physics 2113 lecture 03: fri 29 aug
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Physics 2113 Jonathan Dowling. Physics 2113 Lecture 03: FRI 29 AUG. Isaac Newton (1642–1727). CH13: Gravitation III. Michael Faraday (1791–1867). Version: 10/23/2014. 13.7: Planets and Satellites: Kepler ’ s 1 st Law. - PowerPoint PPT PresentationTRANSCRIPT
Physics 2113 Physics 2113 Lecture 03: FRI 29 AUGLecture 03: FRI 29 AUG
CH13: Gravitation IIICH13: Gravitation III
Physics 2113
Jonathan Dowling
Michael Faraday (1791–1867)Version: 04/20/23
Isaac Newton (1642–1727)
13.7: Planets and Satellites: Kepler’s 1st Law
1. THE LAW OF ORBITS: All planets move in elliptical orbits, with the Sun at one focus.
Johannes Kepler1571–1630Tycho Brahe
1546–1601
Laws were based on data fits!
13.7: Planets and Satellites: Kepler’s 2nd Law
2. THE LAW OF AREAS:A line that connects a planet to the Sun sweeps out equal areas in the plane of the planet’s orbit in equal time intervals; that is, the rate dA/dt at which it sweeps out area A is constant.
Angular momentum, L:
13.7: Planets and Satellites: Kepler’s 3rd Law
3. THE LAW OF PERIODS: The square of the period of any planet is proportional to the cube of the semi-major axis of its orbit.
Consider a circular orbit with radius r (the radius of a circle is equivalent to the semimajor axis of an ellipse). Applying Newton’s second law to the orbiting planet yields
Using the relation of the angular velocity, ω, and the period, T, one gets:
13.7: Planets and Satellites: Kepler’s 3rd Law
ICPP:
(a) The larger the orbit the longer the period: SAT-2.
12
(b) The smaller the orbit the greater the speed: SAT-1.
13.7: Newton Derived Kepler’s Laws from Inverse Square Law!http://galileo.phys.virginia.edu/classes/152.mf1i.spring02/KeplersLaws.htm
Kepler’s Second Law First:Equal Areas Proportional to Equal Time!
Rate of sweeping out of area,
is proportional to the angular momentum L, and equal to L/2m = Constant = C.
Angular Momentum
13.7: Newton Derived Kepler’s Laws from Inverse Square Law!http://galileo.phys.virginia.edu/classes/152.mf1i.spring02/KeplersLaws.htm
Kepler’s First Law: Ellipse with Sun at Focus
This is equivalent to the standard (r, q ) equation of an ellipse of semi-major axis a and eccentricity e, with the origin — the Sun — at one focus. Note 1/L2 is from inverse Square Law.
13.7: Newton Derived Kepler’s Laws from Inverse Square Law!http://galileo.phys.virginia.edu/classes/152.mf1i.spring02/KeplersLaws.htm
Kepler’s 3rd Law:For Ellipse
Example, Halley’s Comet
ICPP: Estimate comet’s speed at farthest distance?
13.8: Satellites: Orbits and Energy
As a satellite orbits Earth in an elliptical path, the mechanical energy E of the satellite remains constant. Assume that the satellite’s mass is so much smaller than Earth’s mass.The potential energy of the system is given by
For a satellite in a circular orbit,
Thus, one gets:
For an elliptical orbit (semimajor axis a),
(a)path 1: As E decreases (dE < 0); r decreases (dr < 0)
(b) Less: As r decreases (dr < 0); T decreases (dT < 0)
ICPP
NASA Gravity Recovery and Climate Experiment What Do the Two Satellites Measure? Changing g field!
http://www.jpl.nasa.gov/missions/gravity-recovery-and-climate-experiment-grace/
Earth is NOT a Uniform Sphere —> Gravitational Field Changes in Orbit.
• Changing field Δg give rise to changing velocity Δv.• Changing Δv gives changing satellite-to-sattellite distance. • Microwave link measures changing distance between satellites. • Measuring Δg allows computation of ΔM — Earth’s Mass Distribution.
ΔM
Rocky Mtn. High
mid-Atl. Low
Example, Mechanical Energy of a Bowling Ball
13.9: Einstein and Gravitation: Curvature of Space
13.9: Einstein and Gravitation: Gravity Waves
LIVINGSTON LASER INTERFEROMETER GRAVITATIONAL-WAVE OBSERVATORY
Disturbances in the Gravitational Field Move Outward As Waves
Two Orbiting Black Holes
HW01 DUE TONIGHT: 11:59PM FRI 29 AUG!WEB ASSIGN CLASS KEY FOR SECTION 2: lsu 8181 3713
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