AERSP/STS 055 Space Science & Technology 
<!#include virtual="../menu.html">

Lecture Notes

Orbits
· Gravity
· Isaac Newton (ca 1665) discovered the Law of Universal Gravitation
·
Every two
objects in the universe attract each other with a force (gravity) proportional
to the product of their masses and inversely proportional to the square of the
distance between them.
·
r =
distance between the two masses (if they are particles)
·
r =
distance between their centers (if they have significant size, i.e., one mass
is a planet)
· G = universal gravitational constant
= 6.67 ´ 10^{11} N× m^{2}/kg^{2}
· Example (gravitational force acting on mass m_{2})
R_{E} = radius of Earth = 6378 km
h = altitude (distance from Earth's surface)
r
= R_{E} + h
m_{E} = mass of Earth
· Weight (w) of an object is the gravitational force acting on it, so w = F_{GRAV }
· At altitude h, an object with mass m_{2} has weight
· At Earth's surface, the same object has weight
so by simple algebra
· If an object weighs 1000 N. at Earth's surface, then at an altitude of 10 km, it will weigh
· Even at very high altitudes, this formula still applies. So if h = 200 km (typical altitude for Space Shuttle operations) and the object is an orbiting satellite, its weight is
A satellite that weighs 1000 lb on
Earth will then weigh 910 lb at that 200 miles altitude. So why do people say that objects and people are weightless in space?
· Objects (including people) are not really weightless; they're falling.
·
But if they're falling, why don't they crash
into the Earth? (same question
· An object in orbit is both falling and moving forward, and thus travelling on a curved path. But Earth's surface is also curved. So if object moving forward fast enough, it never gets any closer to Earth because the ground curves away from the falling path. (Both the textbook and the film The Apple and the Moon explain how Newton reasoned this out in terms of firing a series of progressively faster cannonballs.)
·
Gravity plays a key role in orbits. If there were
no gravity, then
Same effect when you swing a ball on the end of a string . As long as you provide the tension in the string, the ball continues to travel in a circular path; when you release the string, the ball flies away.
Replace the tension in the string with gravity, replace yourself with the Earth and the ball with a satellite, and you have an orbiting spacecraft.
CIRCULAR ORBITS
· If satellite has just the right speed at a particular altitude, it will move in a perfectly circular orbit.
· Gravity provides the centripetal force necessary for the satellite to move on a circular orbit with radius r
·
· Therefore
· So the satellite must have the exact speed
in order to maintain a circular orbit with radius r.
· Example  if a satellite is in a circular orbit with altitude h = 1000 km, how fast is it moving?
· First, calculate the radius of the orbit. r = h + R_{E} = 1000 + 6378 km = 7378 km
· Then calculate the speed
· Since G and Earth's mass m_{E} are constants, we usually multiply them together first,
· So
ELLIPTICAL ORBITS
· If its speed is less than or greater than the necessary circular speed, then it will move on an elliptical orbit.
·
Ellipse is an elongated circle. Its eccentricity (e) is a measure of the
amount of elongation. If e = 0, the ellipse becomes a circle. If e = 0.75 (as
in the figure above), the elongation is quite evident.
· Perigee = point on elliptical orbit closes to Earth
·
r_{p}
= distance from Earth's center to perigee
· h_{p} = altitude of perigee (height above Earth's surface)
· Apogee = point on elliptical orbit farthest from Earth
·
r_{a}
= distance from Earth's center to apogee
· h_{a} = altitude of apogee (height above Earth's surface)
· Eccentricity determined by
· NASA usually reports Space Shuttle orbits in terms of h_{a} and h_{p}. So a Shuttle orbit of 230 ´ 390 km has h_{p} = 230 km, h_{a} = 390 km, which means that e = 0.012 (nearly circular!)
· Orbital period = time for satellite to make one complete trip (one revolution) around the orbit. Calculate the period using
· for circular orbits: _{} (for Earth, GM = 3.986 ´ 10^{5} km^{3}/s^{2})
· for elliptical orbits: _{}
· Additional examples for orbit problems.
· NOTE: There is a substantial amount of additional material on orbits in the ninepage handout provided in class. Those handouts are available here in two parts (pdf files): part 1 part 2
Copyright © 1998, Robert G. Melton
Updated Friday, 27Jan2006 10:42:31 EST