Kepler's third law hypothesizes that for all the small bodies in orbit around the
same central body, the ratio of (orbital period squared) / (orbital radius cubed)
is the same number.
<u>Moon #1:</u> (1.262 days)² / (2.346 x 10^4 km)³
<u>Moon #2:</u> (orbital period)² / (9.378 x 10^3 km)³
If Kepler knew what he was talking about ... and Newton showed that he did ...
then these two fractions are equal, and may be written as a proportion.
Cross multiply the proportion:
(orbital period)² x (2.346 x 10^4)³ = (1.262 days)² x (9.378 x 10^3)³
Divide each side by (2.346 x 10^4)³:
(Orbital period)² = (1.262 days)² x (9.378 x 10^3 km)³ / (2.346 x 10^4 km)³
= 0.1017 day²
Orbital period = <u>0.319 Earth day</u> = about 7.6 hours.
Answer:
the final velocity of the two blocks is
the distance that A slides relative to B is
Explanation:
From the diagram below;
acceleration of A relative to B is : 
where
v = u + at

Making t the subject of the formula; we have:


which implies the distance that A slides relative to B.
The final velocities of the two blocks can be determined as follows:
v = u + at

Thus, the final velocity of the two blocks is
5.1 m
Explanation:
Let's set the ground as our reference point. Let's also call the dropped ball to be ball #1 and its height above the ground at any time t is given by
(1)
where 10 represents its initial height or displacement of 10 m above the ground. At the same time, the displacement of the second ball with respect to the ground
is given by
(2)
At the instant the two balls collide, they will have the same displacement, therefore

or

Solving for t, we get

We can use either Eqn(1) or Eqn(2) to hind the height where they collide. Let's use Eqn(1):

