From :
http://en.wikipedia.org/wiki/Kepler%27s_laws_of_planetary_motionQuote
For circular orbits, Kepler's 3rd Law is also commonly represented as
4pi² / T² = GxM / R^3
Where T is the period, G is the Gravitational constant, M is the mass of the larger body, and R is the distance between the centers of mass of the two bodies.
Problem 1 (satellite 214.2 km above surface of Earth) :
4pi² / T² = G x 5.98.10^24 / (6.38.10^6 + 214.2.10^3)^3
either you already know a value of G = 6.6738.10^(-11) m^3.kg^(-1).s^(-2),
or you can express it given the numbers for the Moon :
4pi² / (27.423x24x3600)² = G x 5.98.10^24 / (3.84.10^8)^3
-> solve for G
Answer for problem 1 :
T² = 4pi² x (6.38.10^6 + 214.2.10^3)^3 / (6.6738.10^(-11) x 5.98.10^24)
T² ~ 28364275.5
T ~ 5326
5326 s ~ 1h 28min 46 s
Problem 2 leaves me confused. Are you talking about a satellite around the Moon, or around the Earth ?
What's the use of mass of Moon and radius of Moon if it's an Earth satellite ?
Also, it seems to me that mass of satellite (47.5 kg) is useless for your problem.
At 73.3.10^3 km above surface of Earth, using same formulas :
T ~ 223700 s
T ~ 2 days 14h 8min 20 s