 # NCERT Solutions for Class 11 Physics Chapter 8 Gravitation

## NCERT Solutions For Class 11 Physics Chapter 8 PDF Free Download

NCERT solutions class 11 Physics Chapter 8 Gravitation is a vital resource you must refer to score good marks in class 11 examination. This solution is the result of referring to a number of textbooks by experts. These solutions are prepared as per the latest CBSE syllabus 2018-19. They present you the answers to the question in the textbooks, important questions from previous year question papers and sample papers.

NCERT solutions help your preparation with worksheets, exemplar problems, MCQ’s (multiple choice questions), HOTS (high order thinking skills), Short answer questions, NCERT tips and tricks. Solving this solution repeatedly will help you in understanding the type of question to be asked in class 1 examinations and entrance exams for the under-graduation course.

## Class 11 Physics NCERT Solutions for  Chapter 8 Gravitation

Gravitation is a very popular subject for class 11 students as most of the topics you study in future are based on this phenomenon. We should be knowing the difference between gravitation and gravity in order to understand more complex subjects. This chapter consists of questions belonging to various important concepts such as how can a body be shielded from gravitational influences of any nearby matter, whose gravitational force if greater on earth, the suns or moons?.

We find various complex but easy to understand topics in this chapter such as acceleration due to gravity, finding potential energy difference between two points which are at a certain distance from the earth’s centre. We can even know that the acceleration due to gravity increases/decreases when the depth increases or altitude decreases. We will be finding questions on an interplanetary motion such as a planet revolving around the sun with a speed double than that of earth, this question will show you the use of Kepler’s laws of motion. We will be seeing questions on Jupiter’s satellites radius of revolutions.

This chapter talks about the distance and speed of light among stars which are far away in a different galaxy and the time taken for the stars to complete one revolution. We will see here questions related to a space shuttles escape velocity and its dependency on factors like an object’s mass, location and direction of projection and the gravitational influences on it. We will be finding the angular speed, kinetic energy, total energy, potential energy, linear speed and angular momentum of an asteroid revolving around a star.

We will be going through the medical problems faced by astronauts in space and the reason behind it. We will be seeing problems on gravitational intensity within a hemisphere. We will be knowing the mass of the sun in one of the questions asked below. Do you know the distance between Uranus and earth and the time taken to reach there? You will get to know it by studying this solution.

We will see here the maximum height attained by a missile when it is fired vertically upwards before falling down on the earth’s surface. We will see the international space station’s motion around the earth and the influence of the earth’s gravitational field upon it. Do you know what will happen when two planets collide with each other, what will be their speed? We will see it here. How a star turns into a black hole and the energy required to launch a space station in mars are the type of questions you will find below.

### Important questions of Class 11 Physics Chapter 8 Gravitation

Q.1: (a). By putting an electric charge inside a hollow conductor you can shield it from the influences of electrical forces. Can a body be shielded from the gravitational influences of nearby matter in a similar fashion?

(b). An astronaut in a shuttle orbiting Mars cannot feel gravity. If he was traveling in a very large space ship would he have detected gravity?

(c). The Sun’s gravitational force on Earth is greater than the moon’s. However, the Moon affects the tidal waves much more than the Sun. Why?

Sol:

(a). No, as of now, no method has been devised to shield a body from gravity because gravity is independent of medium and it is the virtue of each and every matter. So the shield would exert the gravitational forces.

(b). Yes, if the spaceship is large enough then the astronaut will definitely detect the Mars gravity.

(c). Gravitational force is inversely proportional to the square of the distance whereas, Tidal effects are inversely proportional to the cube of the distance. So as the distance between the earth and moon is smaller than the distance between earth and sun, the moon will have a greater influence on the earth’s tidal waves.

Q2. Pick the right choice:
(a). Acceleration due to gravity does not depend upon the mass of the [body/earth]

(b). The formula, mg (r2 – r1) is [more/less] accurate than the formula $\frac{GMm}{\left ( \frac{1}{r_{2}}-\frac{1}{r_{2}} \right )}$ for the difference of potential energy between two points at a distance of r1 and r2  from the earth’s center.

(c) Acceleration due to gravity [decreases/increases] with increasing depth. (Consider earth has a uniform density).

(d) Acceleration due to gravity [decreases/increases] with decreasing altitude

Sol:

(a). body.

(b). more.

(c). decreases.

(d). increases.

Q.3: Imagine a planet that revolves around the sun at a double speed of the earth. Find the size of its orbit as compared to the orbit of the earth.

Sol:

Time taken by the earth for one complete revolution, TE = 1 Year

Radius of Earth’s orbit, RE = 1 AU

Thus, the time taken by the planet to complete one complete revolution:

TP = $\frac{1}{2}$TE  = $\frac{1}{2}$ year

Let, the orbital radius of this planet = RP

Now, according to the Kepler’s third law of planetary motion:

$\left ( \frac{R_{P}}{R_{E}} \right )^{3}=\left ( \frac{T_{P}}{T_{E}} \right )^{2}\\$ $\frac{R_{P}}{R_{E}}=\left ( \frac{T_{P}}{T_{E}} \right )^{\frac{2}{3}}\\$
$\frac{R_{P}}{R_{E}}=\left ( \frac{T_{P}}{T_{E}} \right )^{\frac{2}{3}}=\left ( \frac{\frac{1}{2}\;T_{E}}{T_{E}} \right )^{\frac{2}{3}}=\left ( \frac{1}{2} \right )^{\frac{2}{3}}=0.63$

Therefore, radius of orbit of this planet is 0.63 times smaller than the radius of orbit of the Earth.

Q.4: One of Jupiter’s satellites, Io has an orbital radius of 4.22 x 108 m and its revolution time around Jupiter is 1.769 days. Prove that the mass of the Sun is a thousand times that of Jupiter.

Sol:

Given,

Orbital period of Io, TI0 = 1.769 days  =  1.769 × 24 × 60 × 60 s

Orbital radius of Io, RI0 = 4.22 × 108 m

We know mass of Jupiter:

MJ = 4π2RI03 / GTI02    . . . . . . . . . . . . . . . (1)

Where;

MJ = Mass of Jupiter

G = Universal gravitational constant

Also,

Orbital period of the earth,

T= 365.25 days = 365.25 × 24 × 60 × 60 s

Orbital radius of the Earth, R= 1 AU = 1.496 × 1011 m

We know that the mass of sun is:

MS = $\frac{4\;\pi ^{2}\;R_{E}^{3}}{G\;T_{E}^{2}}$. . . . . . . . . . . . .  (2)

Therefore,  $\\\frac{M_{S}}{M_{J}}$ = $\frac{4\;\pi ^{2}\;R_{E}^{3}}{G\;T_{E}^{2}}\;\times \;\frac{G\;T_{10}^{2}}{4\;\pi ^{2}\;R_{10}^{3}}\\$ = $\\\frac{R_{E}^{3}}{T_{E}^{2}}\;\times \;\frac{T_{10}^{2}}{R_{10}^{3}}$

Now, on substituting the values, we will get:

= $\left [ \frac{1.769\times 24\times 60\times 60}{365.25\times 24\times 60\times 60} \right ]^{2}\times \left [ \frac{1.496\times 10^{11}}{4.22\times 10^{8}} \right ]^{3}$ = 1045.04

Therefore, $\frac{M_{S}}{M_{J}}$ ~ 1000

M~ 1000 × MJ

[Which proves that, the Sun’s mass is 1000 times that of Jupiter’s)

Q.5: Consider that the Sombrero galaxy has 3 x 1011 stars, each of one solar mass. If the diameter of the galaxy is 105 light years, calculate the time of a star, at a distance of 5000 light years from the galactic center, takes to complete one revolution.

Sol:

Mass of Sombrero Galaxy, M = 3 × 1011 solar mass
Solar mass = Mass of Sun = 2.0 × 1036 kg
Mass of the galaxy, M = 3 × 1011 × 2 × 1036 = 6 × 1041 kg
Diameter of Sombrero Galaxy, d = 5 x 104 ly
Radius of Sombrero Galaxy, r = 2.5 × 104 ly

We know that:

1 light year = 9.46 × 1015 m
Therefore, r = 2.5 × 104 × 9.46 × 1015= 2.365 x 1020 m

As this star revolves around the massive black hole in center of the Sombrero galaxy, its time period can be found with the relation:
T = $\left [ \frac{4\;\pi ^{2}\;r^{3}}{GM} \right ]^{\frac{1}{2}}\\$
$\\\left [ \frac{4\times 3.14^{2}\times (2.365\times 10^{20})^{3}}{(6.67\times 10^{-11})\times (6\times 10^{41})} \right ]^{\frac{1}{2}}\\$ =   4.246 x 1015  s
Now we know, 1 year = 365 × 24 × 60 × 60 s

1s = $\frac{1}{365\times 24\times 60\times 60}\\$ years
Therefore, 4.246 × 1015s = $\frac{4.246\times 10^{15}}{365\times 24\times 60\times 60}$ =  1.34 × 108 years.

Q.6: Pick the right alternative:

(a). The energy spent on sending a rocket vertically upwards out of the earth’s gravitational influence is more /  less than the energy spent on sending an orbiting satellite to the same height out of the earth’s influence.

(b). If potential energy is zero at infinity, the total energy of an orbiting comet is negative of its potential / kinetic energy.

Sol:

(a).  more

(b).  kinetic.

Q7. Choose the factors upon, which the escape velocity of an object from earth depends upon:

(a) body’s mass.

(b) location of projection.

(c) direction of projection.

Sol: (b)

Explanation:

Escape velocity is independent of the direction of projection and the mass of the body. It depends upon the gravitational potential at the place from where the body is projected. Gravitational potential depends slightly on the altitude and the latitude of the place, thus escape velocity depends slightly upon the location from where it is projected.

Q.8: An asteroid orbits a star in an elliptical orbit.  Does the asteroid have a constant (a) angular speed, (b) kinetic energy, (c) total energy (d), linear speed, (e) potential energy and (f) angular momentum throughout its revolution?

Sol:

An asteroid orbiting a star will have constant angular momentum and the constant value of total energy throughout its orbit.

Q9. Which of the following problems is likely to affect an astronaut in space? (a) Swollen feet, (b) bone loss, (c) orientational problem, (d) headache.

Sol:

(a). In zero gravity the blood flow to the feet isn’t increased so the astronaut does not get swollen feet.

(b). Due to zero gravity, the weight the bones have to bear is greatly reduced, this causes bone loss in astronauts spending greater amounts of time in space.

(c). Space has different orientations, so orientational problems can affect an astronaut.

(d). Due to increased blood supply to their faces, astronauts can be affected by headaches.

Q.10: Pick up the right answers from the given ones:

The direction of gravitational intensity inside a hemispherical sphere of a uniform mass is indicated by the arrow:

(i) c

(ii) x

(iii) z

(iv) o Sol: (i) c

Reason:

Inside a hollow sphere, gravitational forces on any particle at any point is symmetrically placed. However, in this case, the upper half of the sphere is removed. Since gravitational intensity is gravitational force per unit mass it will act in direction point downwards along ‘c’.

Q.11: For the above problem the gravitational intensity at P will be directed towards:

(i) h

(ii) f

(iii) m

(iv) v

Sol: (iii) m

Reason: Making use of the logic/explanation from the above answer we can conclude that the gravitational intensity at P is directed downwards along m.

Q12. A rocket is launched off from the earth’s surface for a massive comet nearing the earth. At what distance from the earth’s center will the shuttle of the rocket be free from the earth’s gravitational force. Mass of the comet = 7.4 x 1022, mass of Earth = 6 x 1024 and distance between earth and the comet= 3.84 x 1010 m.

Sol:

Given:

Mass of the comet, MC = 7.4 × 1024 kg

Mass of the Earth, ME = 6 × 10 24 kg
Orbital radius, r = 3.84 × 1010 m
Mass of the shuttle = m kg

Let ‘x’ be the distance from the center of the Earth where the gravitational force acting on the Shuttle ‘S’ becomes zero.

According to Newton’s law of gravitation, we have:

$\\\Rightarrow \frac{G\;m\;M_{A}}{(r-x)^{2}}=\frac{G\;m\;M_{E}}{x^{2}}\\$ $\\\Rightarrow$   $\frac{M_{A}}{M_{E}}=\left ( \frac{r-x}{x} \right )^{2}$ $\Rightarrow$   $\frac{r}{x}-1=\left ( \frac{7.4\times 10^{24}}{6\times 10^{24}} \right )^{\frac{1}{2}}\\$ $\Rightarrow$   $\frac{r}{x}-1=1.1106$ $\\\Rightarrow$   $x=\frac{r}{2.1106}=\frac{3.84\times 10^{10}}{2.1106}=1.819\times 10^{10}\;m$

Q.13: If the earth’s orbit around the sun is 1.5x 108 km long, estimate the mass of the Sun.

Sol:

Given:
Earth’s orbit, r = 1.5 × 1011 m
Time taken by the Earth for one complete revolution,
T = 1 year = 365.25 days
i.e. T = (365.25 × 24 × 60 × 60) seconds

Since, Universal gravitational constant, G = 6.67 × 10–11 Nm2 kg–2
Therefore, mass of the Sun, M = $\frac{4\;\pi ^{2}r^{3}}{G\;T^{2}}\\$
$\\\Rightarrow M =\frac{4\times (3.14)^{2}\times (1.5\times 10^{11})^{3}}{(6.67\times 10^{-11})\times (365.25\times 24\times 60\times 60)^{2}}\\$ $\\\Rightarrow M =\frac{4\times (3.14)^{2}\times (1.5\times 10^{11})^{3}}{(6.67\times 10^{-11})\times (365.25\times 24\times 60\times 60)^{2}}\\$ $\\\Rightarrow$   $M=\frac{1.331\times 10^{35}}{66.425\times 10^{3}}=2.004\times 10^{30}\;kg\\$
Therefore, the estimated mass of the Sun is 2.004 × 1030 Kg

Q14. Uranus is 84 times the earth year. If the Earth is 15 x 107 km away from the Sun, what is the distance between the Sun and Uranus?

Sol:

Given:

Distance between Earth and the Sun, re = 15 × 107 km = 1.5 × 1011 m
Time period of the Earth = T­e
Time period of Uranus, Tu = 84 Te

Let, the distance between the Sun and the Uranus be r

Now, according to the Kepler’s third law of planetary motion:
T =$\left ( \frac{4\pi ^{2}r^{3}}{GM} \right )^{\frac{1}{2}}$

For Uranus and Sun, we can write:
$\Rightarrow \frac{r_{u}^{3}}{r_{e}^{3}}=\frac{T_{u}^{2}}{T_{e}^{2}}\\\\\\ \Rightarrow r_{u}=r_{e}\left [ \frac{T_{u}}{T_{e}} \right ]^{\frac{2}{3}}\\\\\\ \Rightarrow r_{u}=1.5\times 10^{11}\left [ \frac{84\;T_{e}}{T_{e}} \right ]^{\frac{2}{3}}=\boldsymbol{1.5\times 10^{11}\times (84)^{\frac{2}{3}}}$ $\Rightarrow r_{u}=28.77\times 10^{12}\\$m
Therefore, Uranus is  28.77 × 1012 m away from the Sun.

Q.15: A man weighing 60 N on the earth’s surface is taken to the height that is equal to half of the earth’s radius. What is the amount of gravitational force which the earth will exert on this man now?

Sol:

Given:

Weight of the man, W = 60 N

We know that acceleration due to gravity at height ‘h’ from the Earth’s surface is:

g‘ = $\frac{g}{\left [ 1+\left ( \frac{h}{R_{e}} \right ) \right ]^{2}}$
Where, g = Acceleration due to gravity on the Earth’s surface
And, Re = Radius of the Earth
For h = $\frac{R_{e}}{2}\\$
g’ = $\\\frac{g}{\left [ 1+\left ( \frac{R_{e}}{2R_{e}} \right ) \right ]^{2}}\\$
$\\\Rightarrow$ g‘ = $\frac{g}{\left [ 1+\left (\frac{1}{2} \right ) \right ]^{2}}=\frac{4}{9}\;g$

Also , the weight of a body of mass ‘m’ kg at a height of ‘h’ meters can be represented as :
W’ = mg
= m × $\frac{4}{9}$g  =  $\frac{4}{9}\\$mg
= $\\\frac{4}{9}\\$W
= $\\\frac{4}{9}$ × 60  = 26.66 N.

Q.16: Considering the earth to be a sphere of uniform mass density. Find the weight of a body at one-third of the way down to the center of the earth if it weighed 200 N on the surface?

Sol:

Given,

The weight of a body having mass ‘m’ at the surface of earth, W = mg = 200 N
Body of mass m’ is located at depthd = $\frac{1}{3}$ Re
Where, Re = Radius of the Earth
Now, acceleration due to gravity g’ at depth (d) is given by the relation:
g’ = $1-\left ( \frac{d}{R_{e}} \right )g\\$
$\Rightarrow g’ = 1-\left ( \frac{R_{e}}{3R_{e}} \right )g=\frac{2}{3}\;g$

Now, weight of the body at depth d,
W’ = mg’
W’ = m × $\frac{2}{3}$g  = $\frac{2}{3}$ mg

W’ = $\frac{2}{3}$ W

$\Rightarrow$ W = $\frac{2}{3}$ × 200  =  133.33 N

Therefore, the weight of a body at one-third of the way down to the center of the earth = 133.33 N

Q.17: A missile is fired vertically upwards from the surface at 4 km m/s. What is the greatest height the missile can attain before falling back to the earth? Also find the final distance of the missile from the center of the earth. [Mass of earth = 6 x 1024 kg, mean radius of earth = 6.4 x 106m and take G =6.67 x 10-11 N m2 kg-2]

Sol:

Given:
Velocity of the missile,  v = 4 km/s = 4 × 103 m/s
Mass of the Earth,     ME = 6 × 1024 kg
Radius of the Earth,    RE = 6.4 × 106 m

Let, the height reached by the missile be ‘h’ and the mass of the missile  be ‘m’.
Now, at the surface of the Earth:
Total energy of the rocket at the surface of the Earth = Kinetic energy + Potential energy
TE1 = $\\\frac{1}{2}mv^{2}+\frac{-GM_{E}\;m}{R_{E}}$

Now, at highest point h’:

Kinetic Energy = 0   [Since, v = 0]
And, Potential energy = $\\\frac{-GM_{E}\;m}{R_{E}+h}$

Therefore, total energy of the missile at highest point ‘h’:

TE2 = 0 + $\frac{-GM_{E}\;m}{R_{E}+h}$ $\\\Rightarrow$ TE2 = $\frac{-GM_{E}\;m}{R_{E}+h}$

According to the law of conservation of energy, we have :
Total energy of the rocket at the Earth’s surface TE1 = Total energy at height h’ TE2:
$\\\Rightarrow \frac{1}{2}mv^{2}+\frac{-GM_{E}\;m}{R_{E}}=\frac{-GM_{E}\;m}{R_{E}+h}\\\\\\ \Rightarrow \frac{1}{2}v^{2}+\frac{-GM_{E}}{R_{E}}=\frac{-GM_{E}}{R_{E}+h}\\\\\\ \Rightarrow v^{2} = 2GM_{E}\times \left [ \frac{1}{R_{E}}-\frac{1}{(R_{E}+h)} \right ]=2GM_{E}\left [ \frac{h}{(R_{E}+h)R_{E}} \right ]\\$
$\\\Rightarrow v^{2}=\frac{g\;R_{E}\;h}{R_{E}+h}\\$
Where, $\\g=\frac{GM}{R_{E}^{2}}\\$ = 9.8 ms-2
Therefore, v2 (RE + h) = 2gREh
$\\\Rightarrow$ v2RE = h (2gRE – v2)

$\\\Rightarrow$ $h=\frac{R_{E}\;v^{2}}{2gR_{E}-v^{2}}=\frac{(6.4\times 10^{6})\times (4\times 10^{3})^{2}}{2\times 9.8\times 6.4\times 10^{6}-(4\times 10^{3})^{2}}\\$
$\\\Rightarrow$ h = 9.356 × 105  m
Therefore, the missile reaches at height of 9.36 × 105 m from the surface.

Now, the distance from the center of the earth = h + RE = 9.36 × 105 + 6.4 x 106 = 7.33 x106 m

Therefore, the greatest height the missile can attain before falling back to the earth is   9.356 × 105 m and the final distance of the missile from the center of the earth is 7.33 x106 m

Q.18: On the surface of the earth escape velocity is 11.2 km/s. If a body (rocket) is projected upward with twice this speed, find the speed of this rocket at a distance far away from the surface of the earth. Neglect the presence of other heavenly bodies like the sun and other planets.

Sol:

Given,

Escape velocity of the Earth’s surface, vesc = 11.2 km/s
Projection
velocity of the rocket, vP = 2vesp

Let, mass of the body = m kg

And, the velocity of the rocket at a distance very far away from the surface of earth = vF

Total energy of the rocket on the surface = $\frac{1}{2}$ mvp2 – $\frac{1}{2}$mv2esp

Total energy of the rocket at a distance very far away from the Earth = $\frac{1}{2}$ mvF2

Now, according to the law of conservation of energy, we have:
$\frac{1}{2}$mvP2 – $\frac{1}{2}$mvESC2  =  $\frac{1}{2}$mvF2

mvESC2  =  $\frac{1}{2}$ mvF2
vF = $\\\sqrt{(v_{p})^{2}-(v_{esc})^{2}}\\$    [Since, vP = 2vesp ]
vF = $\\\sqrt{(2v_{esp})^{2}-(v_{esc})^{2}}\\$
vF =$\\\sqrt{3}$ vesc

$\Rightarrow$ vF =$\sqrt{3}$ × 11.2 = 19.39 km/s

Therefore, the speed of rocket at a distance far away from the surface of earth is 19.39 km/s.

Q.19: International Space Station (ISS) orbits the earth at a height of 380 km and has a mass of 420000 kg. Find the amount of energy required to take it out from the gravitational influence of earth. [Mass of earth = 6.0 x 1024 kg, radius of earth = 6.4 x10 6m and take G = 6.67x 10 -11 N m2 kg–2]

Sol:

Given:

Mass of the satellite, m = 420000 kg

Radius of the Earth, RE = 6.4 × 106 m

Mass of the Earth, ME = 6.0 × 1024 kg
Universal gravitational constant, G = 6.67 × 10–11 Nm2 kg –2

Height of the satelliteh = 380 km = 0.38 ×106 m
We know that the Total energy of the satellite at height ‘h’ $=\frac{1}{2}mv^{2}+\left [ \frac{-GM_{E}\;m}{R_{E}+h} \right ]$

Also, orbital velocity of the satellite, v $=\left [ \frac{GM_{E}}{R_{E}+h} \right ]^{\frac{1}{2}}$

Total energy at height, h$=\frac{1}{2}\left [ \frac{GM_{E}}{R_{E}+h} \right ]-\left [ \frac{GM_{E}\;m}{R_{E}+h} \right ]$

Therefore, TE$=\frac{-1}{2}\left [ \frac{GM_{E}\;m}{R_{E}+h} \right ]$
This negative sign means that the ISS is bounded to Earth. This is the bound energy of the satellite.
Now, Total Energy required to send the satellite out of its orbit = – (Bound energy)
TE$\\=\frac{1}{2}\left [ \frac{GM_{E}\;m}{R_{E}+h} \right ]\\$
TE$\\=\frac{1}{2}\left [ \frac{(6.67\times 10^{-11})\times (6\times 10^{24})\times (4.2\times 10^{5})}{(6.4\times 10^{6})+(0.380\times 10^{6})} \right ]=\frac{1}{2}\times \left [ \frac{1.681\times 10^{20}}{6.78\times 10^{6}} \right ]\\$
$\\\Rightarrow$  TE = 1.2396 x 1013 J

Therefore, the amount of energy required to take ISS out from the gravitational influence of earth is 1.2396 x 1013 J

Q.20: Two planets each of mass 2 x 1031 kg are on a path of collision with each other. If they have negligible speeds at a distance of 1010 km. Find the speed at which they collide if each planet has a radius of 103 km. [Take G = 6.67 x 10-11]

Sol:

Given:
Radius of each planet, R = 103 km = 106 m

Distance between the planet, r = 1010 km = 1013 m

Mass of each planet, M = 2 × 1031 kg

For negligible speeds, v = 0

So the total energy of two planets separated by a distance ‘r’:

TE =$\frac{-GMM}{r}+\frac{1}{2}mv^{2}$

Since, v = 0;
Therefore, TE =$\frac{-GMM}{r}$  . . . . . . . . . . . . . . . . (1)
Now, when the planets are just about to collide:

Let, the velocity of the planets = v

The centers of the two planets are at a distance of = 2R
Total kinetic energy of the two planets = $\frac{1}{2}$ Mv2 + $\frac{1}{2}$ Mv2 = Mv2
Total potential energy of the two planets = $\frac{-GMM}{2R}$
Therefore, Total energy of the two stars = Mv2 -$\\\frac{GMM}{2R}$ . . . . . . . . . . . . (2)

Now, according to the law of conservation of energy :
Mv2 – $\\\frac{GMM}{2R}$ = $\frac{-GMM}{r}\\$
v2 = $\\\frac{-GM}{r}$ + $\frac{GM}{2R}\\$
v2 = GM × $\\\left [ \frac{-1}{r}+\frac{1}{2R} \right ]$ $\Rightarrow$ v2 = 6.67 × 10-11 × 2 × 1031 × $\left [ \frac{-1}{(10^{13})}+\frac{1}{(2\times 10^{6})} \right ]$
$\Rightarrow$v2 = 6.67 × 1014
Therefore, v = (6.67 × 1014)1/2  =  2.583 × 107m/s.

Hence, the speed at which they will collide = 2.583 × 107m/s.

Q.21: Two spheres each having a radius of 0.15 m and mass 1000 kg are placed 1.0 m apart from each other on a horizontal plane. Calculate the gravitational potential and force at the midpoint of the line connecting the centers of the two spheres. If an object is kept at that point will it be in equilibrium? If yes, is this equilibrium position is unstable or stable?

Sol:

Given:

Radius of spheres, R = 0.15 m

Distance between two spheres, r = 1.0 m

Mass of each sphere, M = 1000 kg Two spheres

From the above figure, ‘A’ is the mid-point and since each sphere will exert the gravitational force in the opposite direction. Therefore, the gravitational force at this point will be zero.

Gravitational potential at the midpoint (A) is;

U= $\left [ \frac{-GM}{\frac{r}{2}}+\frac{-GM}{\frac{r}{2}} \right ]$

U= $\left [ \frac{-4GM}{r} \right ]$

U= $\left [ \frac{-4\times (6.67\times 10^{-11})\times (1000)}{1.0} \right ]$

$\Rightarrow$ U= -2.668 x 10-7 J /kg

Therefore, the gravitational potential and force at the mid-point of the line connecting the centers of the two spheres is = -2.668 x 10-7 J /kg

The net force on an object, placed at the mid-point is zero. However, if the object is displaced even a little towards any of the two bodies it will not return to its equilibrium position. Thus, the body is in unstable equilibrium.

Q.22: Find the gravitational potential due to Earth’s gravity on a geo-stationary satellite orbiting earth at 36000 km above the surface. [Mass of earth = 6 x 1024 kg, radius = 6400 km and Assume that the potential energy is zero at infinity]

Sol:

Given:

Radius of the Earth, R = 6400 km = 0.64 × 107 m

Mass of Earth, M = 6 x 1024 kg

Height of the geo-stationary satellite from earth’s surface, h = 36000 km = 3.6 x 107 m

Therefore, gravitational potential at height ‘h’ on the geo-stationary satellite due to the earth’s gravity:

GP = $\frac{-GM}{R+h}\\$
$\\\Rightarrow$ GP = $\frac{-(6.67\times 10^{-11})\times (6\times 10^{24})}{(0.64\times 10^{7})+(3.6\times 10^{7})}\\$
$\\\Rightarrow$ GP = $\frac{-40.02\times 10^{13}}{4.24\times 10^{7}}$= -9.439 × 106 J/Kg

Therefore, the gravitational potential due to Earth’s gravity on a geo-stationary satellite orbiting earth is -9.439 × 106 J/Kg

Q.23: A star 10 times the size of the sun collapses on itself and gets reduced to a black hole of radius 10km, rotating at a speed of 10 revolutions per second. Prove that an object placed on its equator will remain stuck on the equator due to its gravity. [Mass of the sun = 2 x 103 kg]

Sol.

Any matter/ object will remain stuck to the surface if the outward centrifugal force is lesser than the inward gravitational pull.

Gravitational force, fG = $\frac{GM\;m}{R^{2}}$ [Neglecting negative sign]

Here,
M = Mass of the star = 10 × 2 × 1030 = 2 × 1031 kg
= Mass of the object
R = Radius of the star = 10 km = 1 ×104 m
Therefore, fG = $\\\frac{(6.67\times 10^{-11})\times (2\times 10^{31})\;m}{(1\times 10^{4})^{2}}=1.334\times 10^{13}m\;N$

Now, Centrifugal force, fC = m r ω2
Here, ω = Angular speed = 2πν
ν = Angular frequency = 10 rev s–1
fc = m R (2πν)2

fc = m × (104) × 4 × (3.14)2 × (10)2 = (3.9 ×107m) N

As fG > fC, the object will remain stuck to the surface of black hole.

Q.24: Find the amount of energy required to launch a spaceship stationed on Mars to out of the solar system.

(Mass of the Sun = 2 × 1030 kg; mass of the space ship = 2000 kg, mass of mars = 6.4 × 1023 kg; radius of mars = 3395 km; radius of the orbit of mars = 2.28 × 108 km; G= 6.67 × 10–11 m2kg–2)

Sol:

Given,

Mass of the Sun, M = 2 × 1030 kg

Mass of the spaceshipm= 2000 kg

Radius of Mars, r = 3395 km = 3.395 × 106 m

Mass of Mars, Mm = 6.4 × 10 23 kg

Orbital radius of Mars, R = 2.28 × 10km = 2.28 × 1011 m

Universal gravitational constant, G = 6.67 × 10–11 m2 kg– 2

Now,

Potential energy of the spaceship due to the gravity of Sun = $\frac{-GMm_{s}}{R}$
Potential energy of the spaceship due to gravity of Mars = $\frac{-GM_{M}\;m_{s}}{r}$

As the spaceship is stationed on Mars, its velocity is ‘zero’ and thus, its kinetic energy is also ‘zero’.
Thus, Total energy of the spaceship $\\=\frac{-GM_{M}\;m_{s}}{r}-\frac{GMm_{s}}{R}$
TE $\\=-Gm_{s}\left [ \frac{M}{R}+\frac{M_{M}}{r} \right ]$

The negative sign means that the system is in bound state.

Therefore, energy required to launch the spaceship out of the solar system:
TE = – (bound energy)
TE$\\=Gm_{s}\left [ \frac{M}{R}+\frac{M_{M}}{r} \right ]$

Now, on substituting the values of G, M, R, ms, MM and r we will get:

TE $=(6.67\times 10^{-11})\times (2\times 10^{3})\times \left [ \frac{2\times 10^{30}}{2.28\times 10^{11}}+\frac{6.4\times 10^{23}}{3.395\times 10^{6}} \right ]$ $\\\Rightarrow$   $13.34\times 10^{-8}\times \left [ 87.7\times 10^{17} \;+\;1.885\times 10^{17}\right ]\boldsymbol{=1.195\times 10^{12}J}$

Therefore, the total amount of energy required to launch a spaceship stationed on Mars to out of the solar system = 1.195 × 1012 J

Q.25: A missile is shot vertically upward from the surface of Venus; if 25% of its initial energy is lost in overcoming Venus’s atmospheric resistance, find the maximum height the missile will achieve before returning back to the surface. Take Initial velocity of the missile = 3 km s– 1, Mass of Venus = 4.8 × 1024 kg and the radius of Venus= 6052 km. [G = 6.67× 10-11 N m2 kg–2 ]

Sol.

Given:

Mass of Venus, M = 4.8 × 1024 kg

Initial velocity of the missile, v = 3 km/s = 3 × 103 m/s

Radius of Venus, = 6052 km = 6.05 x 106 m

Universal gravitational constant, G = 6.67× 10–11 N m2 kg–2

Let the mass of the missilem kg

Since, the Initial kinetic energy of the missile = $\frac{1}{2}$ mv2
and the Initial potential energy of the missile = $\frac{-GMm}{R}$
Thus, total initial energy $=\frac{1}{2}mv^{2}+\left ( \frac{-GMm}{R} \right )$

It is given that 25 % of initial kinetic energy is lost in overcoming the atmospheric resistance of Venus; this means that only 75% of the total kinetic energy is available for propelling it upwards.

Hence, the total available initial energy $=\left [ \frac{75}{100}\times \frac{1}{2}mv^{2} \right ]-\frac{GMm}{R}=0.375mv^{2}-\frac{GMm}{R}$

Let ‘h’ be the maximum height attained by the missile.
Now, at height ‘h’ the final velocity = 0 and hence, the kinetic energy = 0

Therefore, the total energy of the missile at height ‘h’ = $\frac{-GMm}{R+h}$
Now, according to the law of conservation of energy:
$\\\Rightarrow\;\;\; 0.375mv^{2}-\frac{GM}{R}=\frac{-GMm}{R+h}$ $\\\Rightarrow$   $\;\;\; 0.375\;v^{2}=GMm\left ( \frac{1}{R}-\frac{1}{R+h} \right )$ $\\\Rightarrow 0.375 v^{2}=GM\times \left [ \frac{h}{R\;(R+h)} \right ]\\$ $\\\Rightarrow$   $\frac{R+h}{h}=\frac{GM}{0.375\;v^{2}R}\\$ $\\\Rightarrow$   $\frac{R}{h}=\frac{GM}{0.375\;v^{2}R}-1\\$ $\\\Rightarrow$   $\frac{R}{h}=\frac{GM-0.375\;v^{2}R}{0.375\;v^{2}R}\\$ $\\\Rightarrow$   $\frac{1}{h}=\frac{GM-0.375\;v^{2}R}{0.375\;v^{2}R^{2}}\\$ $\\\Rightarrow$   $h=\frac{0.375\;v^{2}R^{2}}{GM-0.375\;v^{2}R}$

Now, on substituting the values of G, M, v and R we will get:

$\Rightarrow h=\frac{0.375\;\times \;(3\;\times \;10^{3})^{2}\;\times \;(6.05\;\times \;10^{6})^{2}}{\left [ (6.67\;\times \;10^{-11})\;\times \;(4.8\;\times \;10^{24}) \right ]-[0.375\;\times \;(3\;\times \;10^{3})^{2}\;\times \;6.05\;\times \;10^{6}]}\\$ $\\\Rightarrow h=\frac{0.375\;\times \;(3\;\times \;10^{3})^{2}\;\times \;(6.05\;\times \;10^{6})^{2}}{\left [ (6.67\;\times \;10^{-11})\;\times \;(4.8\;\times \;10^{24}) \right ]-[0.375\;\times \;(3\;\times \;10^{3})^{2}\;\times \;6.05\;\times \;10^{6}]}\\$ $\\\Rightarrow$   $\frac{1.235\;\times \;10^{20}}{3.2016\;\times \;10^{14}-2.042\;\times \;10^{13}}\boldsymbol{=412023.75\;m=4.12\;km}$

Therefore, the maximum height that is achieved by the missile before returning back to the surface = 4.12 km.

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