### Transcript for this Giancoli solution

This is Giancoli Answers with Mr. Dychko. Centripetal force on this satellite orbiting the moon is being provided by gravity and that means the mass of the satellite times*v*squared over

*r*—centripetal acceleration—equals the universal gravitational constant times mass of the satellite times mass of the moon divided by distance from the center of the moon to the satellite squared. And we also know that

*v*in circular motion is the circumference of the circle, that's the distance divided by the period or the time to do one full circle. So this is circumference over the time it takes to do a circumference. And we can substitute that in for

*v*. And also divide it both sides by mass of the satellite, in this line here, and multiply both sides by

*r*, which makes it disappear on the left side and turns this into

*r*to the power of 1. So, we have substituted for

*v*here. And that becomes 4

*π*squared

*r*squared and then the

*T*squared; let's multiply both sides by that and we get it over on the right side. And then, we'll times by

*r*over

*G*mass of the moon; this becomes

*r*cubed and 4

*π*squared over

*G*times mass of the moon and we'll square root both sides though to solve for

*T*—the period. And we can take this 4

*π*squared out from the square root sign and make it into 2

*π*and then plug in some numbers. So, we have 2

*π*times the square root of 1740 times 10 to the 3 meters— radius of the moon— plus—the distance above the moon's surface—95 times 10 to the 3 meters and cube that result of that addition and divide by 6.67 times 10 to the minus 11 and then times by 7.35 times 10 to the 22 kilograms— mass of the moon— and you get about 118 minutes, after you take this result and times by 1 minute for every 60 seconds and that's the time to do one full orbit.