Mechanics Physics 151

Similar documents
Mechanics Physics 151

Mechanics Physics 151

Mechanics Physics 151

F(r) = r f (r) 4.8. Central forces The most interesting problems in classical mechanics are about central forces.

Classical Mechanics Homework set 7, due Nov 8th: Solutions

Lecture 23: Central Force Motion

AST 121S: The origin and evolution of the Universe. Introduction to Mathematical Handout 1

Physics 506 Winter 2006 Homework Assignment #9 Solutions

Kepler's 1 st Law by Newton

Tutorial Exercises: Central Forces

Math Notes on Kepler s first law 1. r(t) kp(t)

Chapter 13: Gravitation

= 4 3 π( m) 3 (5480 kg m 3 ) = kg.

AY 7A - Fall 2010 Section Worksheet 2 - Solutions Energy and Kepler s Law

Lecture 7: Angular Momentum, Hydrogen Atom

Newton s Laws, Kepler s Laws, and Planetary Orbits

DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS

Chapter 2: Basic Physics and Math Supplements

Gravitation. Chapter 12. PowerPoint Lectures for University Physics, Twelfth Edition Hugh D. Young and Roger A. Freedman. Lectures by James Pazun

Central Force Problem. Central Force Motion. Two Body Problem: Center of Mass Coordinates. Reduction of Two Body Problem 8.01 W14D1. + m 2. m 2.

Chapter 12. Kinetics of Particles: Newton s Second Law

KEPLER S LAWS AND PLANETARY ORBITS

Physics 181. Assignment 4

Chap 5. Circular Motion: Gravitation

AH Mechanics Checklist (Unit 2) AH Mechanics Checklist (Unit 2) Circular Motion

S7: Classical mechanics problem set 2

Experiment 09: Angular momentum

Scattering in Three Dimensions

Central Force Motion

KEPLER S LAWS OF PLANETARY MOTION

Radius of the Moon is 1700 km and the mass is 7.3x 10^22 kg Stone. Moon

Physics: Work & Energy Beyond Earth Guided Inquiry

Kepler s problem gravitational attraction

F 12. = G m m 1 2 F 21 = F 12. = G m 1m 2. Review. Physics 201, Lecture 22. Newton s Law Of Universal Gravitation

Extra notes for circular motion: Circular motion : v keeps changing, maybe both speed and

When a mass moves because of a force, we can define several types of problem.

Rigid Body Dynamics 2. CSE169: Computer Animation Instructor: Steve Rotenberg UCSD, Winter 2018

m1 m2 M 2 = M -1 L 3 T -2

Physics 235 Chapter 5. Chapter 5 Gravitation

r cos, and y r sin with the origin of coordinate system located at

OSCILLATIONS AND GRAVITATION

Phys-272 Lecture 17. Motional Electromotive Force (emf) Induced Electric Fields Displacement Currents Maxwell s Equations

Physics 161 Fall 2011 Extra Credit 2 Investigating Black Holes - Solutions The Following is Worth 50 Points!!!

MAGNETIC FIELD INTRODUCTION

Chapter 13 Gravitation

3D-Central Force Problems I

Pendulum in Orbit. Kirk T. McDonald Joseph Henry Laboratories, Princeton University, Princeton, NJ (December 1, 2017)

Math 124B February 02, 2012

Mechanics and Special Relativity (MAPH10030) Assignment 3

Lecture 1a: Satellite Orbits

SIO 229 Gravity and Geomagnetism. Lecture 6. J 2 for Earth. J 2 in the solar system. A first look at the geoid.

! E da = 4πkQ enc, has E under the integral sign, so it is not ordinarily an

Anyone who can contemplate quantum mechanics without getting dizzy hasn t understood it. --Niels Bohr. Lecture 17, p 1

Physics 2212 GH Quiz #2 Solutions Spring 2016

PHYSICS NOTES GRAVITATION

Potential Energy and Conservation of Energy

m 1 r = r 1 - r 2 m 2 r 2 m1 r1

HW Solutions # MIT - Prof. Please study example 12.5 "from the earth to the moon". 2GmA v esc

Chapter 22: Electric Fields. 22-1: What is physics? General physics II (22102) Dr. Iyad SAADEDDIN. 22-2: The Electric Field (E)

Physics 505 Homework No. 9 Solutions S9-1

PHYS Dynamics of Space Vehicles

This gives rise to the separable equation dr/r = 2 cot θ dθ which may be integrated to yield r(θ) = R sin 2 θ (3)

Kinematics in 2-D (II)

Orbital Angular Momentum Eigenfunctions

10. Force is inversely proportional to distance between the centers squared. R 4 = F 16 E 11.

Question 1: The dipole

The Schwartzchild Geometry

Final Review of AerE 243 Class

? this lecture. ? next lecture. What we have learned so far. a Q E F = q E a. F = q v B a. a Q in motion B. db/dt E. de/dt B.

= e2. = 2e2. = 3e2. V = Ze2. where Z is the atomic numnber. Thus, we take as the Hamiltonian for a hydrogenic. H = p2 r. (19.4)

(r) = 1. Example: Electric Potential Energy. Summary. Potential due to a Group of Point Charges 9/10/12 1 R V(r) + + V(r) kq. Chapter 23.

Electrostatics (Electric Charges and Field) #2 2010

b) (5) What average force magnitude was applied by the students working together?

Kinetic energy, work, and potential energy. Work, the transfer of energy: force acting through distance: or or

Physics 107 TUTORIAL ASSIGNMENT #8

Gravitation. AP/Honors Physics 1 Mr. Velazquez

Lecture 22. PE = GMm r TE = GMm 2a. T 2 = 4π 2 GM. Main points of today s lecture: Gravitational potential energy: Total energy of orbit:

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department. Problem Set 10 Solutions. r s

Physics 2B Chapter 22 Notes - Magnetic Field Spring 2018

PHYSICS 4E FINAL EXAM SPRING QUARTER 2010 PROF. HIRSCH JUNE 11 Formulas and constants: hc =12,400 ev A ; k B. = hf " #, # $ work function.

Physics 312 Introduction to Astrophysics Lecture 7


Between any two masses, there exists a mutual attractive force.

CHAPTER 25 ELECTRIC POTENTIAL

Rotational Motion: Statics and Dynamics

Faraday s Law (continued)

PS113 Chapter 5 Dynamics of Uniform Circular Motion

AP Physics - Coulomb's Law

m 2 r 1 = m 1 + m 2 M r 2 = m 1 = m 1m 2

ω = θ θ o = θ θ = s r v = rω

EM Boundary Value Problems

d 2 x 0a d d =0. Relative to an arbitrary (accelerating frame) specified by x a = x a (x 0b ), the latter becomes: d 2 x a d 2 + a dx b dx c

Calculate the electric potential at B d2=4 m Calculate the electric potential at A d1=3 m 3 m 3 m

= 1. For a hyperbolic orbit with an attractive inverse square force, the polar equation with origin at the center of attraction is

( ) [ ] [ ] [ ] δf φ = F φ+δφ F. xdx.

Ch 13 Universal Gravitation

is the instantaneous position vector of any grid point or fluid

20th Century Atomic Theory - Hydrogen Atom

Magnetic Field. Conference 6. Physics 102 General Physics II

10. Universal Gravitation

Transcription:

Mechanics Physics 151 Lectue 5 Cental Foce Poblem (Chapte 3)

What We Did Last Time Intoduced Hamilton s Pinciple Action integal is stationay fo the actual path Deived Lagange s Equations Used calculus of vaiation Discussed consevation laws Genealized (conugate) momentum Symmety Invaiance Momentum consevation We ae almost done with the basic concepts One moe thing to cove

Goals fo Today Enegy consevation Define enegy function Subtle diffeence fom the Newtonian vesion Cental foce poblem Fist application Motion of a paticle unde a cental foce Simplify the poblem using angula momentum consevation Discuss qualitative behavio of the solution Use enegy consevation Distinguish bounded/unbounded obits Actual solution Thusday

Enegy Consevation Conside time deivative of Lagangian dl( q, q, t) L dq L dq L = + + dt q dt q dt t Using Lagange s equation one can deive d L L q L + = dt q t Conseved if Lagangian does not depend explicitly on t L d L = q dt q Define this as enegy function hqqt (,, )

Enegy Function? Does enegy function epesent the total enegy? Let s ty an easy example fist Single paticle moving along x axis mx L= V( x) h= mx L mx = + V( x) = T + V How geneal is this? L hqqt (,, ) q L q Total enegy

Enegy Function Suppose L can be witten as L( q, q, t) = L ( q, t) + L ( q, q, t) + L ( q, q, t) Tue in most cases of inteest Deivatives satisfy L q = q 1 L q 1 = L 1 1 st ode in q q L q nd ode in q = L L hqqt (,, ) q L= L L q L hqqt (,, ) q L q Eule s theoem

Enegy Function hqqt (,, ) = L L L= T V Enegy function equals to the total enegy T + V if T L and = V = L 1 st condition is satisfied if tansfomation fom i to q is time-independent nd condition holds if the potential is velocity-independent No fictions Fiction would dissipate enegy Let s look into the 1 st condition

Kinetic Enegy mi T = i i Using the chain ule This wouldn t wok if = ( q,..., q, t) because d i dt = ( q,..., q ) i i 1 n d = q dt i = q i i 1 n i q i q i + t Time-independent m m m = qq = qq i i i i i i i i k k i i k, q qk k, i q qk nd ode homogeneous No q

Enegy Consevation L hqqt (,, ) q L q Enegy function equals to the total enegy if Constaints ae time-independent Kinetic enegy T is nd ode homogeneous function of the velocities Potential V is velocity-independent Enegy function is conseved if Lagangian does not depend explicitly on time These ae estatement of the enegy consevation theoem in a moe geneal famewok Conditions ae clealy defined

Cental Foce Poblem Conside a paticle unde a cental foce Foce F paallel to Assume F is consevative V is function of if F is cental Such systems ae quite common Planet aound the Sun Satellite aound the Eath Electon aound a nucleus F = V() These examples assume the body at the cente is heavy and does not move O F m

Two-Body Poblem Conside two paticles without extenal foce 1 and elative to cente of mass Lagangian is L Motion of CoM ( m + m ) R m 1 i i = + i= 1 Motion of paticles aound CoM V() m 1 O R 1 CoM m Potential is function of = 1 Stong law of action and eaction m m ( ) 1 1 = = ( m1+ m) m1+ m mi i 1 mm 1 = i= 1 m1+ m ( )

Two-Body Cental Foce L ( m + m ) R 1 mm ( m + m ) 1 1 = + R is cyclic 1 V() CoM moves at a constant velocity Move O to CoM and foget about it m 1 O R CoM m L 1 mm ( m + m ) = 1 1 V() Relative motion of two paticles is identical to the motion of one paticle in a cental-foce potential mm 1 Reduced mass µ = o ( m m ) 1 1 1 µ = m + m 1+ 1

Hydogen and Positonium Positonium is a bound state of a positon and an electon Simila to hydogen except m(p) >> m(e + ) Potential V() is identical Tun them into cental foce poblem µ = mm e e me positonium ( me + me) = µ = mm p e hydogen me ( m + m ) p Spectum of positonium identical to hydogen with m e m e / e e e + e p q V() =

Spheical Symmety Cental-foce system is spheically symmetic It can be otated aound any axis though the oigin Lagangian L= T( ) V( ) doesn t depend on the diection L= p=const Diection of L is fixed L by definition is always in a plane Angula momentum is conseved Choose pola coodinates Pola axis = diection of L = (, θ, ψ) = (, θ) Azimuth Zenith = 1/π L O

Moe Fomally Lagangian in pola coodinates θ is cyclic, but ψ is not We can choose the pola axis so that the initial condition is Now ψ is constant. We can foget about it = (, θ, ψ ) m L= T V = + + V d L L dt ψ ψ ( sin ψθ ψ ) ( ) ( sin cos ) = m ψ ψ ψθ = ψ = π, ψ = nd tem vanishes ψ =

Angula Momentum m L= T V = + V θ is cyclic. Conugate momentum p θ conseves Altenatively ( θ ) ( ) L = = = θ pθ m θ const l Aeal velocity Keple s nd law da dt 1 = θ = Tue fo any cental foce const Magnitude of angula momentum d da

Radial Motion m L = T V = + V ( θ ) ( ) Lagange s equation fo Deivative of V is the foce m = m θ + f () Centifugal foce Using the angula momentum l l m = + f () 3 m d dt V() ( m ) m θ + = Cental foce V() f() = l = We know how to integate this. But we also know what we ll get by integating this m θ

Enegy Consevation 1 E = T + V = m + + V = m + l + V = m ( θ ) ( ) ( ) const l = E V() m m One can solve this (in pinciple) by t d t = dt = = t() l E V() m m Then invet t() (t) Then calculate θ(t) by integating 1 st ode diffeential equation of θ = l m NB: This neve goes negative Done! (?)

Degees of Feedom A paticle has 3 degees of feedom Eqn of motion is nd ode diffeential 6 constants Each consevation law educes one diffeentiation By saying time-deivative equals zeo We used L and E 4 conseved quantities Left with constants of integation = and θ We don t have to use consevation laws It s ust easie than solving all of Lagange s equations

Qualitative Behavio Integating the adial motion isn t always easy Moe often impossible You can still tell geneal behavio by looking at E V () V() + l m Enegy E is conseved, and E V must be positive m = + V () m Plot V () and see how it intesects with E l = E V() m m Quasi potential including the centifugal foce = E V () > E > V ()

Invese-Squae Foce Conside an attactive 1/ foce k k f() = V() = Gavity o electostatic foce k l V () = + m 1/ foce dominates at lage Centifugal foce dominates at small A dip foms in the middle V () l m k

Unbounded Motion Take V simila to 1/ case Only geneal featues ae elevant E = E 1 > min E = V ( ) 1 min Paticle can go infinitely fa E 1 V () 1 m Aive fom = E Tuning point E = V = Go towad = E 3 A 1/ foce would make a hypebola

Bounded Motion E = E min < < max Paticle is confined between two cicles E 1 V () Goes back and foth between two adii E 1 m E 3 Obit may o may not be closed. (This one isn t) A 1/ foce would make an ellipse

Cicula Motion E = E 3 = (fixed) Only one adius is allowed Stays on a cicle Classification into unbounded, bounded and cicula motion depends on the geneal shape of V Not on the details (1/ o othewise) E = V ( ) = = const = E 1 E E 3 V ()

Anothe Example V a = f = 3 4 Attactive -4 foce V has a bump 3a Paticle with enegy E may be eithe bounded o unbounded, depending on the initial a V = + l m 3 E V l m V

Stable Cicula Obit Cicula obit occus at the bottom of a dip of V m = E V = Top of a bump woks in theoy, but it is unstable Initial condition must be exactly = and = = const Stable cicula obit equies dv m = = d dv d > E E stable unstable

Powe Law Foce V () V() + l m dv d = l = f( ) = 3 m dv df 3l = + > d d m 4 = = df d = < 3 f( ) Suppose the foce has a fom k > fo attactive foce Condition fo stable cicula obit is n 1 n 1 kn < 3k n > 3 f = k Powe-law foces with n > 3 can make stable cicula obit n

Summay Stated discussing Cental Foce Poblems Reduced -body poblem into cental foce poblem l m = + f () 3 m Poblem is educed to one equation Used angula momentum consevation l V () V() + m Unbounded, bounded, and cicula obits Condition fo stable cicula obits Qualitative behavio depends on Next step: Can we actually solve fo the obit?