 24 7.3. Significant Figures 24 7.4. Unit Conversions 26 8. References 27 2 Energy & Society Energy Units and Fundamentals 1. KEY CONCEPTS: FORCE, WORK, ENERGY & POWER Among the most important fundamentals to be mastered when studying energy pertain to the differences and inter-relationships among four concepts: force, work, energy, and power. Each of these terms has a technical meaning in addition to popular or colloquial meanings. -
STARS in HYDROSTATIC EQUILIBRIUM Gravitational Energy
STARS IN HYDROSTATIC EQUILIBRIUM Gravitational energy and hydrostatic equilibrium We shall consider stars in a hydrostatic equilibrium, but not necessarily in a thermal equilibrium. Let us define some terms: U = kinetic, or in general internal energy density [ erg cm −3], (eql.1a) U u ≡ erg g −1 , (eql.1b) ρ R M 2 Eth ≡ U4πr dr = u dMr = thermal energy of a star, [erg], (eql.1c) Z Z 0 0 M GM dM Ω= − r r = gravitational energy of a star, [erg], (eql.1d) Z r 0 Etot = Eth +Ω = total energy of a star , [erg] . (eql.1e) We shall use the equation of hydrostatic equilibrium dP GM = − r ρ, (eql.2) dr r and the relation between the mass and radius dM r =4πr2ρ, (eql.3) dr to find a relations between thermal and gravitational energy of a star. As we shall be changing variables many times we shall adopt a convention of using ”c” as a symbol of a stellar center and the lower limit of an integral, and ”s” as a symbol of a stellar surface and the upper limit of an integral. We shall be transforming an integral formula (eql.1d) so, as to relate it to (eql.1c) : s s s GM dM GM GM ρ Ω= − r r = − r 4πr2ρdr = − r 4πr3dr = (eql.4) Z r Z r Z r2 c c c s s s dP s 4πr3dr = 4πr3dP =4πr3P − 12πr2P dr = Z dr Z c Z c c c s −3 P 4πr2dr =Ω. Z c Our final result: gravitational energy of a star in a hydrostatic equilibrium is equal to three times the integral of pressure within the star over its entire volume. -
Energy Conservation in a Spring
Part II: Energy Conservation in a Spring Activity 4 Title: Forces and Energy in a Spring Summary: Students will use the “Masses and Springs” simulation from PhET to investigate the relationship between gravitational potential energy, spring potential energy, and mass. Standard: PS2 (Ext) - 5 Students demonstrate an understanding of energy by… 5aa Identifying, measuring, calculating and analyzing qualitative and quantitative relationships associated with energy transfer or energy transformation. Specific Learning Goals: 1. Understand how to calculate the force constant of a spring using the formula F = -k ∆x 2. Understand that even though energy is transformed during the oscillation of a spring among gravitational potential energy, elastic potential energy, and kinetic energy, the total energy in the system remains constant. 3. Understand how to calculate the gravitational potential energy for a mass which is lifted to a height above a table. 4. Understand how to calculate the elastic potential energy for a spring which has been displaced by a certain distance. Prior Knowledge: 1. The restoring force that a spring exerts on a mass is proportional to the displacement of the spring and the spring constant and is in a direction opposite the displacement: F = -k ∆x 2. Gravitational potential energy is calculated by the formula: PEg = mgΔh 2 3. Elastic potential energy is calculated by the formula: PEs = ½ k ∆x 4. In a mass and spring system at equilibrium, the restoring force is equal to the gravitational force on the suspended mass (Fg = mg) Schedule: 40-50 minutes Materials: “Masses and Springs 2.02 PhET” Engage: Three different masses are suspended from a spring. -
Potential Energy
Potential Energy • So far: Considered all forces equal, calculate work done by net force only => Change in kinetic energy. – Analogy: Pure Cash Economy • But: Some forces seem to be able to “store” the work for you (when they do negative work) and “give back” the same amount (when they do positive work). – Analogy: Bank Account. You pay money in (ending up with less cash) - the money is stored for you - you can withdraw it again (get cash back) • These forces are called “conservative” (they conserve your work/money for you) Potential Energy - Example • Car moving up ramp: Weight does negative work ΔW(grav) = -mgΔh • Depends only on initial and final position • Can be retrieved as positive work on the way back down • Two ways to describe it: 1) No net work done on car on way up F Pull 2) Pulling force does positive F Normal y work that is stored as gravitational x potential energy ΔU = -ΔW(grav) α F Weight Total Mechanical Energy • Dimension: Same as Work Unit: Nm = J (Joule) Symbol: E = K.E. + U 1) Specify all external *) forces acting on a system 2) Multiply displacement in the direction of the net external force with that force: ΔWext = F Δs cosφ 3) Set equal to change in total energy: m 2 m 2 ΔE = /2vf - /2vi + ΔU = ΔWext ΔU = -Wint *) We consider all non-conservative forces as external, plus all forces that we don’t want to include in the system. Example: Gravitational Potential Energy *) • I. Motion in vertical (y-) direction only: "U = #Wgrav = mg"y • External force: Lift mass m from height y i to height y f (without increasing velocity) => Work gets stored as gravitational potential energy ΔU = mg (yf -yi)= mg Δy ! • Free fall (no external force): Total energy conserved, change in kinetic energy compensated by change in m 2 potential energy ΔK.E. -
How Long Would the Sun Shine? Fuel = Gravitational Energy? Fuel
How long would the Sun shine? Fuel = Gravitational Energy? • The mass of the Sun is M = 2 x 1030 kg. • The Sun needs fuel to shine. – The amount of the fuel should be related to the amount of – The Sun shines by consuming the fuel -- it generates energy mass. from the fuel. • Gravity can generate energy. • The lifetime of the Sun is determined by – A falling body acquires velocity from gravity. – How fast the Sun consumes the fuel, and – Gravitational energy = (3/5)GM2/R – How much fuel the Sun contains. – The radius of the Sun: R = 700 million m • How fast does the Sun consume the fuel? – Gravitational energy of the Sun = 2.3 x 1041 Joules. – Energy radiated per second is called the “luminosity”, which • How long could the Sun shine on gravitational energy? is in units of watts. – Lifetime = (Amount of Fuel)/(How Fast the Fuel is – The solar luminosity is about 3.8 x 1026 Watts. Consumed) 41 26 • Watts = Joules per second – Lifetime = (2.3 x 10 Joules)/(3.8 x 10 Joules per second) = 0.6 x 1015 seconds. • Compare it with a light bulb! – Therefore, the Sun lasts for 20 million years (Helmholtz in • What is the fuel?? 1854; Kelvin in 1887), if gravity is the fuel. Fuel = Nuclear Energy Burning Hydrogen: p-p chain • Einstein’s Energy Formula: E=Mc2 1 1 2 + – The mass itself can be the source of energy. • H + H -> H + e + !e 2 1 3 • If the Sun could convert all of its mass into energy by • H + H -> He + " E=Mc2… • 3He + 3He -> 4He + 1H + 1H – Mass energy = 1.8 x 1047 Joules. -
Gravitational Potential Energy
An easy way for numerical calculations • How long does it take for the Sun to go around the galaxy? • The Sun is travelling at v=220 km/s in a mostly circular orbit, of radius r=8 kpc REVISION Use another system of Units: u Assume G=1 Somak Raychaudhury u Unit of distance = 1kpc www.sr.bham.ac.uk/~somak/Y3FEG/ u Unit of velocity= 1 km/s u Then Unit of time becomes 109 yr •Course resources 5 • Website u And Unit of Mass becomes 2.3 × 10 M¤ • Books: nd • Sparke and Gallagher, 2 Edition So the time taken is 2πr/v = 2π × 8 /220 time units • Carroll and Ostlie, 2nd Edition Gravitational potential energy 1 Measuring the mass of a galaxy cluster The Virial theorem 2 T + V = 0 Virial theorem Newton’s shell theorems 2 Potential-density pairs Potential-density pairs Effective potential Bertrand’s theorem 3 Spiral arms To establish the existence of SMBHs are caused by density waves • Stellar kinematics in the core of the galaxy that sweep • Optical spectra: the width of the spectral line from around the broad emission lines Galaxy. • X-ray spectra: The iron Kα line is seen is clearly seen in some AGN spectra • The bolometric luminosities of the central regions of The Winding some galaxies is much larger than the Eddington Paradox (dilemma) luminosity is that if galaxies • Variability in X-rays: Causality demands that the rotated like this, the spiral structure scale of variability corresponds to an upper limit to would be quickly the light-travel time erased. -
Gravitational Potential and Energy of Homogeneous Rectangular
View metadata, citationGravitational and similar papers potential at core.ac.uk and energy of homogeneous rectangular parallelepipedbrought to you by CORE provided by CERN Document Server Zakir F. Seidov, P.I. Skvirsky Department of Physics, Ben-Gurion University of the Negev, Beer-Sheva, 84105, Israel Gravitational potential and gravitational energy are presented in analytical form for homogeneous right parallelepiped. PACS numbers: 01.55.+b, 45.20.Dd, 96.35.Fs Keywords: Newtonian mechanics; mass, size, gravitational fields I. INTRODUCTION: BASIC FORMULAE As it is well known, Newtonian gravitational potential, of homogeneous body with constant density ρ,atpoint (X,Y,Z) is defined as triple integral over the body's volume: ZZZ U(X; Y; Z)=Gρ u(X; Y; Z; x; y; z) dxdydz (1) with −1=2 u(X; Y; Z; x; y; z)=[(x − X)2 +(y − Y )2 +(z − Z)2] ;(2) here G stands for Newtonian constant of gravitation. In spite of almost 400-year-long attempts since Isaac Newton' times, the integral (1) is known in closed form (not in the series!) in quite a few cases [1]: a) a piece of straight line, b) a sphere, c) an ellipsoid; note that both cases a) and b) may be considered as particular cases of c). As to serial solution, the integral (1) is expressed in terms of the various kinds of series for external points outside the minimal sphere containing the whole body (non-necessary homogeneous), as well as for inner points close to the origin of co-ordinates. However in this note we do not touch the problem of serial solution and are only interested in exact analytical solution of (1). -
Mechanical Energy
Chapter 2 Mechanical Energy Mechanics is the branch of physics that deals with the motion of objects and the forces that affect that motion. Mechanical energy is similarly any form of energy that’s directly associated with motion or with a force. Kinetic energy is one form of mechanical energy. In this course we’ll also deal with two other types of mechanical energy: gravitational energy,associated with the force of gravity,and elastic energy, associated with the force exerted by a spring or some other object that is stretched or compressed. In this chapter I’ll introduce the formulas for all three types of mechanical energy,starting with gravitational energy. Gravitational Energy An object’s gravitational energy depends on how high it is,and also on its weight. Specifically,the gravitational energy is the product of weight times height: Gravitational energy = (weight) × (height). (2.1) For example,if you lift a brick two feet off the ground,you’ve given it twice as much gravitational energy as if you lift it only one foot,because of the greater height. On the other hand,a brick has more gravitational energy than a marble lifted to the same height,because of the brick’s greater weight. Weight,in the scientific sense of the word,is a measure of the force that gravity exerts on an object,pulling it downward. Equivalently,the weight of an object is the amount of force that you must exert to hold the object up,balancing the downward force of gravity. Weight is not the same thing as mass,which is a measure of the amount of “stuff” in an object. -
Gy Use Units and the Scales of Ener
The Basics: SI Units A tour of the energy landscape Units and Energy, power, force, pressure CO2 and other greenhouse gases conversion The many forms of energy Common sense and computation 8.21 Lecture 2 Units and the Scales of Energy Use September 11, 2009 8.21 Lecture 2: Units and the scales of energy use 1 The Basics: SI Units A tour of the energy landscape Units and Energy, power, force, pressure CO2 and other greenhouse gases conversion The many forms of energy Common sense and computation Outline • The basics: SI units • The principal players:gy ener , power, force, pressure • The many forms of energy • A tour of the energy landscape: From the macroworld to our world • CO2 and other greenhouse gases: measurements, units, energy connection • Perspectives on energy issues --- common sense and conversion factors 8.21 Lecture 2: Units and the scales of energy use 2 The Basics: SI Units tour of the energy landscapeA Units and , force, pressure, powerEnergy CO2 and other greenhouse gases conversion The many forms of energy Common sense and computation SI ≡ International System MKSA = MeterKilogram, , Second,mpereA Unit s Not cgs“English” or units! Electromagnetic units Deriud v n e its ⇒ Char⇒ geCoulombs EnerJ gy oul es ⇒ Current ⇒ Amperes Po werW a tts ⇒ Electrostatic potentialV⇒ olts Pr e ssuP a r s e cals ⇒ Resistance ⇒ Ohms Fo rNe c e wto n s T h erma l un i ts More about these next... TemperatureK⇒ elvinK) ( 8.21 Lecture 2: Units and the scales of energy use 3 The Basics: SI Units A tour of the energy landscape Units and Energy, power, -
3. Energy, Heat, and Work
3. Energy, Heat, and Work 3.1. Energy 3.2. Potential and Kinetic Energy 3.3. Internal Energy 3.4. Relatively Effects 3.5. Heat 3.6. Work 3.7. Notation and Sign Convention In these Lecture Notes we examine the basis of thermodynamics – fundamental definitions and equations for energy, heat, and work. 3-1. Energy. Two of man's earliest observations was that: 1)useful work could be accomplished by exerting a force through a distance and that the product of force and distance was proportional to the expended effort, and 2)heat could be ‘felt’ in when close or in contact with a warm body. There were many explanations for this second observation including that of invisible particles traveling through space1. It was not until the early beginnings of modern science and molecular theory that scientists discovered a true physical understanding of ‘heat flow’. It was later that a few notable individuals, including James Prescott Joule, discovered through experiment that work and heat were the same phenomenon and that this phenomenon was energy: Energy is the capacity, either latent or apparent, to exert a force through a distance. The presence of energy is indicated by the macroscopic characteristics of the physical or chemical structure of matter such as its pressure, density, or temperature - properties of matter. The concept of hot versus cold arose in the distant past as a consequence of man's sense of touch or feel. Observations show that, when a hot and a cold substance are placed together, the hot substance gets colder as the cold substance gets hotter. -
How Stars Work: • Basic Principles of Stellar Structure • Energy Production • the H-R Diagram
Ay 122 - Fall 2004 - Lecture 7 How Stars Work: • Basic Principles of Stellar Structure • Energy Production • The H-R Diagram (Many slides today c/o P. Armitage) The Basic Principles: • Hydrostatic equilibrium: thermal pressure vs. gravity – Basics of stellar structure • Energy conservation: dEprod / dt = L – Possible energy sources and characteristic timescales – Thermonuclear reactions • Energy transfer: from core to surface – Radiative or convective – The role of opacity The H-R Diagram: a basic framework for stellar physics and evolution – The Main Sequence and other branches – Scaling laws for stars Hydrostatic Equilibrium: Stars as Self-Regulating Systems • Energy is generated in the star's hot core, then carried outward to the cooler surface. • Inside a star, the inward force of gravity is balanced by the outward force of pressure. • The star is stabilized (i.e., nuclear reactions are kept under control) by a pressure-temperature thermostat. Self-Regulation in Stars Suppose the fusion rate increases slightly. Then, • Temperature increases. (2) Pressure increases. (3) Core expands. (4) Density and temperature decrease. (5) Fusion rate decreases. So there's a feedback mechanism which prevents the fusion rate from skyrocketing upward. We can reverse this argument as well … Now suppose that there was no source of energy in stars (e.g., no nuclear reactions) Core Collapse in a Self-Gravitating System • Suppose that there was no energy generation in the core. The pressure would still be high, so the core would be hotter than the envelope. • Energy would escape (via radiation, convection…) and so the core would shrink a bit under the gravity • That would make it even hotter, and then even more energy would escape; and so on, in a feedback loop Ë Core collapse! Unless an energy source is present to compensate for the escaping energy.