Chapter 11 Gravity
Chapter 11 Gravity
Chapter 11 Gravity
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Substitute for cosθ and simplify to<br />
obtain:<br />
Substitute in equation (1) and<br />
simplify:<br />
General Problems<br />
r<br />
F<br />
C<br />
GMm<br />
=<br />
2 ⎛ 2 R ⎞<br />
4 ⎜<br />
⎜d<br />
+<br />
4 ⎟<br />
⎝ ⎠<br />
GMmd<br />
=<br />
2 ⎛ 2 R ⎞<br />
4 ⎜<br />
⎜d<br />
+<br />
4 ⎟<br />
⎝ ⎠<br />
3 / 2<br />
d<br />
2<br />
iˆ<br />
d<br />
R<br />
+<br />
4<br />
r GMm<br />
F iˆ<br />
GMmd<br />
= − + 2<br />
d<br />
2 ⎛ 2 R ⎞<br />
4 ⎜<br />
⎜d<br />
+<br />
4 ⎟<br />
⎝ ⎠<br />
=<br />
⎡<br />
⎢<br />
GMm ⎢<br />
− 1 2 ⎢ −<br />
d<br />
⎢ ⎧<br />
⎢<br />
⎨d<br />
⎣ ⎩<br />
2<br />
<strong>Gravity</strong><br />
2<br />
iˆ<br />
3 / 2<br />
3<br />
d<br />
4<br />
2<br />
R ⎫<br />
+<br />
4<br />
89 •• A neutron star is a highly condensed remnant of a massive star in the<br />
last phase of its evolution. It is composed of neutrons (hence the name) because<br />
the star’s gravitational force causes electrons and protons to ″coalesce″ into the<br />
neutrons. Suppose at the end of its current phase, the Sun collapsed into a neutron<br />
star (it can’t in actuality because it does not have enough mass) of radius 12.0 km,<br />
without losing any mass in the process. (a) Calculate the ratio of the gravitational<br />
acceleration at the surface of the Sun following its collapse compared to its value<br />
at the surface of the Sun today. (b) Calculate the ratio of the escape speed from<br />
the surface of the neutron-Sun to its value today.<br />
Picture the Problem We can apply Newton’s second law and the law of gravity<br />
to an object of mass m at the surface of the Sun and the neutron-Sun to find the<br />
ratio of the gravitational accelerations at their surfaces. Similarly, we can express<br />
the ratio of the corresponding expressions for the escape speeds from the two suns<br />
to determine their ratio.<br />
(a) Express the gravitational force<br />
acting on an object of mass m at the<br />
surface of the Sun:<br />
Solving for ag yields:<br />
GM<br />
F g = mag<br />
=<br />
R<br />
Sun<br />
2<br />
Sun<br />
Sun<br />
2<br />
Sun<br />
m<br />
⎬<br />
⎭<br />
iˆ<br />
3 / 2<br />
⎤<br />
⎥<br />
⎥<br />
iˆ<br />
⎥<br />
⎥<br />
⎥<br />
⎦<br />
GM<br />
a g = (1)<br />
R<br />
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