1 Class #22 Celestial engineering Central Forces DVD The power of Equivalent 1-D problem and Pseudopotential  Kepler’s 3 rd law Orbits and Energy  The.

Slides:



Advertisements
Similar presentations
UNIT 6 (end of mechanics) Universal Gravitation & SHM
Advertisements

Review Chap. 12 Gravitation
The Beginning of Modern Astronomy
ASTR100 (Spring 2008) Introduction to Astronomy Newton’s Laws of Motion Prof. D.C. Richardson Sections
ASTRONOMY 161 Introduction to Solar System Astronomy Class 8.
1 Class #18 of 30 Celestial engineering Central Forces DVD The power of Equivalent 1-D problem and Pseudopotential  Kepler’s 3 rd law Orbits and Energy.
1 Class #19 Central Force Motion Gravitational law Properties of Inverse-square forces Center of Mass motion Lagrangian for Central forces Reduced Mass.
1 Class #24 of 30 Exam -- Tuesday Additional HW problems posted Friday (also due Tuesday). Bring Index Card #3. Office hours on Monday 3:30-6:00 Topics.
1 Class #20 The power of Equivalent 1-D problem and Pseudopotential  Kepler’s 3 rd law Orbits and Energy  The earth-moon flywheel :02.
1 Class #17 of 30 Central Force Motion Gravitational law Properties of Inverse-square forces Center of Mass motion Lagrangian for Central forces Reduced.
1 Class #19 of 30 Celestial engineering - II Reduced 2-body problem Kepler 1 st, 2 nd and 3 rd laws Cometary collision prediction A whiff of scattering.
Kepler’s Laws of Planetary Motion Newton’s Laws of Gravity
Conservation of Momentum
R F For a central force the position and the force are anti- parallel, so r  F=0. So, angular momentum, L, is constant N is torque Newton II, angular.
NJIT Physics 320: Astronomy and Astrophysics – Lecture II Carsten Denker Physics Department Center for Solar–Terrestrial Research.
1 Class #23 Celestial engineering Kepler’s Laws Energy, angular momentum and Eccentricity.
1 Class #20 of 30 Celestial engineering Clarification on scattering angles Rotating reference frames Vector angular velocity Newton’s laws on rotating.
Department of Physics and Applied Physics , F2010, Lecture 10 Physics I LECTURE 10 3/3/10.
Planets Along the Ecliptic. Retrograde Motion Retrograde Motion Explained.
Chapter 12 Gravitation. Theories of Gravity Newton’s Einstein’s.
Newton’s Laws of Motion and Planetary Orbits Gravity makes the solar system go round.
Chapter 12.
Sect. 13.3: Kepler’s Laws & Planetary Motion. German astronomer (1571 – 1630) Spent most of his career tediously analyzing huge amounts of observational.
Unless otherwise noted, the content of this course material is licensed under a Creative Commons BY 3.0 License.
Universal Gravitation
Gravity & orbits. Isaac Newton ( ) developed a mathematical model of Gravity which predicted the elliptical orbits proposed by Kepler Semi-major.
Kinetics of Particles:
Osculating Circles and Trajectories Just Kidding.
Special Applications: Central Force Motion
Typical interaction between the press and a scientist?!
Lecture 5: Gravity and Motion
Kepler’s first law of planetary motion says that the paths of the planets are A. Parabolas B. Hyperbolas C. Ellipses D. Circles Ans: C.
Two-Body Systems.
Physics 201: Lecture 24, Pg 1 Chapter 13 The beautiful rings of Saturn consist of countless centimeter-sized ice crystals, all orbiting the planet under.
MA4248 Weeks 4-5. Topics Motion in a Central Force Field, Kepler’s Laws of Planetary Motion, Couloumb Scattering Mechanics developed to model the universe.
Homework 1 due Tuesday Jan 15. Celestial Mechanics Fun with Kepler and Newton Elliptical Orbits Newtonian Mechanics Kepler’s Laws Derived Virial Theorem.
Lecture 4: Gravity and Motion Describing Motion Speed (miles/hr; km/s) Velocity (speed and direction) Acceleration (change in velocity) Units: m/s 2.
Orbits Read Your Textbook: Foundations of Astronomy –Chapter 5 Homework Problems –Review Questions: 3, 4, 5, 9, 10 –Review Problems: 1, 3, 4 –Web Inquiries:
Gravitation. Gravitational Force and Field Newton proposed that a force of attraction exists between any two masses. This force law applies to point masses.
The Two-Body Problem. The two-body problem The two-body problem: two point objects in 3D interacting with each other (closed system) Interaction between.
Ast 1001 lecture Sept 13 (kd). 4. How Orbits Work Astronomy 1001, Sept 2007 – Prof. K. Davidson.
ASTRONOMY 340 FALL 2007 Class #2 6 September 2007.
Monday, Oct. 6, 2003PHYS , Fall 2003 Dr. Jaehoon Yu 1 PHYS 1443 – Section 003 Lecture #11 Newton’s Law of Gravitation Kepler’s Laws Work Done by.
Gravitational Field Historical facts Geocentric Theory Heliocentric Theory – Nicholas Copernicus (1473 – 1543) Nicholas Copernicus – All planets, including.
Planetary Orbits Planetary orbits in terms of ellipse geometry. In the figure, ε  e Compute major & minor axes (2a & 2b) as in text. Get (recall k =
Newton’s Law of Universal Gravitation
Sect. 3.7: Kepler Problem: r -2 Force Law Inverse square law force: F(r) = -(k/r 2 ); V(r) = -(k/r) –The most important special case of Central Force.
EART 160: Planetary Science First snapshot of Mercury taken by MESSENGER Flyby on Monday, 14 January 2008 Closest Approach: 200 km at 11:04:39 PST
Chapter 13 Gravitation Newton’s Law of Gravitation Here m 1 and m 2 are the masses of the particles, r is the distance between them, and G is the.
Spring 2002 Lecture #21 Dr. Jaehoon Yu 1.Kepler’s Laws 2.The Law of Gravity & The Motion of Planets 3.The Gravitational Field 4.Gravitational.
T. K. Ng, HKUST Lecture III: (1)Reference frame problem: Coriolis force (2)Circular motion and angular momentum (3)Planetary motion (Kepler ’ s Laws)
Q12.1 The mass of the Moon is 1/81 of the mass of the Earth.
Kepler’s Laws & Planetary Motion
Lecture 4 Stellar masses. Spectroscopy Obtaining a spectrum of a star allows you to measure: 1.Chemical composition 2.Distance (via spectral parallax)
Section Orbital Motion of Satellites and Kepler’s Laws
Celestial Mechanics I Introduction Kepler’s Laws.
The Motion of Planets Kepler’s laws Johannes Kepler.
Chapter 13 Gravitation & 13.3 Newton and the Law of Universal Gravitation Newton was an English Scientist He wanted to explain why Kepler’s Laws.
PHYS 2006 Tim Freegarde Classical Mechanics. 2 Newton’s law of Universal Gravitation Exact analogy of Coulomb electrostatic interaction gravitational.
Physics 141Mechanics Lecture 18 Kepler's Laws of Planetary Motion Yongli Gao The motion of stars and planets has drawn people's imagination since the.
Kepler’s Third Law Applied to Our Solar System
PHYSICS 197 Section 1 Chapter N11 Kepler’s Laws
Chapter 13 Universal Gravitation
Kepler’s Laws of Planetary Motion Newton’s Laws of Gravity
Eccentricity Notes.
Gravitational Fields, Circular Orbits and Kepler
Chapter 2 - Part 1 The two body problem
Gravitational Fields, Circular Orbits and Kepler’s Laws
Kepler’s Laws of Planetary Motion
Presentation transcript:

1 Class #22 Celestial engineering Central Forces DVD The power of Equivalent 1-D problem and Pseudopotential  Kepler’s 3 rd law Orbits and Energy  The earth-moon flywheel Energy and Eccentricity :02

2 Two particles with central forces

3 The power of :20

4 The power of - part 2 :25

5 Equivalent 1-D problem :30 Relative Lagrangian Radial equation Total Radial Force

6 Pseudopotential and Energy :35

7 Pseudopotential and Energy :37

8 Earth and Moon 1. What is the reduced mass for the earth-moon system (in kg)? 2. How many percent different is it than the lunar mass 3. What is theta-dot? 4. What is the radius of a circular orbit? 5. How would this change if the earth were fixed in space by the hand of God or a Borg tractor beam?

9 Orbital Energy :47 1. Last class we derived values for omega, mu and r for the earth- moon system 2. Total energy consumption on Earth is 1000 Terajoules/day 3. If we could power human activites by stealing the angular kinetic energy from the earth-moon system, how much should omega change to give us 100 years of power?

10 Converting. :30

11 Properties of ellipses :30

12 E, L and Eccentricity :30 The physics is in E and L. Epsilon is purely a geometrical factor. Epsilon equation applies to ALL conic sections (hyperbolae, ellipses, parabolas).

13 Energy and Eccentricity :30 EccentricityEnergyOrbit E<0 Circle E<0 Ellipse E=0 Parabola E>0 hyperbola

14 Kepler’s 1 st, 2 nd and 3 rd laws (1610) :37 1 st Law – Planets move in ellipses with sun at one focus Third law demonstrated previously relates period to semi-minor radius 2 nd law is direct consequence of momentum conservation “Equal areas are swept out in equal times” True for ALL central forces

15 E, L and Eccentricity :30 The physics is in E and L, and it transfers to quantum mechanics.

16 Predicting collisions :37 Case All objects hit the earth, regardless of initial distance. At turning point

17 Predicting collisions :37 Case Need

18 Predicting collisions :37

19 Predicting collisions :37 For v-infinity comparable to v-escape, R-impact is approx same as R-earth. For v-infinity < v-escape, R-impact is many times R- earth

20 Planetary Scattering Angle :37