According to Kepler’s third law of planetary motion
T2=R3 ( For geo stationary satellite)-------1
T’2=R’3( For Moon)----------------------------2
Dividing eq(2) by eq(1), we get
T’2 / T2=R’3/ R3
Since T’=27 T
Then we can write as
27 T2 /T2= R’3/
R3
Or
R’3=27 R3
Or
R’=3 R
or
R= 1/3 R'
so the distance between the centre of the earth and the geostationary satellite which always stays above the fixed location on the equator is 1/3 times distance between the centre of the earth and that of the moon .
No comments:
Post a Comment