18 - Gravitational Fields Flashcards
effect of us on the earth
we pull up the earth with the same amount of force we put on the earth - forces equal due to N3L but accelerations are different
earth is attracted to us but does not experience it as is mass is so big, a=F/m
newtons square law of gravitation
grav. force between two bodies, m and M, is proportional to mM and inversely proportional to the square of the distance between their centres
Fgrav ∝ mM/r^2
full mathematical expression of Newton’s law of universal gravitation
Fgrav = -GmM/r^2
Universal gravitational constant: G = 6.67 × 10–11 Nm2kg–2
why is gravitational force only significant when at least one of the masses involved is very large
G is a very small number
why is force have a negative sign
to indicate that the force is attractive
The Earth’s gravitational field appears to act from…
it’s centre of mass.
how does grav field strength change as distance increases from surface of earth
The Earth’s gravitational field gets weaker with distance from the Earth, this is shown by the greater separation of field lines.
new equation for grav. field strength
g=F/m and F=-GmM/r^2
> g=-GM/r^2
M > massive object causing grav. field
Define gravitational field strength at a point in space.
the force per unit mass an object feels whilst in orbit of a large mass (causing grav. field) at that point.
relationship between velocity and radius of a stable
geostationary orbit
Fcentriptal = Fgrav
mv^2/r = GMm/r^2
v=root(GM/r)
name for being closest anf furthest away from sun in an eliptical orbit
closest to sun - perihelion (perigee for moon)
furthest from son - aphelion (apogee for moon)
first law of planetary motion
the orbit of a planet is an ellipse with the sun at one focus
(eccentricity (how long and narrow) is low so motion can be modelled as circular)
second law of planetary motion
a line joining a planet and the sun sweeps out equal areas during equal intervals of time
(due to moving faster when closer to sun)
orbital period
t=d/v
T=2πr/v (time for one complete circuit)
keplers 3rd law equation
v^2=GM/r and T=2πr/v
T^2 = (4π^2/GM)r^3
T^2∝r^3
keplers third law
T^2∝r^3
The square of a planet’s orbital period is proportional to the cube of the radius of its orbit
what is a satellite
an object that orbits a larger object
examples of satellites
natural - moons, comets, asteroids
artificial - ISS, HST