38 1 Kinematics and Statics
Fig. 1.26
Z
CM
R
0
r
3
dr
π
2
0
sin θ cos θ dθ
2π
0
dφ
2π R
3
3
=
3R
8
1.46 The mass of any portion of the disc will be proportional to its surface area.
The area of the original disc is π R
2
, that corresponding to the hole is
1
4
π R
2
and that of the remaining portion is π R
2
−
π R
2
4
=
3
4
π R
2
.
Let the centre of the original disc be at O, Fig. 1.10. The hole touches the
circumference of the disc at A, the centre of the hole being at C. When this
hole is cut, let the centre of mass of the remaining part be at G, such that
OG = x or AG = AO + OG = R + x
If we put back the cut portion of the hole and fill it up then the centre of the
mass of this small disc (C) and that of the remaining portion (G) must be
located at the centre of the original disc at O
AO = R =
ACπ(R
2
/4) + AG
3π
4
R
2
π R
2
/4 + 3π R
2
/4
=
R
8
+
3
4
(R + x)
∴ x =
R
6
Thus the C:M of the remaining portion of the disc is located at distance R/6
from O on the left side.
1.47 Let m
1
be the mass of the earth and m
2
that of the moon. Let the centre of
mass of the earth–moon system be located at distance r
1
from the centre of
the earth and at distance r
2
from the centre of the moon, so that r = r
1
+r
2
is the distance between the centres of earth and moon, Fig. 1.27. Taking the
origin at the centre of mass