Multiple Integrals
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												  Rotational Motion (The Dynamics of a Rigid Body)University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln Robert Katz Publications Research Papers in Physics and Astronomy 1-1958 Physics, Chapter 11: Rotational Motion (The Dynamics of a Rigid Body) Henry Semat City College of New York Robert Katz University of Nebraska-Lincoln, [email protected] Follow this and additional works at: https://digitalcommons.unl.edu/physicskatz Part of the Physics Commons Semat, Henry and Katz, Robert, "Physics, Chapter 11: Rotational Motion (The Dynamics of a Rigid Body)" (1958). Robert Katz Publications. 141. https://digitalcommons.unl.edu/physicskatz/141 This Article is brought to you for free and open access by the Research Papers in Physics and Astronomy at DigitalCommons@University of Nebraska - Lincoln. It has been accepted for inclusion in Robert Katz Publications by an authorized administrator of DigitalCommons@University of Nebraska - Lincoln. 11 Rotational Motion (The Dynamics of a Rigid Body) 11-1 Motion about a Fixed Axis The motion of the flywheel of an engine and of a pulley on its axle are examples of an important type of motion of a rigid body, that of the motion of rotation about a fixed axis. Consider the motion of a uniform disk rotat ing about a fixed axis passing through its center of gravity C perpendicular to the face of the disk, as shown in Figure 11-1. The motion of this disk may be de scribed in terms of the motions of each of its individual particles, but a better way to describe the motion is in terms of the angle through which the disk rotates.
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												  MULTIVARIABLE CALCULUS (MATH 212 ) COMMON TOPIC LIST (Approved by the Occidental College Math Department on August 28, 2009)MULTIVARIABLE CALCULUS (MATH 212 ) COMMON TOPIC LIST (Approved by the Occidental College Math Department on August 28, 2009) Required Topics • Multivariable functions • 3-D space o Distance o Equations of Spheres o Graphing Planes Spheres Miscellaneous function graphs Sections and level curves (contour diagrams) Level surfaces • Planes o Equations of planes, in different forms o Equation of plane from three points o Linear approximation and tangent planes • Partial Derivatives o Compute using the definition of partial derivative o Compute using differentiation rules o Interpret o Approximate, given contour diagram, table of values, or sketch of sections o Signs from real-world description o Compute a gradient vector • Vectors o Arithmetic on vectors, pictorially and by components o Dot product compute using components v v v v v ⋅ w = v w cosθ v v v v u ⋅ v = 0⇔ u ⊥ v (for nonzero vectors) o Cross product Direction and length compute using components and determinant • Directional derivatives o estimate from contour diagram o compute using the lim definition t→0 v v o v compute using fu = ∇f ⋅ u ( u a unit vector) • Gradient v o v geometry (3 facts, and understand how they follow from fu = ∇f ⋅ u ) Gradient points in direction of fastest increase Length of gradient is the directional derivative in that direction Gradient is perpendicular to level set o given contour diagram, draw a gradient vector • Chain rules • Higher-order partials o compute o mixed partials are equal (under certain conditions) • Optimization o Locate and
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												  Basic Galactic Dynamics5 Basic galactic dynamics 5.1 Basic laws govern galaxy structure The basic force on galaxy scale is gravitational • Why? The other long-range force is electro-magnetic force due to electric • charges: positive and negative charges are difficult to separate on galaxy scales. 5.1.1 Gravitational forces Gravitational force on a point mass M1 located at x1 from a point mass M2 located at x2 is GM M (x x ) F = 1 2 1 − 2 . 1 − x x 3 | 1 − 2| Note that force F1 and positions, x1 and x2 are vectors. Note also F2 = F1 consistent with Newton’s Third Law. Consider a stellar− system of N stars. The gravitational force on ith star is the sum of the force due to all other stars N GM M (x x ) F i j i j i = −3 . − xi xj Xj=6 i | − | The equation of motion of the ith star under mutual gravitational force is given by Newton’s second law, dv F = m a = m i i i i i dt and so N dvi GMj(xi xj) = − 3 . dt xi xj Xj=6 i | − | 5.1.2 Energy conservation Assuming M2 is fixed at the origin, and M1 on the x-axis at a distance x1 from the origin, we have m1dv1 GM1M2 = 2 dt − x1 1 2 Using 2 dv1 dx1 dv1 dv1 1 dv1 = = v1 = dt dt dx1 dx1 2 dx1 we have 2 1 dv1 GM1M2 m1 = 2 , 2 dx1 − x1 which can be integrated to give 1 2 GM1M2 m1v1 = E , 2 − x1 The first term on the lhs is the kinetic energy • The second term on the lhs is the potential energy • E is the total energy and is conserved • 5.1.3 Gravitational potential The potential energy of M1 in the potential of M2 is M Φ , − 1 × 2 where GM2 Φ2 = − x1 is the potential of M2 at a distance x1 from it.
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												  A Brief Tour of Vector CalculusA BRIEF TOUR OF VECTOR CALCULUS A. HAVENS Contents 0 Prelude ii 1 Directional Derivatives, the Gradient and the Del Operator 1 1.1 Conceptual Review: Directional Derivatives and the Gradient........... 1 1.2 The Gradient as a Vector Field............................ 5 1.3 The Gradient Flow and Critical Points ....................... 10 1.4 The Del Operator and the Gradient in Other Coordinates*............ 17 1.5 Problems........................................ 21 2 Vector Fields in Low Dimensions 26 2 3 2.1 General Vector Fields in Domains of R and R . 26 2.2 Flows and Integral Curves .............................. 31 2.3 Conservative Vector Fields and Potentials...................... 32 2.4 Vector Fields from Frames*.............................. 37 2.5 Divergence, Curl, Jacobians, and the Laplacian................... 41 2.6 Parametrized Surfaces and Coordinate Vector Fields*............... 48 2.7 Tangent Vectors, Normal Vectors, and Orientations*................ 52 2.8 Problems........................................ 58 3 Line Integrals 66 3.1 Defining Scalar Line Integrals............................. 66 3.2 Line Integrals in Vector Fields ............................ 75 3.3 Work in a Force Field................................. 78 3.4 The Fundamental Theorem of Line Integrals .................... 79 3.5 Motion in Conservative Force Fields Conserves Energy .............. 81 3.6 Path Independence and Corollaries of the Fundamental Theorem......... 82 3.7 Green's Theorem.................................... 84 3.8 Problems........................................ 89 4 Surface Integrals, Flux, and Fundamental Theorems 93 4.1 Surface Integrals of Scalar Fields........................... 93 4.2 Flux........................................... 96 4.3 The Gradient, Divergence, and Curl Operators Via Limits* . 103 4.4 The Stokes-Kelvin Theorem..............................108 4.5 The Divergence Theorem ...............................112 4.6 Problems........................................114 List of Figures 117 i 11/14/19 Multivariate Calculus: Vector Calculus Havens 0.
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												  Laplace Transforms: Theory, Problems, and SolutionsLaplace Transforms: Theory, Problems, and Solutions Marcel B. Finan Arkansas Tech University c All Rights Reserved 1 Contents 43 The Laplace Transform: Basic Definitions and Results 3 44 Further Studies of Laplace Transform 15 45 The Laplace Transform and the Method of Partial Fractions 28 46 Laplace Transforms of Periodic Functions 35 47 Convolution Integrals 45 48 The Dirac Delta Function and Impulse Response 53 49 Solving Systems of Differential Equations Using Laplace Trans- form 61 50 Solutions to Problems 68 2 43 The Laplace Transform: Basic Definitions and Results Laplace transform is yet another operational tool for solving constant coeffi- cients linear differential equations. The process of solution consists of three main steps: • The given \hard" problem is transformed into a \simple" equation. • This simple equation is solved by purely algebraic manipulations. • The solution of the simple equation is transformed back to obtain the so- lution of the given problem. In this way the Laplace transformation reduces the problem of solving a dif- ferential equation to an algebraic problem. The third step is made easier by tables, whose role is similar to that of integral tables in integration. The above procedure can be summarized by Figure 43.1 Figure 43.1 In this section we introduce the concept of Laplace transform and discuss some of its properties. The Laplace transform is defined in the following way. Let f(t) be defined for t ≥ 0: Then the Laplace transform of f; which is denoted by L[f(t)] or by F (s), is defined by the following equation Z T Z 1 L[f(t)] = F (s) = lim f(t)e−stdt = f(t)e−stdt T !1 0 0 The integral which defined a Laplace transform is an improper integral.
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												  Numerical Methods in Multiple IntegrationNUMERICAL METHODS IN MULTIPLE INTEGRATION Dissertation for the Degree of Ph. D. MICHIGAN STATE UNIVERSITY WAYNE EUGENE HOOVER 1977 LIBRARY Michigan State University This is to certify that the thesis entitled NUMERICAL METHODS IN MULTIPLE INTEGRATION presented by Wayne Eugene Hoover has been accepted towards fulfillment of the requirements for PI; . D. degree in Mathematics w n A fl $11 “ W Major professor I (J.S. Frame) Dag Octdber 29, 1976 ., . ,_.~_ —- (‘sq I MAY 2T3 2002 ABSTRACT NUMERICAL METHODS IN MULTIPLE INTEGRATION By Wayne Eugene Hoover To approximate the definite integral 1:" bl [(1):] f(x1"”’xn)dxl”'dxn an a‘ over the n-rectangle, n R = n [41, bi] , 1' =1 conventional multidimensional quadrature formulas employ a weighted sum of function values m Q“) = Z ij(x,'1:""xjn)- i=1 Since very little is known concerning formulas which make use of partial derivative data, the objective of this investigation is to construct formulas involving not only the traditional weighted sum of function values but also partial derivative correction terms with weights of equal magnitude and alternate signs at the corners or at the midpoints of the sides of the domain of integration, R, so that when the rule is compounded or repeated, the weights cancel except on the boundary. For a single integral, the derivative correction terms are evaluated only at the end points of the interval of integration. In higher dimensions, the situation is somewhat more complicated since as the dimension increases the boundary becomes more complex. Indeed, in higher dimensions, most of the volume of the n-rectande lies near the boundary.
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												  Center of Mass, Torque and Rotational InertiaCenter of Mass, Torque and Rotational Inertia Objectives 1. Define center of mass, center of gravity, torque, rotational inertia 2. Give examples of center of gravity 3. Explain how center of mass affects rotation and toppling 4. Write the equations for torque and rotational inertia 5. Explain how to change torque and rotational inertia Center of Mass/Gravity • COM – point which is at the center of the objects mass – Middle of meter stick – Center of a ball – Middle of a donut • Donuts are yummy • COG – center of object’s weight distribution – Usually the same point as center of mass Rotation and Center of Mass • Objects rotate around their center of mass – Wobbling baseball bat tossed through the air • They also balance there – Balancing a broom on your finger • Things topple over when their center of gravity is not above the base – Leaning Tower of Pisa Torque • Force that causes rotation • Equation τ = Fr τ = torque (in Nm) F = force (in N) r = arm radius (in m) • How do you increase torque – More force – Longer radius Rotational Inertia • Resistance of an object to a change in its rotational motion • Controlled by mass distribution and location of axis • Equation I = mr2 I = rotational inertia (in kgm2) m = mass (in kg) r = radius (in m) • How do you increase rotational inertia? – Even mass distribution Angular Momentum • Measure how difficult it is to start or stop a rotating object • Equations L = Iω = mvtr • It is easier to balance on a moving bicycle • Precession – Torque applied to a spinning wheel changes the direction of its angular momentum – The wheel rotates about the axis instead of toppling over Satellite Motion John Glenn 6 min • Satellites “fall around” the object they orbit • The tangential speed must be exact to match the curvature of the surface of the planet – On earth things fall 4.9 m in one second – Earth “falls” 4.9 m every 8000 m horizontally – Therefore a satellite must have a tangential speed of 8000 m/s to keep from hitting the ground – Rockets are launched vertically and rolled to horizontal during their flights Sputnik-30 sec .
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												  Lecture 18, Structure of Spiral GalaxiesGALAXIES 626 Upcoming Schedule: Today: Structure of Disk Galaxies Thursday:Structure of Ellipticals Tuesday 10th: dark matter (Emily©s paper due) Thursday 12th :stability of disks/spiral arms Tuesday 17th: Emily©s presentation (intergalactic metals) GALAXIES 626 Lecture 17: The structure of spiral galaxies NGC 2997 - a typical spiral galaxy NGC 4622 yet another spiral note how different the spiral structure can be from galaxy to galaxy Elementary properties of spiral galaxies Milky Way is a ªtypicalº spiral radius of disk = 15 Kpc thickness of disk = 300 pc Regions of a Spiral Galaxy · Disk · younger generation of stars · contains gas and dust · location of the open clusters · Where spiral arms are located · Bulge · mixture of both young and old stars · Halo · older generation of stars · contains little gas and dust · location of the globular clusters Spiral Galaxies The disk is the defining stellar component of spiral galaxies. It is the end product of the dissipation of most of the baryons, and contains almost all of the baryonic angular momentum Understanding its formation is one of the most important goals of galaxy formation theory. Out of the galaxy formation process come galactic disks with a high level of regularity in their structure and scaling laws Galaxy formation models need to understand the reasons for this regularity Spiral galaxy components 1. Stars · 200 billion stars · Age: from >10 billion years to just formed · Many stars are located in star clusters 2. Interstellar Medium · Gas between stars · Nebulae, molecular clouds, and diffuse hot and cool gas in between 3. Galactic Center ± supermassive Black Hole 4.
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												  Chapter 8: Rotational MotionTODAY: Start Chapter 8 on Rotation Chapter 8: Rotational Motion Linear speed: distance traveled per unit of time. In rotational motion we have linear speed: depends where we (or an object) is located in the circle. If you ride near the outside of a merry-go-round, do you go faster or slower than if you ride near the middle? It depends on whether “faster” means -a faster linear speed (= speed), ie more distance covered per second, Or - a faster rotational speed (=angular speed, ω), i.e. more rotations or revolutions per second. • Linear speed of a rotating object is greater on the outside, further from the axis (center) Perimeter of a circle=2r •Rotational speed is the same for any point on the object – all parts make the same # of rotations in the same time interval. More on rotational vs tangential speed For motion in a circle, linear speed is often called tangential speed – The faster the ω, the faster the v in the same way v ~ ω. directly proportional to − ω doesn’t depend on where you are on the circle, but v does: v ~ r He’s got twice the linear speed than this guy. Same RPM (ω) for all these people, but different tangential speeds. Clicker Question A carnival has a Ferris wheel where the seats are located halfway between the center and outside rim. Compared with a Ferris wheel with seats on the outside rim, your angular speed while riding on this Ferris wheel would be A) more and your tangential speed less. B) the same and your tangential speed less.
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												  Galactic Mass Distribution Without Dark Matter Or Modified Newtonian1 astro-ph/0309762 v2, revised 1 Mar 2007 Galactic mass distribution without dark matter or modified Newtonian mechanics Kenneth F Nicholson, retired engineer key words: galaxies, rotation, mass distribution, dark matter Abstract Given the dimensions (including thickness) of a galaxy and its rotation profile, a method is shown that finds the mass and density distribution in the defined envelope that will cause that rotation profile with near-exact speed matches. Newton's law is unchanged. Surface-light intensity and dark matter are not needed. Results are presented in dimensionless plots allowing easy comparisons of galaxies. As compared with the previous version of this paper the methods are the same, but some data are presented in better dimensionless parameters. Also the part on thickness representation is simplified and extended, the contents are rearranged to have a logical buildup in the problem development, and more examples are added. 1. Introduction Methods used for finding mass distribution of a galaxy from rotation speeds have been mostly those using dark-matter spherical shells to make up the mass needed beyond the assumed loading used (as done by van Albada et al, 1985), or those that modify Newton's law in a way to approximately match measured data (for example MOND, Milgrom, 1983). However the use of the dark-matter spheres is not a correct application of Newton's law, and (excluding relativistic effects) modifications to Newton's law have not been justified. In the applications of dark-matter spherical shells it is assumed that all galaxies are in two parts, a thin disk with an exponential SMD loading (a correct solution for rotation speeds by Freeman, 1970) and a series of spherical shells centered on the galaxy center.
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												  Multiple IntegralsChapter 11 Multiple Integrals 11.1 Double Riemann Sums and Double Integrals over Rectangles Motivating Questions In this section, we strive to understand the ideas generated by the following important questions: What is a double Riemann sum? • How is the double integral of a continuous function f = f(x; y) defined? • What are two things the double integral of a function can tell us? • Introduction In single-variable calculus, recall that we approximated the area under the graph of a positive function f on an interval [a; b] by adding areas of rectangles whose heights are determined by the curve. The general process involved subdividing the interval [a; b] into smaller subintervals, constructing rectangles on each of these smaller intervals to approximate the region under the curve on that subinterval, then summing the areas of these rectangles to approximate the area under the curve. We will extend this process in this section to its three-dimensional analogs, double Riemann sums and double integrals over rectangles. Preview Activity 11.1. In this activity we introduce the concept of a double Riemann sum. (a) Review the concept of the Riemann sum from single-variable calculus. Then, explain how R b we define the definite integral a f(x) dx of a continuous function of a single variable x on an interval [a; b]. Include a sketch of a continuous function on an interval [a; b] with appropriate labeling in order to illustrate your definition. (b) In our upcoming study of integral calculus for multivariable functions, we will first extend 181 182 11.1.
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												  Dirac Function and Its Applications in Solving Some Problems in MathematicsDirac function and its applications in solving some problems in mathematics Hisham Rehman Mohammed Department of Mathematics Collage of computer science and Mathematics University of Al- Qadisiyia Diwaniya-Iraq E-mail:hisham [email protected] Abstract The paper presents various ways of defining and introducing Dirac delta function, its application in solving some problems and show the possibility of using delta- function in mathematics and physics. Introduction The development of science requires for its theoretical basis more and more "high mathematics", one of the achievements which are generalized functions, in particular the Dirac function. The theory of generalized functions is relevant in physics and mathematics, as have of remarkable properties that extend the classical mathematical analysis extends the range of tasks and, moreover, leads to significant simplifications in the calculations, automating basic operations. The objectives of this work: 1) study the concept of Dirac function; 2) to consider the physical and mathematical approaches to its definition; 3) show the application to the determination of derivatives of discontinuous functions. 1.1. Basic concepts. In various issues of mathematical analysis, the term "function" has to understand, with varying degrees of generality. Sometimes considered continuous but not differentiable functions, other issues have to assume that we are talking about functions, differentiable once or several times, etc. However, in some cases, the classical notion of function, even interpreted in the broadest sense,that is as an 1 arbitrary rule, which relates each value of x in the domain of this function, a number of y = f (x), is insufficient. That's an important example: using the apparatus of mathematical analysis to some problems, we are faced with a situation in which certain operations analysis are impractical, for example, a function that has no derivative (in some points or even everywhere), it is impossible to differentiate if derivatives are understood as an elementary function.