Satellite Motion

Low Orbit  A container falls off the space station while in low earth orbit. It will move A) straight down toward Earth. A) straight down toward Earth. B) curving slowly down toward Earth. B) curving slowly down toward Earth. C) in the same orbit as the space station. C) in the same orbit as the space station. D) ever farther away due to lower mass. D) ever farther away due to lower mass. E) rapidly away into space. E) rapidly away into space.

Short Period  An object in space would go in a straight line without another force.  Gravity supplies a force to hold objects in circular orbits.  In low orbit the period is related to the gravitational acceleration. no gravity gravity Low Earth orbit period: T < 90 min.

Geosynchronous Orbit  In higher orbits, the gravitational force is significantly less than on the surface. Use the force of universal gravitation.Use the force of universal gravitation. F grav = G M m / r 2F grav = G M m / r 2  The height for a satellite with a 24 hr period can be found. radius: r = 4.22 x 10 7 m altitude is r km = 36,000 km

Testing Models  Geocentric (or Ptolemaic) means the Earth is at the center and motionless.  Heliocentric (or Copernican) means the Sun is at the center and motionless.  Scholars wanted to differentiate models by comparing the predictions with precise observations.  This originated the modern scientific method.

Kepler’s Work  Tycho Brahe led a team which collected data on the position of the planets ( with no telescopes).  Mathematician Johannes Kepler was hired by Brahe to analyze the data.  He took 20 years of data on position and relative distance.  No calculus, no graph paper, no log tables.  Both Ptolemy and Copernicus were wrong.  He determined 3 laws of planetary motion ( ).

Kepler’s First Law  The orbit of a planet is an ellipse with the sun at one focus. A path connecting the two foci to the ellipse always has the same length.

Orbital Speed  The centripetal force is due to gravity. GMm/r 2 = mv 2 /rGMm/r 2 = mv 2 /r v 2 = GM/rv 2 = GM/r  Larger radius orbit means slower speed.  Within an ellipse larger distance also gives slower speed.

Kepler’s Second Law  The line joining a planet and the sun sweeps equal areas in equal time. The planet moves slowly here. The planet moves quickly here. tt tt

Orbital Period  An ellipse is described by two axes. Long – semimajor (a)Long – semimajor (a) Short – semiminor (b)Short – semiminor (b)  The area is  ab (becomes  r 2 for a circle).  The speed is related to the period in a circular orbit. v 2 = GM/r (2  r/T) 2 = GM/r T 2 = 4  2 r 3 /GM  Larger radius orbit means longer period.  Within an ellipse, a larger semimajor axis also gives a longer period. b a

Kepler’s Third Law  The square of a planet’s period is proportional to the cube of the length of the orbit’s semimajor axis. T 2 /a 3 = constantT 2 /a 3 = constant The constant is the same for all objects orbiting the SunThe constant is the same for all objects orbiting the Sun semimajor axis : a direction of orbit The time for one orbit is one period: T next