Simple Relativity Approach to Special Relativity
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Classical Mechanics
Classical Mechanics Hyoungsoon Choi Spring, 2014 Contents 1 Introduction4 1.1 Kinematics and Kinetics . .5 1.2 Kinematics: Watching Wallace and Gromit ............6 1.3 Inertia and Inertial Frame . .8 2 Newton's Laws of Motion 10 2.1 The First Law: The Law of Inertia . 10 2.2 The Second Law: The Equation of Motion . 11 2.3 The Third Law: The Law of Action and Reaction . 12 3 Laws of Conservation 14 3.1 Conservation of Momentum . 14 3.2 Conservation of Angular Momentum . 15 3.3 Conservation of Energy . 17 3.3.1 Kinetic energy . 17 3.3.2 Potential energy . 18 3.3.3 Mechanical energy conservation . 19 4 Solving Equation of Motions 20 4.1 Force-Free Motion . 21 4.2 Constant Force Motion . 22 4.2.1 Constant force motion in one dimension . 22 4.2.2 Constant force motion in two dimensions . 23 4.3 Varying Force Motion . 25 4.3.1 Drag force . 25 4.3.2 Harmonic oscillator . 29 5 Lagrangian Mechanics 30 5.1 Configuration Space . 30 5.2 Lagrangian Equations of Motion . 32 5.3 Generalized Coordinates . 34 5.4 Lagrangian Mechanics . 36 5.5 D'Alembert's Principle . 37 5.6 Conjugate Variables . 39 1 CONTENTS 2 6 Hamiltonian Mechanics 40 6.1 Legendre Transformation: From Lagrangian to Hamiltonian . 40 6.2 Hamilton's Equations . 41 6.3 Configuration Space and Phase Space . 43 6.4 Hamiltonian and Energy . 45 7 Central Force Motion 47 7.1 Conservation Laws in Central Force Field . 47 7.2 The Path Equation . -
Resolution of the Ehrenfest Paradox in the Dynamic Interpretation of Lorentz Invariance F
Resolution of the Ehrenfest Paradox in the Dynamic Interpretation of Lorentz Invariance F. Winterberg University of Nevada, Reno, Nevada 89557-0058, USA Z. Naturforsch. 53a, 751-754 (1998); received July 14, 1998 In the dynamic Lorentz-Poincare interpretation of Lorentz invariance, clocks in absolute motion through a preferred reference system (resp. aether) suffer a true contraction and clocks, as a result of this contraction, go slower by the same amount. With the one-way velocity of light unobservable, there is no way this older pre-Einstein interpretation of special relativity can be tested, except in cases involv- ing rotational motion, where in the Lorentz-Poincare interpretation the interaction symmetry with the aether is broken. In this communication it is shown that Ehrenfest's paradox, the Lorentz contraction of a rotating disk, has a simple resolution in the dynamic Lorentz-Poincare interpretation of Lorentz invariance and can perhaps be tested against the prediction of special relativity. One of the oldest and least understood paradoxes of contraction. With all clocks understood as light clocks special relativity is the Ehrenfest paradox [ 1 ], the Lorentz made up of Lorentz-contraded rods, clocks in absolute contraction of a rotating disk, whereby the ratio of cir- motion go slower by the same amount. For an observer cumference of the disk to its diameter should become less in absolute motion against the preferred reference than n. The paradox gave Einstein the idea that in accel- system, the contraction and time dilation observed on an erated frames of reference the metric is non-euclidean object at rest in this reference system is there explained and that by reason of his principle of equivalence the as an illusion caused by the Lorentz contraction and time same should be true in the presence of gravitational fields. -
6. Non-Inertial Frames
6. Non-Inertial Frames We stated, long ago, that inertial frames provide the setting for Newtonian mechanics. But what if you, one day, find yourself in a frame that is not inertial? For example, suppose that every 24 hours you happen to spin around an axis which is 2500 miles away. What would you feel? Or what if every year you spin around an axis 36 million miles away? Would that have any e↵ect on your everyday life? In this section we will discuss what Newton’s equations of motion look like in non- inertial frames. Just as there are many ways that an animal can be not a dog, so there are many ways in which a reference frame can be non-inertial. Here we will just consider one type: reference frames that rotate. We’ll start with some basic concepts. 6.1 Rotating Frames Let’s start with the inertial frame S drawn in the figure z=z with coordinate axes x, y and z.Ourgoalistounderstand the motion of particles as seen in a non-inertial frame S0, with axes x , y and z , which is rotating with respect to S. 0 0 0 y y We’ll denote the angle between the x-axis of S and the x0- axis of S as ✓.SinceS is rotating, we clearly have ✓ = ✓(t) x 0 0 θ and ✓˙ =0. 6 x Our first task is to find a way to describe the rotation of Figure 31: the axes. For this, we can use the angular velocity vector ! that we introduced in the last section to describe the motion of particles. -
Special Relativity Announcements: • Homework Solutions Will Soon Be Culearn • Homework Set 1 Returned Today
Special relativity Announcements: • Homework solutions will soon be CULearn • Homework set 1 returned today. • Homework #2 is due today. • Homework #3 is posted – due next Wed. • First midterm is 2 weeks from Christian Doppler tomorrow. (1803—1853) Today we will investigate the relativistic Doppler effect and look at momentum and energy. http://www.colorado.edu/physics/phys2170/ Physics 2170 – Fall 2013 1 Clickers Unmatched • #12ACCD73 • #3378DD96 • #3639101F • #36BC3FB5 Need to register your clickers for me to be able to associate • #39502E47 scores with you • #39BEF374 • #39CAB340 • #39CEDD2A http://www.colorado.edu/physics/phys2170/ Physics 2170 – Fall 2013 2 Clicker question 4 last lecture Set frequency to AD A spacecraft travels at speed v=0.5c relative to the Earth. It launches a missile in the forward direction at a speed of 0.5c. How fast is the missile moving relative to Earth? This actually uses the A. 0 inverse transformation: B. 0.25c C. 0.5c Have to keep signs straight. Depends on D. 0.8c which way you are transforming. Also, E. c the velocities can be positive or negative! Best way to solve these is to figure out if the speeds add or subtract and then use the appropriate formula. Since the missile if fired forward in the spacecraft frame, the spacecraft and missile velocities add in the Earth frame. http://www.colorado.edu/physics/phys2170/ Physics 2170 – Fall 2013 3 Velocity addition works with light too! A Spacecraft moving at 0.5c relative to Earth sends out a beam of light in the forward direction. What is the light velocity in the Earth frame? What about if it sends the light out in the backward direction? It works. -
Frame of Reference
Frame of Reference Ineral frame of reference– • a reference frame with a constant speed • a reference frame that is not accelerang • If frame “A” has a constant speed with respect to an ineral frame “B”, then frame “A” is also an ineral frame of reference. Newton’s 3 laws of moon are valid in an ineral frame of reference. Example: We consider the earth or the “ground” as an ineral frame of reference. Observing from an object in moon with a constant speed (a = 0) is an ineral frame of reference A non‐ineral frame of reference is one that is accelerang and Newton’s laws of moon appear invalid unless ficous forces are used to describe the moon of objects observed in the non‐ineral reference frame. Example: If you are in an automobile when the brakes are abruptly applied, then you will feel pushed toward the front of the car. You may actually have to extend you arms to prevent yourself from going forward toward the dashboard. However, there is really no force pushing you forward. The car, since it is slowing down, is an accelerang, or non‐ineral, frame of reference, and the law of inera (Newton’s 1st law) no longer holds if we use this non‐ineral frame to judge your moon. An observer outside the car however, standing on the sidewalk, will easily understand that your moon is due to your inera…you connue your path of moon unl an opposing force (contact with the dashboard) stops you. No “fake force” is needed to explain why you connue to move forward as the car stops. -
Linear Momentum
p-1 Linear Momentum Definition: Linear momentum of a mass m moving with velocity v : p m v Momentum is a vector. Direction of p = direction of velocity v. units [p] = kgm/s (no special name) (No one seems to know why we use the symbol p for momentum, except that we couldn't use "m" because that was already used for mass.) Definition: Total momentum of several masses: m1 with velocity v1 , m2 with velocity v2, etc.. ptot p i p 1 p 2 m 1 v 1 m 2 v 2 i Momentum is an extremely useful concept because total momentum is conserved in a system isolated from outside forces. Momentum is especially useful for analyzing collisions between particles. Conservation of Momentum: You can never create or destroy momentum; all we can do is transfer momentum from one object to another. Therefore, the total momentum of a system of masses isolated from external forces (forces from outside the system) is constant in time. Similar to Conservation of Energy – always true, no exceptions. We will give a proof that momentum is conserved later. Two objects, labeled A and B, collide. v = velocity before collision, v' (v-prime) = velocity after collision. mA vA mA vA' collide v mB mB B vB' Before After Conservation of momentum guarantees that ptot m AA v m BB v m AA v m BB v . The velocities of all the particles changes in the collision, but the total momentum does not change. 10/17/2013 ©University of Colorado at Boulder p-2 Types of collisions elastic collision : total KE is conserved (KE before = KE after) superball on concrete: KE just before collision = KE just after (almost!) The Initial KE just before collision is converted to elastic PE as the ball compresses during the first half of its collision with the floor. -
Physics 3550, Fall 2012 Two Body, Central-Force Problem Relevant Sections in Text: §8.1 – 8.7
Two Body, Central-Force Problem. Physics 3550, Fall 2012 Two Body, Central-Force Problem Relevant Sections in Text: x8.1 { 8.7 Two Body, Central-Force Problem { Introduction. I have already mentioned the two body central force problem several times. This is, of course, an important dynamical system since it represents in many ways the most fundamental kind of interaction between two bodies. For example, this interaction could be gravitational { relevant in astrophysics, or the interaction could be electromagnetic { relevant in atomic physics. There are other possibilities, too. For example, a simple model of strong interactions involves two-body central forces. Here we shall begin a systematic study of this dynamical system. As we shall see, the conservation laws admitted by this system allow for a complete determination of the motion. Many of the topics we have been discussing in previous lectures come into play here. While this problem is very instructive and physically quite important, it is worth keeping in mind that the complete solvability of this system makes it an exceptional type of dynamical system. We cannot solve for the motion of a generic system as we do for the two body problem. The two body problem involves a pair of particles with masses m1 and m2 described by a Lagrangian of the form: 1 2 1 2 L = m ~r_ + m ~r_ − V (j~r − ~r j): 2 1 1 2 2 2 1 2 Reflecting the fact that it describes a closed, Newtonian system, this Lagrangian is in- variant under spatial translations, time translations, rotations, and boosts.* Thus we will have conservation of total energy, total momentum and total angular momentum for this system. -
Einstein's Apple: His First Principle of Equivalence
Einstein’s Apple 1 His First Principle of Equivalence August 13, 2012 Engelbert Schucking Physics Department New York University 4 Washington Place New York, NY 10003 [email protected] Eugene J. Surowitz Visiting Scholar New York University New York, NY 10003 [email protected] Abstract After a historical discussion of Einstein’s 1907 principle of equivalence, a homogeneous gravitational field in Minkowski spacetime is constructed. It is pointed out that the reference frames in gravitational theory can be understood as spaces with a flat connection and torsion defined through teleparallelism. This kind of torsion was first introduced by Einstein in 1928. The concept of torsion is discussed through simple examples and some historical observations. arXiv:gr-qc/0703149v2 9 Aug 2012 1The text of this paper has been incorporated as various chapters in a book of the same name, that is, Einstein’s Apple; which is available for download as a PDF on Schucking’s NYU Physics Department webpage http://physics.as.nyu.edu/object/EngelbertSchucking.html 1 1 The Principle of Equivalence In a speech given in Kyoto, Japan, on December 14, 1922 Albert Einstein remembered: “I was sitting on a chair in my patent office in Bern. Suddenly a thought struck me: If a man falls freely, he would not feel his weight. I was taken aback. The simple thought experiment made a deep impression on me. It was what led me to the theory of gravity.” This epiphany, that he once termed “der gl¨ucklichste Gedanke meines Lebens ” (the happiest thought of my life), was an unusual vision in 1907. -
Relative Motion of Orbiting Bodies
Relative motion of orbiting bodies Eugene I Butikov St. Petersburg State University, St. Petersburg, Russia E-mail: [email protected] Abstract. A problem of relative motion of orbiting bodies is investigated on the example of the free motion of any body ejected from the orbital station that stays in a circular orbit around the earth. An elementary approach is illustrated by a simulation computer program and supported by a mathematical treatment based on approximate differential equations of the relative orbital motion. 1. Relative motion of bodies in space orbits—an introductory approach Let two satellites orbit the earth. We know that their passive orbital motion obeys Kepler’s laws. But how does one of them move relative to the other? This relative motion is important, say, for the spacecraft docking in orbit. If two satellites are brought together but have a (small) nonzero relative velocity, they will drift apart nonrectilinearly. In unusual conditions of the orbital flight, navigation is quite different from what we are used to here on the earth, and our intuition fails us. The study of the relative motion of the spacecraft reveals many extraordinary features that are hard to reconcile with common sense and our everyday experience. In this paper we discuss the problem of passive relative motion of orbiting bodies on the specific example of the free motion of any body that is ejected from the orbital station that stays in a circular orbit. The free motion of an astronaut in the vicinity of an orbiting spacecraft has been investigated in [1]. The discussion in [1] is restricted to a low relative speed and short elapsed time (constituting a small fraction of the orbital period). -
Arxiv:1904.12755V1 [Cond-Mat.Soft] 29 Apr 2019 and Microorganisms As Well As Inanimate Synthetic Parti- Noise Is the Same in Both Frames
Active particles in non-inertial frames: how to self-propel on a carousel Hartmut L¨owen1 1Institut f¨urTheoretische Physik II: Weiche Materie, Heinrich-Heine-Universit¨atD¨usseldorf,D-40225 D¨usseldorf, Germany (Dated: April 30, 2019) Typically the motion of self-propelled active particles is described in a quiescent environment establishing an inertial frame of reference. Here we assume that friction, self-propulsion and fluc- tuations occur relative to a non-inertial frame and thereby the active Brownian motion model is generalized to non-inertial frames. First, analytical solutions are presented for the overdamped case, both for linear swimmers and circle swimmers. For a frame rotating with constant angular velocity ("carousel"), the resulting noise-free trajectories in the static laboratory frame trochoids if these are circles in the rotating frame. For systems governed by inertia, such as vibrated granulates or active complex plasmas, centrifugal and Coriolis forces become relevant. For both linear and cir- cling self-propulsion, these forces lead to out-spiraling trajectories which for long times approach a spira mirabilis. This implies that a self-propelled particle will typically leave a rotating carousel. A navigation strategy is proposed to avoid this expulsion, by adjusting the self-propulsion direction at wish. For a particle, initially quiescent in the rotating frame, it is shown that this strategy only works if the initial distance to the rotation centre is smaller than a critical radius Rc which scales with the self-propulsion velocity. Possible experiments to verify the theoretical predictions are discussed. I. INTRODUCTION ments [14{20]. In this paper, we consider self-propelled particles in a One of the basic principles of classical mechanics is non-inertial frame of reference such as a rotating sub- that Newton's second law holds only in inertial frames strate ("carousel"). -
Talking at Cross-Purposes. How Einstein and Logical Empiricists Never Agreed on What They Were Discussing About
Talking at Cross-Purposes. How Einstein and Logical Empiricists never Agreed on what they were Discussing about Marco Giovanelli Abstract By inserting the dialogue between Einstein, Schlick and Reichenbach in a wider network of debates about the epistemology of geometry, the paper shows, that not only Einstein and Logical Empiricists came to disagree about the role, principled or provisional, played by rods and clocks in General Relativity, but they actually, in their life-long interchange, never clearly identified the problem they were discussing. Einstein’s reflections on geometry can be understood only in the context of his “measuring rod objection” against Weyl. Logical Empiricists, though carefully analyzing the Einstein-Weyl debate, tried on the contrary to interpret Einstein’s epistemology of geometry as a continuation of the Helmholtz-Poincaré debate by other means. The origin of the misunderstanding, it is argued, should be found in the failed appreciation of the difference between a “Helmhotzian” and a “Riemannian” tradition. The epistemological problems raised by General Relativity are extraneous to the first tradition and can only be understood in the context of the latter, whose philosophical significance, however, still needs to be fully explored. Keywords: Logical Empiricism Moritz Schlick, Hans Reichenbach, Albert Einstein, Hermann Weyl, Epistemology of Geometry 1. Introduction on the notion of rigid bodies in Special Relativity (§2.1) and most of all those between Einstein, Herman Weyl Mara Beller in her classical Quantum dialogue (Beller, and Walter Dellänbach (§3) on the role of rigid rods and 1999) famously suggested a “dialogical” approach to the clocks in General Relativity (§2.2) around the 1920s. -
Special Relativity Based on Minkowski Formula
Special Relativity based on Minkowski formula Introduction and relevance The theory of Special Relativity (SR) as published by Albert Einstein in 1905 is based on the Lorentz transformation. The accomplishments of SR are found in many areas: time dilation, energy in mass ( E = m.c 2), and the relativistic Doppler Effect. However, Henrik Lorentz objected to the use of his transformation to two equal reference frames and Ehrenfest objected to the resulting deformation of a rigid cylinder (Ehrenfest paradox). In 1908, Hermann Minkowski developed his own variation of SR based on a proper observer travelling within a dominant reference frame. This formula differs from the Lorentz transformation in two ways: 1) the proper observer has a very limited reference frame, which is subservient to the larger reference frame, and 2) the speed of the proper observer can vary, it is a differential formula. Albert Einstein did not use the Lorentz transformation as the basis of his theory of General Relativity (GR), but chose to use Minkowski’s differential formula. In other words, Einstein must have listened to both Lorentz and Ehrenfest. This article is about the changes in SR caused by the change of formula to Minkowski’s formula. This change solves the twin, clock, and Ehrenfest paradox of SR. Differential Minkowski formula of SR The formula is as follows: 2 2 2 2 2 2 2 2 2 ds = c .dt 0 = c .dt – dx – dy – dz [m0 ] Minkowski space (1) In this formula is “ ds ” the line element, “c” the speed of light, “ dt 0” the time difference as measured by a travelling proper observer, “dt” the time difference on the synchronized clocks within the larger Euclidean reference frame, and are “dx”, “dy”, and “dz” the movements of the proper observer in time “dt”.