
1.Basic Maths (1) : Vectors
7
Lecture1.1

Lecture1.2

Lecture1.3

Lecture1.4

Lecture1.5

Lecture1.6

Lecture1.7


2.Basic Maths (2) : Calculus
4
Lecture2.1

Lecture2.2

Lecture2.3

Lecture2.4


3.Unit and Measurement
13
Lecture3.1

Lecture3.2

Lecture3.3

Lecture3.4

Lecture3.5

Lecture3.6

Lecture3.7

Lecture3.8

Lecture3.9

Lecture3.10

Lecture3.11

Lecture3.12

Lecture3.13


4.Motion (1) : Straight Line Motion
10
Lecture4.1

Lecture4.2

Lecture4.3

Lecture4.4

Lecture4.5

Lecture4.6

Lecture4.7

Lecture4.8

Lecture4.9

Lecture4.10


5.Motion (2) : Graphs
3
Lecture5.1

Lecture5.2

Lecture5.3


6.Motion (3) : Two Dimensional Motion
6
Lecture6.1

Lecture6.2

Lecture6.3

Lecture6.4

Lecture6.5

Lecture6.6


7.Motion (4) : Relative Motion
7
Lecture7.1

Lecture7.2

Lecture7.3

Lecture7.4

Lecture7.5

Lecture7.6

Lecture7.7


8.Newton's Laws of Motion
8
Lecture8.1

Lecture8.2

Lecture8.3

Lecture8.4

Lecture8.5

Lecture8.6

Lecture8.7

Lecture8.8


9.Constrain Motion
3
Lecture9.1

Lecture9.2

Lecture9.3


10.Friction
6
Lecture10.1

Lecture10.2

Lecture10.3

Lecture10.4

Lecture10.5

Lecture10.6


11.Circular Motion
6
Lecture11.1

Lecture11.2

Lecture11.3

Lecture11.4

Lecture11.5

Lecture11.6


12.Work Energy Power
12
Lecture12.1

Lecture12.2

Lecture12.3

Lecture12.4

Lecture12.5

Lecture12.6

Lecture12.7

Lecture12.8

Lecture12.9

Lecture12.10

Lecture12.11

Lecture12.12


13.Momentum
9
Lecture13.1

Lecture13.2

Lecture13.3

Lecture13.4

Lecture13.5

Lecture13.6

Lecture13.7

Lecture13.8

Lecture13.9


14.Center of Mass
5
Lecture14.1

Lecture14.2

Lecture14.3

Lecture14.4

Lecture14.5


15.Rotational Motion
14
Lecture15.1

Lecture15.2

Lecture15.3

Lecture15.4

Lecture15.5

Lecture15.6

Lecture15.7

Lecture15.8

Lecture15.9

Lecture15.10

Lecture15.11

Lecture15.12

Lecture15.13

Lecture15.14


16.Rolling Motion
11
Lecture16.1

Lecture16.2

Lecture16.3

Lecture16.4

Lecture16.5

Lecture16.6

Lecture16.7

Lecture16.8

Lecture16.9

Lecture16.10

Lecture16.11


17.Gravitation
8
Lecture17.1

Lecture17.2

Lecture17.3

Lecture17.4

Lecture17.5

Lecture17.6

Lecture17.7

Lecture17.8


18.Simple Harmonic Motion
13
Lecture18.1

Lecture18.2

Lecture18.3

Lecture18.4

Lecture18.5

Lecture18.6

Lecture18.7

Lecture18.8

Lecture18.9

Lecture18.10

Lecture18.11

Lecture18.12

Lecture18.13


19.Waves (Part1)
11
Lecture19.1

Lecture19.2

Lecture19.3

Lecture19.4

Lecture19.5

Lecture19.6

Lecture19.7

Lecture19.8

Lecture19.9

Lecture19.10

Lecture19.11


20.Waves (Part2)
10
Lecture20.1

Lecture20.2

Lecture20.3

Lecture20.4

Lecture20.5

Lecture20.6

Lecture20.7

Lecture20.8

Lecture20.9

Lecture20.10


21.Mechanical Properties of Solids
6
Lecture21.1

Lecture21.2

Lecture21.3

Lecture21.4

Lecture21.5

Lecture21.6


22.Thermal Expansion
5
Lecture22.1

Lecture22.2

Lecture22.3

Lecture22.4

Lecture22.5


23.Heat and Calorimetry
2 
24.Heat Transfer
6
Lecture24.1

Lecture24.2

Lecture24.3

Lecture24.4

Lecture24.5

Lecture24.6


25.Kinetic Theory of Gases
6
Lecture25.1

Lecture25.2

Lecture25.3

Lecture25.4

Lecture25.5

Lecture25.6


26.Thermodynamics
9
Lecture26.1

Lecture26.2

Lecture26.3

Lecture26.4

Lecture26.5

Lecture26.6

Lecture26.7

Lecture26.8

Lecture26.9


27.Fluids
14
Lecture27.1

Lecture27.2

Lecture27.3

Lecture27.4

Lecture27.5

Lecture27.6

Lecture27.7

Lecture27.8

Lecture27.9

Lecture27.10

Lecture27.11

Lecture27.12

Lecture27.13

Lecture27.14


28.Surface Tension and Viscosity
6
Lecture28.1

Lecture28.2

Lecture28.3

Lecture28.4

Lecture28.5

Lecture28.6

NCERT Solutions – Gravitation
(a) You can shield a charge from electrical forces by putting it inside a hollow conductor. Can you shield a body from the gravitational influence of nearby matter by putting it inside a hollow sphere or by some other means?
(b) An astronaut inside a small space ship orbiting around the earth cannot detect gravity. If the space station orbiting around the earth has a large size, can he hope to detect gravity?
(c) If you compare the gravitational force on the earth due to the sun to that due to the moon, you would find that the Sun’s pull is greater than the moon’s pull. (You can check this yourself using the data available in the succeeding exercises). However, the tidal effect of the moon’s pull is greater than the tidal effect of sun. Why?
Answer
(a) We cannot shiwld a body from the gravitational influence of nearby matter, because the gravitational force on a body due to nearby matter is independent of the presence of other matter, whereas it is not so in case of electric forces. It means the gravitational screens are not possible.
(b) Yes, if the size of the space station is large enough, then the astronaut will detect the change in Earth’s gravity (g).
(c) Tidal effect depends inversely upon the cube of the distance while, gravitational force depends inversely on the square of the distance. Since the distance between the Moon and the Earth is smaller than the distance between the Sun and the Earth, the tidal effect of the Moon’s pull is greater than the tidal effect of the Sun’s pull.
8.2. Choose the correct alternative:
(a) Acceleration due to gravity increases/decreases with increasing altitude.
(b) Acceleration due to gravity increases/decreases with increasing depth. (assume the earth to be a sphere of uniform density).
(c) Acceleration due to gravity is independent of mass of the earth/mass of the body.
(d) The formula –G Mm(1/r_{2}– 1/r_{1}) is more/less accurate than the formula mg(r_{2}– r_{1}) for the difference of potential energy between two points r_{2}and r_{1}distance away from the centre of the earth.
(a) decreases
(b) decreases
(c) mass of the body
(d) more.
8.3. Suppose there existed a planet that went around the sun twice as fast as the earth.What would be its orbital size as compared to that of the earth?
Time taken by the Earth to complete one revolution around the Sun,
T_{e} = 1 year
Orbital radius of the Earth in its orbit, R_{e }= 1 AU
Time taken by the planet to complete one revolution around the Sun, T_{P} = ½T_{e} = ½ year
Orbital radius of the planet = R_{p}
From Kepler’s third law of planetary motion, we can write:
(R_{p} / R_{e})^{3} = (T_{p} / T_{e})^{2}
(R_{p} / R_{e}) = (T_{p} / T_{e})^{2/3}
= (½ / 1)^{2/3} = 0.5^{2/3} = 0.63
Hence, the orbital radius of the planet will be 0.63 times smaller than that of the Earth.
8.4. Io, one of the satellites of Jupiter, has an orbital period of 1.769 days and the radius of the orbit is 4.22 × 10^{8} m. Show that the mass of Jupiter is about onethousandth that of the sun.
Orbital period of I_{0} , T_{I0} = 1.769 days = 1.769 × 24 × 60 × 60 s
8.5. Let us assume that our galaxy consists of 2.5 × 10^{11} stars each of one solar mass. How long will a star at a distance of 50,000 ly from the galactic centre take to complete one revolution? Take the diameter of the Milky Way to be 10^{5} ly.
Mass of our galaxy Milky Way, M = 2.5 × 10^{11} solar mass
Solar mass = Mass of Sun = 2.0 × 10^{36} kg
Mass of our galaxy, M = 2.5 × 10^{11} × 2 × 10^{36} = 5 × 10^{41} kg
Diameter of Milky Way, d = 10^{5} ly
Radius of Milky Way, r = 5 × 10^{4} ly
1 ly = 9.46 × 10^{15} m
∴r = 5 × 10^{4} × 9.46 × 10^{15}
= 4.73 ×10^{20} m
Since a star revolves around the galactic centre of the Milky Way, its time period is given by the relation:
T = ( 4π^{2}r^{3} / GM)^{1/2}
= [ (4 × 3.14^{2} × 4.73^{3} × 10^{60}) / (6.67 × 10^{11} × 5 × 10^{41}) ]^{1/2}
= (39.48 × 105.82 × 10^{30} / 33.35 )^{1/2}
= 1.12 × 10^{16} s
1 year = 365 × 324 × 60 × 60 s
1s = 1 / (365 × 324 × 60 × 60) years
∴ 1.12 × 10^{16} s = 1.12 × 10^{16} / (365 × 24 × 60 × 60) = 3.55 × 10^{8} years.
8.6. Choose the correct alternative:
(a) If the zero of potential energy is at infinity, the total energy of an orbiting satellite is negative of its kinetic/potential energy.
(b) The energy required to launch an orbiting satellite out of earth’s gravitational influence is more/less than the energy required to project a stationary object at the same height (as the satellite) out of earth’s influence.
(a) Kinetic energy
(b) Less
8.7. Does the escape speed of a body from the earth depend on
(a) the mass of the body,
(b) the location from where it is projected,
(c) the direction of projection,
(d) the height of the location from where the body is launched?
Answer
The escape velocity is indpendent of the mass of the body and the direction of projection. It depends upon the gravitational potential at the point from where the body is launched. Since, this potential depends slightly on the latitude and height of the point, therefore, the escape velocity depends slightly on these factors.
8.8. A comet orbits the Sun in a highly elliptical orbit. Does the comet have a constant (a) linear speed, (b) angular speed, (c) angular momentum, (d) kinetic energy, (e) potential energy, (f) total energy throughout its orbit? Neglect any mass loss of the comet when it comes very close to the Sun.
Answer
A comet while going on elliptical orbit around the Sun has constant angular momentum and totaal energy at all locations but other quantities vary with locations.
8.9. Which of the following symptoms is likely to afflict an astronaut in space (a) swollen feet, (b) swollen face, (c) headache, (d) orientational problem?
Answer
(a) Legs hold the entire mass of a body in standing position due to gravitational pull. In space, an astronaut feels weightlessness because of the absence of gravity. Therefore, swollen feet of an astronaut do not affect him/her in space.
(b) A swollen face is caused generally because of apparent weightlessness in space. Sense organs such as eyes, ears nose, and mouth constitute a person’s face. This symptom can affect an astronaut in space.
(c) Headaches are caused because of mental strain. It can affect the working of an astronaut in space.
(d) Space has different orientations. Therefore, orientational problem can affect an astronaut in space.
8.10. Choose the correct answer from among the given ones:The gravitational intensity at the centre of a hemispherical shell of uniform mass density has the direction indicated by the arrow (see Fig 8.12) (i) a, (ii) b, (iii) c, (iv) O.
Gravitational potential (V) is constant at all points in a spherical shell. Hence, the gravitational potential gradient (dV/dR) is zero everywhere inside the spherical shell. The gravitational potential gradient is equal to the negative of gravitational intensity. Hence, intensity is also zero at all points inside the spherical shell. This indicates that gravitational forces acting at a point in a spherical shell are symmetric.
If the upper half of a spherical shell is cut out (as shown in the given figure), then the net gravitational force acting on a particle located at centre O will be in the downward direction.
Since gravitational intensity at a point is defined as the gravitational force per unit mass at that point, it will also act in the downward direction. Thus, the gravitational intensity at centre O of the given hemispherical shell has the direction as indicated by arrow c.
8.11. Choose the correct answer from among the given ones:
For the problem 8.10, the direction of the gravitational intensity at an arbitrary point P is indicated by the arrow (i) d, (ii) e, (iii) f, (iv) g.
Gravitational potential (V) is constant at all points in a spherical shell. Hence, the gravitational potential gradient (dV/dR) is zero everywhere inside the spherical shell. The gravitational potential gradient is equal to the negative of gravitational intensity. Hence, intensity is also zero at all points inside the spherical shell. This indicates that gravitational forces acting at a point in a spherical shell are symmetric.
If the upper half of a spherical shell is cut out (as shown in the given figure), then the net gravitational force acting on a particle at an arbitrary point P will be in the downward direction.
Since gravitational intensity at a point is defined as the gravitational force per unit mass at that point, it will also act in the downward direction. Thus, the gravitational intensity at an arbitrary point P of the hemispherical shell has the direction as indicated by arrow e.
Mass of the Sun, M_{s} = 2 × 10^{30} kg
Mass of the Earth, M_{e} = 6 × 10 ^{24} kg
Orbital radius, r = 1.5 × 10^{11} m
Mass of the rocket = m
From Newton’s law of gravitation, we can equate gravitational forces acting on satellite P under the influence of the Sun and the Earth as:
GmM_{s} / (r – x)^{2} = GmM_{e} / x^{2}
[ (r – x) / x ]^{2} = M_{s} / M_{e}
(r – x) / x = [ 2 × 10^{30} / 60 × 10^{24}]^{1/2} = 577.35
1.5 × 10^{11} – x = 577.35x
578.35x = 1.5 × 10^{11}
x = 1.5 × 10^{11} / 578.35 = 2.59 × 10^{8} m.
8.13.How will you ‘weigh the sun’, that is estimate its mass? The mean orbital radius of the earth around the sun is 1.5 × 10^{8} km.
Orbital radius of the Earth around the Sun, r = 1.5 × 10^{11} m
Time taken by the Earth to complete one revolution around the Sun,
T = 1 year = 365.25 days
= 365.25 × 24 × 60 × 60 s
Universal gravitational constant, G = 6.67 × 10^{–11} Nm^{2} kg^{–2}
Thus, mass of the Sun can be calculated using the relation,
M = 4π^{2}r^{3} / GT^{2}
= 4 × 3.14^{2} × (1.5 × 10^{11})^{3} / [ 6.67 × 10^{11} × (365.25 × 24 × 60 × 60)^{2}]
= 2 × 10^{30} kg
Hence, the mass of the Sun is 2 × 10^{30} kg.
8.14. A Saturn year is 29.5 times the earth year. How far is the Saturn from the sun if the earth is 1.50 ×10^{8} km away from the sun?
Distance of the Earth from the Sun, r_{e} = 1.5 × 10^{8} km = 1.5 × 10^{11} m
Time period of the Earth = T_{e}
Time period of Saturn, T_{s} = 29. 5 T_{e}
Distance of Saturn from the Sun = r_{s}
From Kepler’s third law of planetary motion, we have
T = (4π^{2}r^{3} / GM)^{1/2}
For Saturn and Sun, we can write
r_{s}^{3} / r_{e}^{3} = T_{s}^{2} / T_{e}^{2}
r_{s} = r_{e}(T_{s} / T_{e})^{2/3}
= 1.5 × 10^{11} (29.5 T_{e} / T_{e})^{2/3}
= 1.5 × 10^{11} (29.5)^{2/3}
= 14.32 × 10^{11} m
Hence, the distance between Saturn and the Sun is 1.43 × 10^{12} m.
8.15. A body weighs 63 N on the surface of the earth. What is the gravitational force on it due to the earth at a height equal to half the radius of the earth?
Weight of the body, W = 63 N
Acceleration due to gravity at height h from the Earth’s surface is given by the relation:
Where,
g = Acceleration due to gravity on the Earth’s surface
Re = Radius of the Earth
For h = R_{e} / 2
g‘ = g / [(1 + (R_{e} / 2R_{e}) ]^{2}
= g / [1 + (1/2) ]^{2} = (4/9)g
Weight of a body of mass m at height h is given as:
W‘ = mg
= m × (4/9)g = (4/9)mg
= (4/9)W
= (4/9) × 63 = 28 N.
8.16. Assuming the earth to be a sphere of uniform mass density, how much would a body weigh half way down to the centre of the earth if it weighed 250 N on the surface?
Weight of a body of mass m at the Earth’s surface, W = mg = 250 N
Body of mass m is located at depth, d = (1/2)R_{e}
Where,
R_{e} = Radius of the Earth
Acceleration due to gravity at depth g (d) is given by the relation:
g‘ = (1 – (d / R_{e})g
= [1 – (R_{e} / 2R_{e}) ]g = (1/2)g
Weight of the body at depth d,
W‘ = mg‘
= m × (1/2)g = (1/2) mg = (1/2)W
= (1/2) × 250 = 125 N
8.17. A rocket is fired vertically with a speed of 5 km s^{–1} from the earth’s surface. How far from the earth does the rocket go before returning to the earth? Mass of the earth = 6.0 × 10^{24} kg; mean radius of the earth = 6.4 × 10^{6} m; G= 6.67 × 10^{–11} N m^{2} kg^{–}^{2.}
^{
}
Velocity of the rocket, v = 5 km/s = 5 × 10^{3} m/s
Mass of the Earth, M_{e} = 6 × 10^{24} kg
Radius of the Earth, R_{e} = 6.4 × 10^{6} m
Height reached by rocket mass, m = h
At the surface of the Earth,
Total energy of the rocket = Kinetic energy + Potential energy
= (1/2)mv^{2} + (GM_{e}m / R_{e})
At highest point h,
v = 0
And, Potential energy = GM_{e}m / (R_{e} + h)
Total energy of the rocket = 0 + [ GM_{e}m / (R_{e} + h) ]
= GM_{e}m / (R_{e} + h)
From the law of conservation of energy, we have
Total energy of the rocket at the Earth’s surface = Total energy at height h
(1/2)mv^{2} + (GM_{e}m / R_{e}) = GM_{e}m / (R_{e} + h)
(1/2)v^{2} = GM_{e} [ (1/R_{e}) – 1 / (R_{e} + h) ]
= GM_{e}[ (R_{e} + h – R_{e}) / R_{e}(R_{e}+ h) ]
(1/2)v^{2} = gR_{e}h / (R_{e} + h)
Where g = GM / R_{e}^{2} = 9.8 ms^{2}
∴ v^{2} (R_{e} + h) = 2gR_{e}h
v^{2}R_{e} = h(2gR_{e} – v^{2})
h = R_{e}v^{2} / (2gR_{e} – v^{2})
= 6.4 × 10^{6} × (5 × 10^{3})^{2} / [ 2 × 9.8 × 6.4 × 10^{6} – (5 × 10^{3})^{2}
h = 1.6 × 10^{6} m
Height achieved by the rocket with respect to the centre of the Earth = R_{e} + h
= 6.4 × 10^{6} + 1.6 × 10^{6} = 8 × 10^{6} m.
8.18. The escape speed of a projectile on the earth’s surface is 11.2 km s^{–1}. A body is projected out with thrice this speed. What is the speed of the body far away from the earth? Ignore the presence of the sun and other planets.
Escape velocity of a projectile from the Earth, v_{esc }= 11.2 km/s
Projection velocity of the projectile, v_{p} = 3v_{esc}
Mass of the projectile = m
Velocity of the projectile far away from the Earth = v_{f}
Total energy of the projectile on the Earth = (1/2)mv_{p}^{2} – (1/2)mv_{esc}^{2}
Gravitational potential energy of the projectile far away from the Earth is zero.
Total energy of the projectile far away from the Earth = (1/2)mv_{f}^{2}
From the law of conservation of energy, we have
(1/2)mv_{p}^{2} – (1/2)mv_{esc}^{2} = (1/2)mv_{f}^{2}
v_{f} = ( v_{p}^{2} – v_{esc}^{2 })^{1/2}
= [ (3v_{esc})^{2} – v_{esc}^{2} ]^{1/2}
= √8 v_{esc}
= √8 × 11.2 = 31.68 km/s.
8.19. A satellite orbits the earth at a height of 400 km above the surface. How much energy must be expended to rocket the satellite out of the earth’s gravitational influence? Mass of the satellite = 200 kg; mass of the earth = 6.0 ×10^{24} kg; radius of the earth = 6.4 ×10^{6} m; G = 6.67 × 10^{–11} N m^{2} kg^{–2}.
Mass of the Earth, M = 6.0 × 10^{24} kg
Mass of the satellite, m = 200 kg
Radius of the Earth, R_{e} = 6.4 × 10^{6} m
Universal gravitational constant, G = 6.67 × 10^{–11} Nm^{2}kg^{–2}
Height of the satellite, h = 400 km = 4 × 10^{5} m = 0.4 ×10^{6} m
Total energy of the satellite at height h = (1/2)mv^{2} + [ GM_{e}m / (R_{e} + h) ]
Orbital velocity of the satellite, v_{ }= [ GM_{e} / (R_{e} + h) ]^{1/2}
Total energy of height, h = (1/2)GM_{e}m / (R_{e} + h) – GM_{e}m / (R_{e} + h) = (1/2)GM_{e}m / (R_{e} + h)
The negative sign indicates that the satellite is bound to the Earth. This is called bound energy of the satellite.
Energy required to send the satellite out of its orbit = – (Bound energy)
= (1/2) GM_{e}m / (R_{e} + h)
= (1/2) × 6.67 × 10^{11} × 6 × 10^{24} × 200 / (6.4 × 10^{6} + 0.4 × 10^{6})
= 5.9 × 10^{9} J.
8.20. Two stars each of one solar mass (= 2× 10^{30} kg) are approaching each other for a head on collision. When they are a distance 109 km, their speeds are negligible. What is the speed with which they collide? The radius of each star is 104 km. Assume the stars to remain undistorted until they collide. (Use the known value of G).
Mass of each star, M = 2 × 10^{30 }kg
Radius of each star, R = 10^{4} km = 10^{7} m
Distance between the stars, r = 10^{9} km = 10^{12}m
For negligible speeds, v = 0 total energy of two stars separated at distance r
= [ GMM / r ] + (1/2)mv^{2}
= [ GMM / r ] + 0 ….(i)
Now, consider the case when the stars are about to collide:
Velocity of the stars = v
Distance between the centers of the stars = 2R
Total kinetic energy of both stars = (1/2) Mv^{2} + (1/2)Mv^{2} = Mv^{2}
Total potential energy of both stars = GMM / 2R
Total energy of the two stars = Mv^{2} – GMM / 2R ….(ii)
Using the law of conservation of energy, we can write:
Mv^{2} – GMM / 2R = GMM / r
v^{2} = GM / r + GM / 2R
= GM [ (1/r) + (1/2R) ]
= 6.67 × 10^{11} × 2 × 10^{30} [ (1/10^{12} ) + (1 / 2 × 10^{7}) ]
~ 6.67 × 10^{12}
v = ( 6.67 × 10^{12})^{1/2} = 2.58 × 10^{6} m/s.
8.21. Two heavy spheres each of mass 100 kg and radius 0.10 m are placed 1.0 m apart on a horizontal table. What is the gravitational force and potential at the mid point of the line joining the centers of the spheres? Is an object placed at that point in equilibrium? If so, is the equilibrium
stable or unstable?
Answer
Grvitational field at the midpoint of the line joining the centres of the two spheres
= GM/(r/2)^{2} (alog negative r) + GM/(r/2) (along r) = 0
Gravitational potential at the midpoint f the line joining the centres of the two spheres is
V = – GM/r/2 + (GM/r/2) = 4GM/r = 4 × 6.67 × 10^{11} × 100/1.0
= 2.7 × 10^{8} J/Kg
As the effective force on the body placed at midpoint is zero, sso the body is in equilibrium. If the body is displaced a little towards either mass body from its equilibrium position, it will not return back to its inital position of equilibrium. Hence, the body is in unstable equilibrium.
8.22. As you have learnt in the text, a geostationary satellite orbits the earth at a height of nearly 36,000 km from the surface of the earth. What is the potential due to earth’s gravity at the site of this satellite? (Take the potential energy at infinity to be zero). Mass of the earth = 6.0 × 10^{24} kg, radius = 6400 km.
Mass of the Earth, M = 6.0 × 10^{24} kg
Radius of the Earth, R = 6400 km = 6.4 × 10^{6} m
Height of a geostationary satellite from the surface of the Earth,
h = 36000 km = 3.6 × 10^{7} m
Gravitational potential energy due to Earth’s gravity at height h,
= GM / (R + h)
= – 6.67 × 10^{11} × 6 × 10^{24} / (3.6 × 10^{7} + 0.64 × 10^{7})
= 9.4 × 10^{6} J/kg.
8.23. A star 2.5 times the mass of the sun and collapsed to a size of 12 km rotates with a speed of 1.2 rev. per second. (Extremely compact stars of this kind are known as neutron stars. Certain stellar objects called pulsars belong to this category). Will an object placed on its equator remain stuck to its surface due to gravity? (Mass of the sun = 2 × 10^{30} kg).
A body gets stuck to the surface of a star if the inward gravitational force is greater than the outward centrifugal force caused by the rotation of the star.
Gravitational force, f_{g} = – GMm / R^{2}
Where,
M = Mass of the star = 2.5 × 2 × 10^{30} = 5 × 10^{30 }kg
m = Mass of the body
R = Radius of the star = 12 km = 1.2 ×10^{4} m
∴ f_{g} = 6.67 × 10^{11} × 5 × 10^{30} × m / (1.2 × 10^{4})^{2} = 2.31 × 10^{11} m N
Centrifugal force, f_{c}^{ }= mrω^{2}
ω = Angular speed = 2πν
ν = Angular frequency = 1.2 rev s^{–1}
f_{c} = mR (2πν)^{2}
= m × (1.2 ×10^{4}) × 4 × (3.14)^{2} × (1.2)^{2} = 1.7 ×10^{5}m^{ }N
Since f_{g} > f_{c}, the body will remain stuck to the surface of the star.
8.24. A spaceship is stationed on Mars. How much energy must be expended on the spaceship to launch it out of the solar system? Mass of the space ship = 1000 kg; mass of the Sun = 2 × 10^{30} kg; mass of mars = 6.4 × 10^{23} kg; radius of mars = 3395 km; radius of the orbit of mars = 2.28 × 10^{8}kg; G= 6.67 × 10^{–11} m^{2}kg^{–2}.
Mass of the spaceship, m_{s }= 1000 kg
Mass of the Sun, M = 2 × 10^{30} kg
Mass of Mars, m_{m} = 6.4 × 10 ^{23} kg
Orbital radius of Mars, R = 2.28 × 10^{8 }kg =2.28 × 10^{11}m
Radius of Mars, r = 3395 km = 3.395 × 10^{6} m
Universal gravitational constant, G = 6.67 × 10^{–11} m^{2}kg^{–2}
Potential energy of the spaceship due to the gravitational attraction of the Sun = GMm_{s} / R
Potential energy of the spaceship due to the gravitational attraction of Mars = GM_{m}m_{s} / r
Since the spaceship is stationed on Mars, its velocity and hence, its kinetic energy will be zero.
Total energy of the spaceship = GMm_{s} / R – GM_{m}m_{s} / r
= Gm_{s}[ (M / R) + (m_{m} / r) ]
The negative sign indicates that the system is in bound state.
Energy required for launching the spaceship out of the solar system
= – (Total energy of the spaceship)
= Gm_{s}[ (M / R) + (m_{m} / r) ]
= 6.67 × 10^{11 }× 10^{3} × [ (2 × 10^{30} / 2.28 × 10^{11}) + (6.4 × 10^{23} / 3.395 × 10^{6} ) ]
= 596.97 × 10^{9} = 6 × 10^{11} J.
8.25. A rocket is fired ‘vertically’ from the surface of mars with a speed of 2 km s–1. If 20% of its initial energy is lost due to Martian atmospheric resistance, how far will the rocket go from the surface of mars before returning to it? Mass of mars = 6.4× 1023 kg; radius of mars = 3395 km; G = 6.67× 10^{11} N m^{2} kg^{–2}.
Initial velocity of the rocket, v = 2 km/s = 2 × 10^{3} m/s
Mass of Mars, M = 6.4 × 10^{23} kg
Radius of Mars, R = 3395 km = 3.395 × 10^{6} m
Universal gravitational constant, G = 6.67× 10^{–11} N m^{2} kg^{–2}
Mass of the rocket = m
Initial kinetic energy of the rocket = (1/2)mv^{2}
Initial potential energy of the rocket = GMm / R
Total initial energy = (1/2)mv^{2}– GMm / R
If 20 % of initial kinetic energy is lost due to Martian atmospheric resistance, then only 80 % of its kinetic energy helps in reaching a height.
Total initial energy available = (80/100) × (1/2) mv^{2} – GMm / R = 0.4mv^{2} – GMm / R
Maximum height reached by the rocket = h
At this height, the velocity and hence, the kinetic energy of the rocket will become zero.
Total energy of the rocket at height h = GMm / (R + h)
Applying the law of conservation of energy for the rocket, we can write:
0.4mv^{2} – GMm / R = GMm / (R + h)
0.4v^{2} = GM / R – GM / (R + h)
= GMh / R(R + h)
(R + h) / h = GM / 0.4v^{2}R
R / h = ( GM / 0.4v^{2}R ) – 1
h = R / [ (GM / 0.4v^{2}R) – 1 ]
= 0.4R^{2}v^{2} / (GM – 0.4v^{2}R)
= 0.4 × (3.395 × 10^{6})^{2} × (2 × 10^{3})^{2} / [ 6.67 × 10^{11} × 6.4 × 10^{23} – 0.4 × (2 × 10^{3})^{2} × (3.395 × 10^{6}) ]
= 18.442 × 10^{18} / [ 42.688 × 10^{12} – 5.432 × 10^{12} ]
= 18.442 × 10^{6 }/ 37.256
= 495 × 10^{3} m = 495 km.