Follow Us
Select Medium / माध्यम चुनें:
Eng (English) Beng (বাংলা) Hindi (हिन्दी)
WBB • Class XI • Physics • Ch 6
Estimated Time: 45 Mins
Study Progress: In Progress

Gravitation

Gravitation is the universal attractive interaction that orchestrates the large-scale architecture and dynamical evolution of the cosmos. Discovered by Sir Isaac Newton in 1687, the Universal Law of Gravitation unified terrestrial mechanics with celestial dynamics under a single inverse-square law. This chapter develops the physics of gravitational interactions, beginning with Kepler's empirical laws of planetary motion and their rigorous derivation via angular momentum conservation and central force dynamics. We analyze the universal gravitational constant, the acceleration due to gravity, and its precise variations with altitude, depth, latitude, and Earth's oblate spheroid geometry. We investigate gravitational field intensity, gravitational potential, and potential energy. We derive the energetics of escape velocity and the conditions governing black holes. Finally, we explore satellite mechanics, deriving orbital speeds, revolutionary periods, and energy states of geostationary and polar satellites, along with the true physical nature of orbital weightlessness. This integrated curriculum provides West Bengal Board (WBCHSE) students with a rigorous conceptual and mathematical foundation essential for school board examinations and national entrance tests such as WBJEE, JEE Main, and NEET.

Why This Chapter Matters

Without gravitation, stars could not ignite thermonuclear fusion, planets could not form or retain life-supporting atmospheres, and galaxies would drift apart into cosmic void. In contemporary science and technology, the principles of gravitation govern every facet of space exploration, global telecommunications, weather monitoring, and navigation. GPS satellite constellations must constantly account for both Newtonian orbital variations and gravitational time dilation to deliver metric positional accuracy on Earth. Understanding gravitational field variations, tidal resonance, orbital maneuvers, and orbital transfers forms the indispensable bedrock of modern aerospace engineering and astrophysics.

Chapter Roadmap & Progression

1 1. Kepler's Laws of Planetary Motio...
2 2. Newton's Universal Law of Gravit...
3 3. Acceleration Due to Gravity (g)...
4 4. Gravitational Field, Potential a...
5 5. Escape Velocity, Binding Energy...
6 6. Satellite Mechanics, Orbital Vel...

Complete Concept Guide (100% Curriculum Coverage)

1. Kepler's Laws of Planetary Motion & Inverse-Square Law

Kepler's Three Laws of Planetary Motion

Between 1609 and 1619, Johannes Kepler formulated three empirical laws based on Tycho Brahe's meticulous observational data of planetary positions:

  1. First Law (Law of Orbits): Every planet moves in an elliptical orbit around the Sun, with the Sun situated at one of the two focal points of the ellipse.

    An ellipse is characterized by its semi-major axis $a$, semi-minor axis $b$, and eccentricity $e = \sqrt{1 - b^2/a^2}$ ($0 \le e < 1$). The closest approach to the Sun is the perihelion at distance $r_p = a(1 - e)$, and the farthest point is the aphelion at distance $r_a = a(1 + e)$.

  2. Second Law (Law of Areas): The radius vector drawn from the Sun to a planet sweeps out equal areas in equal intervals of time. That is, the areal velocity of a planet is strictly constant:$$\frac{dA}{dt} = \text{constant}$$
    Proof via Conservation of Angular Momentum: Consider a planet of mass $m$ moving with velocity $\vec{v}$ at position $\vec{r}$ relative to the Sun. In an infinitesimal time $dt$, its displacement is $d\vec{r} = \vec{v}\,dt$. The area swept out is the triangular area $dA = \frac{1}{2}|\vec{r} \times d\vec{r}| = \frac{1}{2}|\vec{r} \times \vec{v}|\,dt$. Thus:$$\frac{dA}{dt} = \frac{1}{2}|\vec{r} \times \vec{v}| = \frac{|\vec{r} \times m\vec{v}|}{2m} = \frac{L}{2m}$$Because the gravitational force exerted by the Sun is purely central (directed along $-\hat{r}$), the net torque is zero: $\vec{\tau} = \vec{r} \times \vec{F}_g = 0$. Therefore, total angular momentum $\vec{L}$ is conserved, proving that $\frac{dA}{dt} = \frac{L}{2m} = \text{constant}$.

    A direct consequence is that the planet moves fastest at perihelion and slowest at aphelion: $v_p r_p = v_a r_a$.

  3. Third Law (Law of Periods): The square of the orbital period of revolution ($T$) of a planet is directly proportional to the cube of the semi-major axis ($a$) of its elliptical orbit:$$T^2 \propto a^3 \implies \frac{T^2}{a^3} = \text{constant}$$
Deduction of Newton's Inverse-Square Law from Kepler's Third Law

Assuming a planet of mass $m$ moves in a circular orbit of radius $r$ around the Sun of mass $M_s$ with constant speed $v$ and period $T$:

The required centripetal force is $F = \frac{m v^2}{r} = m \left(\frac{2\pi r}{T}\right)^2 \frac{1}{r} = \frac{4\pi^2 m r}{T^2}$.

From Kepler's Third Law, $T^2 = k r^3$. Substituting into the force equation:

$$F = \frac{4\pi^2 m r}{k r^3} = \left(\frac{4\pi^2}{k}\right) \frac{m}{r^2} \implies F \propto \frac{1}{r^2}$$

Newton recognized that by his Third Law, the force must also be directly proportional to the mass of the Sun $M_s$, leading directly to the Universal Law of Gravitation: $F = G\frac{M_s m}{r^2}$.

2. Newton's Universal Law of Gravitation & Gravitational Constant

Statement of Newton's Universal Law of Gravitation

Every particle of matter in the universe attracts every other particle with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between their centers:

$$F = G\frac{m_1 m_2}{r^2}$$

Vector Formulation: If $\vec{r}_{12}$ is the position vector of particle 1 with respect to particle 2, the gravitational force $\vec{F}_{12}$ exerted on particle 1 by particle 2 is:

$$\vec{F}_{12} = -G\frac{m_1 m_2}{r_{12}^2}\hat{r}_{12} = -G\frac{m_1 m_2}{|\vec{r}_{12}|^3}\vec{r}_{12}$$

Similarly, $\vec{F}_{21} = -\vec{F}_{12}$. Gravitational interaction satisfies Newton's Third Law identically, forming an action-reaction pair.

Essential Characteristics of Gravitational Force:

  • It is always purely attractive.
  • It is a central force (acts along the line joining the centers of mass of the two bodies).
  • It is a conservative force (work done in any closed path is zero: $\oint \vec{F}\cdot d\vec{r} = 0$).
  • It is completely independent of the intervening medium between the masses.
  • It obeys the Principle of Superposition: The total gravitational force on a particle due to multiple surrounding masses is the vector sum of individual pairwise forces: $\vec{F}_{\text{net}} = \sum_{i=2}^N \vec{F}_{1i}$.
Universal Gravitational Constant ($G$)

The constant $G$ represents the magnitude of the gravitational attraction between two point masses of $1\,\text{kg}$ each separated by a distance of $1\,\text{m}$.

  • SI Value: $G = 6.6743 \times 10^{-11}\,\text{N}\cdot\text{m}^2/\text{kg}^2 = 6.6743 \times 10^{-11}\,\text{m}^3/(\text{kg}\cdot\text{s}^2)$
  • CGS Value: $6.6743 \times 10^{-8}\,\text{dyn}\cdot\text{cm}^2/\text{g}^2$
  • Dimensional Formula: $[G] = \frac{[F][r^2]}{[m^2]} = \frac{[MLT^{-2}][L^2]}{[M^2]} = [M^{-1}L^3T^{-2}]$

Cavendish Experiment (1798): Henry Cavendish determined $G$ experimentally using a sensitive quartz-fiber torsion balance, measuring the deflection caused by large lead spheres on small suspended gold spheres.

Inertial Mass vs Gravitational Mass & Principle of Equivalence

Inertial mass ($m_i$) is the measure of a body's resistance to acceleration when subjected to any external force ($F = m_i a$). Gravitational mass ($m_g$) is the measure of the strength of a body's gravitational interaction ($F_g = G\frac{M m_g}{r^2}$).

Experiments by Eötvös, Dicke, and Braginsky have verified to a precision of 1 part in $10^{15}$ that $m_i = m_g$. This fundamental identity is known as Einstein's Principle of Equivalence, establishing that gravitational acceleration is independent of the mass or composition of the falling body.

3. Acceleration Due to Gravity (g) & Its Multi-Factor Variations

Relation Between $g$ and $G$

For a body of mass $m$ resting on the surface of Earth (mass $M$, radius $R$), its weight equals the gravitational force exerted by Earth:

$$m g = G\frac{M m}{R^2} \implies g = \frac{GM}{R^2}$$

Expressing mass in terms of uniform mean density $\rho$: $M = \frac{4}{3}\pi R^3 \rho$, which yields:

$$g = \frac{G}{R^2}\left(\frac{4}{3}\pi R^3 \rho\right) = \frac{4}{3}\pi G \rho R$$

On Earth's surface, the standard mean value is $g \approx 9.8\,\text{m/s}^2 = 980\,\text{cm/s}^2$.

1. Variation of $g$ with Altitude (Height $h$ Above Surface)

At an altitude $h$ above the Earth's surface, the distance from the center is $r = R + h$:

$$g_h = \frac{GM}{(R + h)^2} = \frac{GM}{R^2\left(1 + \frac{h}{R}\right)^2} = \frac{g}{\left(1 + \frac{h}{R}\right)^2} = g\left(1 + \frac{h}{R}\right)^{-2}$$

When $h \ll R$ (for heights up to a few hundred kilometers), expanding using the Binomial Theorem and neglecting higher-order terms:

$$g_h \approx g\left(1 - \frac{2h}{R}\right)$$

Fractional decrease: $\frac{\Delta g}{g} = \frac{g - g_h}{g} = \frac{2h}{R}$. Percentage decrease: $\frac{2h}{R} \times 100\%$.

2. Variation of $g$ with Depth ($d$ Below Surface)

At a depth $d$ below the Earth's surface, the distance from the center is $(R - d)$. By Gauss's Law of gravitation, the spherical shell of thickness $d$ exerts zero net force at internal points. Only the inner solid sphere of radius $(R - d)$ attracts the mass:

$$M' = \frac{4}{3}\pi (R - d)^3 \rho$$$$g_d = \frac{GM'}{(R - d)^2} = \frac{4}{3}\pi G \rho (R - d) = \left(\frac{4}{3}\pi G \rho R\right)\left(\frac{R - d}{R}\right) = g\left(1 - \frac{d}{R}\right)$$

Important Conclusions:

  • At the center of the Earth ($d = R$): $g_{\text{center}} = g(1 - R/R) = 0$. A body at the center of the Earth is weightless.
  • Comparing height and depth for small distances ($h = d$): $\Delta g_h = 2\Delta g_d$. The decrease in $g$ at height $h$ is twice the decrease at the same depth $d$.
3. Variation of $g$ with Latitude ($\lambda$) Due to Earth's Rotation

As the Earth rotates about its polar axis with angular speed $\omega = \frac{2\pi}{86400} \approx 7.27 \times 10^{-5}\,\text{rad/s}$, a body at latitude $\lambda$ describes a circular path of radius $r = R\cos\lambda$. It experiences an outward centrifugal pseudo-force $m\omega^2 r = m\omega^2 R\cos\lambda$.

Resolving along the local vertical, the apparent acceleration due to gravity is:

$$g_\lambda = g - \omega^2 R \cos^2\lambda$$
  • At the Equator ($\lambda = 0^\circ$): $\cos 0^\circ = 1 \implies g_{\text{eq}} = g - \omega^2 R$ (Minimum value).
  • At the Poles ($\lambda = 90^\circ$): $\cos 90^\circ = 0 \implies g_{\text{pole}} = g$ (Maximum value, completely unaffected by rotation).
  • Difference due to rotation: $g_{\text{pole}} - g_{\text{eq}} = \omega^2 R \approx (7.27 \times 10^{-5})^2 (6.4 \times 10^6) \approx 0.034\,\text{m/s}^2$.
4. Variation of $g$ Due to Earth's Oblate Shape

Earth is an oblate spheroid, flattened at the poles and bulging at the equator: $R_{\text{eq}} - R_{\text{pole}} \approx 21\,\text{km}$. Since $g \propto 1/R^2$, the polar radius being smaller makes $g$ larger at the poles than at the equator by about $0.018\,\text{m/s}^2$. Combined with rotation, total difference is $\approx 0.052\,\text{m/s}^2$ ($g_{\text{pole}} \approx 9.83\,\text{m/s}^2$, $g_{\text{eq}} \approx 9.78\,\text{m/s}^2$).

4. Gravitational Field, Potential and Gravitational Potential Energy

Gravitational Field Intensity ($\vec{E}_g$)

The Gravitational Field Intensity at any point in space is defined as the gravitational force experienced per unit test mass placed at that point:

$$\vec{E}_g = \lim_{m_0 \to 0}\frac{\vec{F}}{m_0} = -\frac{GM}{r^2}\hat{r}$$

It is a vector quantity pointing radially toward the attracting mass $M$. Units: $\text{N/kg}$ or $\text{m/s}^2$, dimensions: $[LT^{-2}]$. Near Earth's surface, $\vec{E}_g = \vec{g}$.

Gravitational Potential ($V$)

The Gravitational Potential at a point is defined as the amount of work done by an external agent in bringing a unit mass from infinity to that point without acceleration:

$$V(r) = -\int_\infty^r \vec{E}_g \cdot d\vec{r} = -\int_\infty^r \left(-\frac{GM}{r'^2}\right)dr' = -\left[\frac{GM}{r'}\right]_\infty^r = -\frac{GM}{r}$$

Properties of Gravitational Potential:

  • It is a scalar quantity.
  • It is always negative throughout space, taking its maximum value of zero at infinity ($r \to \infty$). The negative sign signifies that the gravitational interaction is attractive and work is done by the field itself.
  • Units: $\text{J/kg}$, dimensional formula: $[L^2T^{-2}]$.
  • Relation to field intensity: $\vec{E}_g = -\nabla V = -\frac{dV}{dr}\hat{r}$.
Gravitational Potential Energy ($U$)

The Gravitational Potential Energy of a system of two masses $M$ and $m$ separated by distance $r$ is the work done in bringing mass $m$ from infinity to distance $r$ in the field of $M$:

$$U(r) = m V(r) = -\frac{GMm}{r}$$
Work Done in Raising a Mass to Height $h$ Above Earth's Surface

On Earth's surface ($r_1 = R$), potential energy is $U_1 = -\frac{GMm}{R}$.

At height $h$ ($r_2 = R + h$), potential energy is $U_2 = -\frac{GMm}{R + h}$.

The change in potential energy (work required by external agent) is:

$$\Delta U = U_2 - U_1 = GMm\left(\frac{1}{R} - \frac{1}{R + h}\right) = GMm\left(\frac{h}{R(R + h)}\right) = \frac{GMmh}{R^2\left(1 + \frac{h}{R}\right)}$$

Substituting $GM = g R^2$:

$$\Delta U = \frac{mgh}{1 + \frac{h}{R}}$$

When $h \ll R$, $\frac{h}{R} \to 0$, giving the familiar elementary formula $\Delta U \approx mgh$. However, when $h$ is comparable to $R$ (e.g. $h = R$), $\Delta U = \frac{mgh}{1 + 1} = \frac{1}{2}mgh$.

5. Escape Velocity, Binding Energy & Atmospheric Retention

Concept and Derivation of Escape Velocity ($v_e$)

Escape Velocity is defined as the minimum initial projection speed required for an object launched from the surface of a celestial body to completely overcome its gravitational attraction and reach infinity with zero or positive residual kinetic energy.

Let an object of mass $m$ be projected with speed $v_e$ from the surface of a planet of mass $M$ and radius $R$.

Total initial mechanical energy on the planet's surface:

$$E_i = K_i + U_i = \frac{1}{2}m v_e^2 - \frac{GMm}{R}$$

At infinity ($r \to \infty$), the gravitational potential energy is zero ($U_f = 0$), and for minimum escape speed, the final kinetic energy is zero ($K_f = 0$). By Conservation of Mechanical Energy:

$$E_i = E_f \implies \frac{1}{2}m v_e^2 - \frac{GMm}{R} = 0$$$$v_e = \sqrt{\frac{2GM}{R}}$$

Using $GM = g R^2$ and $M = \frac{4}{3}\pi R^3 \rho$:

$$v_e = \sqrt{2gR} = \sqrt{\frac{8}{3}\pi G \rho R^2} = R\sqrt{\frac{8}{3}\pi G \rho}$$
Numerical Value for Earth and Key Characteristics

For Earth ($R = 6.4 \times 10^6\,\text{m}$, $g = 9.8\,\text{m/s}^2$):

$$v_e = \sqrt{2 \times 9.8 \times 6.4 \times 10^6} = \sqrt{1.2544 \times 10^8} \approx 11200\,\text{m/s} = 11.2\,\text{km/s}$$

Critical Characteristics of Escape Velocity:

  • Independent of projectile mass ($m$): A pebble and a Saturn V rocket have identical escape speeds ($11.2\,\text{km/s}$).
  • Independent of projection angle ($\theta$): Whether launched vertically or at $30^\circ$ to the horizontal, the escape speed is identical (neglecting air resistance).
  • Depends solely on the mass $M$ and radius $R$ (or density $\rho$ and radius $R$) of the celestial body.
Atmospheric Retention: Why Does the Moon Have No Atmosphere?

For the Moon ($M_m \approx \frac{M_e}{81}, R_m \approx \frac{R_e}{4}$):

$$v_{e,\text{moon}} = \sqrt{\frac{2GM_m}{R_m}} \approx 2.38\,\text{km/s}$$

The root-mean-square thermal speed of common atmospheric gas molecules ($O_2, N_2, CO_2, H_2O$) at lunar daytime temperature ($T \approx 400\,\text{K}$) is given by $v_{\text{rms}} = \sqrt{\frac{3k_B T}{m_{\text{molecule}}}}$. Because the thermal speeds exceed or are comparable to $v_{e,\text{moon}}$, the gas molecules escaped into space over cosmic timescales, leaving the Moon without any atmosphere.

Black Holes & Schwarzschild Radius

If a dying star collapses such that its escape velocity equals or exceeds the speed of light $c = 3 \times 10^8\,\text{m/s}$ ($v_e \ge c$):

$$\sqrt{\frac{2GM}{R_s}} \ge c \implies R_s = \frac{2GM}{c^2}$$

$R_s$ is called the Schwarzschild radius. Nothing, not even light, can escape from inside this event horizon, defining a black hole.

6. Satellite Mechanics, Orbital Velocity, Geostationary Satellites & Weightlessness

Orbital Velocity of an Artificial Satellite ($v_o$)

Consider a satellite of mass $m$ revolving in a circular orbit of radius $r = R + h$ around Earth (mass $M$, radius $R$).

The gravitational force provides the necessary centripetal force:

$$\frac{m v_o^2}{R + h} = \frac{GMm}{(R + h)^2} \implies v_o = \sqrt{\frac{GM}{R + h}} = R\sqrt{\frac{g}{R + h}}$$

For a satellite orbiting close to Earth's surface ($h \ll R$):

$$v_o = \sqrt{\frac{GM}{R}} = \sqrt{gR} = \sqrt{9.8 \times 6.4 \times 10^6} \approx 7920\,\text{m/s} \approx 7.92\,\text{km/s} \approx 8\,\text{km/s}$$
Fundamental Relation: Escape Velocity vs Orbital Velocity:$$v_e = \sqrt{2gR} = \sqrt{2}\,v_o \approx 1.414\,v_o$$If the orbital velocity of a satellite is increased by $(\sqrt{2} - 1) \approx 41.4\%$ (or if its kinetic energy is doubled), it escapes the gravitational field along a parabolic trajectory.
Time Period and Energy of a Satellite

Period of revolution ($T$):

$$T = \frac{2\pi r}{v_o} = \frac{2\pi (R + h)}{\sqrt{GM/(R + h)}} = \frac{2\pi (R + h)^{3/2}}{\sqrt{GM}} = 2\pi\sqrt{\frac{(R + h)^3}{gR^2}}$$

For near-Earth orbit ($h \approx 0$): $T_0 = 2\pi\sqrt{\frac{R}{g}} = 2\pi\sqrt{\frac{6.4 \times 10^6}{9.8}} \approx 5078\,\text{s} \approx 84.6\,\text{mins}$.

Satellite Energy Relations:

  • Kinetic Energy: $K = \frac{1}{2}m v_o^2 = \frac{GMm}{2r} = \frac{|U|}{2}$
  • Potential Energy: $U = -\frac{GMm}{r}$
  • Total Mechanical Energy: $E = K + U = \frac{GMm}{2r} - \frac{GMm}{r} = -\frac{GMm}{2r} = -K = \frac{U}{2}$
  • Binding Energy: $\text{BE} = -E = \frac{GMm}{2r}$ (energy required to free satellite to infinity)
Geostationary vs Polar Satellites
ParameterGeostationary Satellite (GEO)Polar Satellite (LEO)
Orbital PlaneEquatorial plane (inclination $0^\circ$)Passes over North and South poles (inclination $\approx 90^\circ$)
Orbital Altitude ($h$)$\approx 35,800\,\text{km} \approx 36,000\,\text{km}$ ($r \approx 6.6 R$)$\approx 500\text{--}800\,\text{km}$
Time Period ($T$)$24\,\text{hours}$ (synchronized with Earth's rotation)$\approx 100\,\text{minutes}$
Direction of OrbitWest to East (same as Earth)North to South (crosses equator)
Primary ApplicationsTelecommunications, DTH television, global weather monitoring (INSAT)Remote sensing, crop mapping, military surveillance, environmental monitoring (IRS)
Physical Origin of Weightlessness in Orbit

A common misconception is that astronauts in orbit experience weightlessness because "gravity is zero in space." In reality, at an ISS altitude of $400\,\text{km}$, $g_h = g(1 + h/R)^{-2} \approx 8.7\,\text{m/s}^2$, which is nearly $89\%$ of surface gravity!

The true reason for weightlessness is that the spacecraft and the astronaut are in a state of continuous free fall toward Earth with identical acceleration $a = g_h$. Because both accelerate together, the normal reaction force exerted by the spaceship floor on the astronaut is zero: $N = m(g_h - a) = 0$. Since human sensation of weight is provided by the contact reaction force $N$, the absence of $N$ produces the sensation of absolute weightlessness.

Key Formulas, Laws & Physical Constants

Newton's Universal Law of Gravitation
$$F = G · (m₁m₂) / r², F_vec = -G · (m₁m₂ / r³) · r_vec$$
Kepler's Third Law (Harmonic Law)
T² = (4π² / GM) · a³ ⇒ T² ∝ a³
Variations of Acceleration Due to Gravity (g)
$$Altitude: g_h ≈ g(1 - 2h/R), Depth: g_d = g(1 - d/R), Latitude: g_λ = g - ω²R cos²λ$$
Gravitational Potential & Potential Energy
V = -GM / r, U = -GMm / r, ΔU = mgh / (1 + h/R)
Escape Velocity
$$v_e = √(2GM / R) = √(2gR) = R · √(8πGρ / 3)$$
Satellite Orbital Velocity & Period
$$v_o = √(GM / r), T = 2π√(r³ / GM), v_e = √2 · v_o$$

Conceptual Solved Examples & Case Studies

Example 1
At what height above the surface of the Earth does the acceleration due to gravity become one-fourth of its value on the surface? (Radius of Earth = R).
Step-by-Step Solution:
Step 1: Write the exact formula for variation of g with height:
$$g_h = \frac{g}{\left(1 + \frac{h}{R}\right)^2}$$
Step 2: Substitute given condition:
Given $g_h = \frac{g}{4}$:
$$\frac{g}{4} = \frac{g}{\left(1 + \frac{h}{R}\right)^2} \implies \left(1 + \frac{h}{R}\right)^2 = 4$$
Step 3: Solve for h:
Taking the positive square root on both sides:
$$1 + \frac{h}{R} = 2 \implies \frac{h}{R} = 1 \implies h = R$$
Final Answer: The acceleration due to gravity drops to one-fourth of its surface value at a height equal to the radius of the Earth ($h = R = 6400\,\text{km}$).
Example 2
Two lead spheres each of radius R and uniform density ρ are placed in contact with each other. Show that the gravitational force between them is directly proportional to R⁴.
Step-by-Step Solution:
Step 1: Express mass of each sphere in terms of radius and density:
Mass of each sphere: $M = \frac{4}{3}\pi R^3 \rho$.

Step 2: Distance between centers:
Since the two spheres touch each other, the distance between their centers is $r = R + R = 2R$.

Step 3: Apply Newton's Law of Gravitation:
$$F = G\frac{M \cdot M}{r^2} = G\frac{M^2}{(2R)^2} = G\frac{\left(\frac{4}{3}\pi R^3 \rho\right)^2}{4R^2}$$
$$F = G\frac{\frac{16}{9}\pi^2 R^6 \rho^2}{4R^2} = \frac{4}{9}\pi^2 G \rho^2 R^4$$
Conclusion: Since $G, \pi,$ and $\rho$ are constants, $F \propto R^4$. Hence proved.
Example 3
The mass of a planet is half that of the Earth and its radius is one-third of the radius of the Earth. If the escape velocity on the surface of the Earth is 11.2 km/s, calculate the escape velocity on the surface of the planet.
Step-by-Step Solution:
Step 1: Write the formula for escape velocity:
$$v_e = \sqrt{\frac{2GM}{R}}$$
Step 2: Form the ratio between planet and Earth:
$$\frac{v_{e,p}}{v_{e,e}} = \sqrt{\frac{M_p}{M_e} \times \frac{R_e}{R_p}}$$
Given: $\frac{M_p}{M_e} = \frac{1}{2}$ and $\frac{R_p}{R_e} = \frac{1}{3} \implies \frac{R_e}{R_p} = 3$.

Step 3: Substitute values:
$$\frac{v_{e,p}}{v_{e,e}} = \sqrt{\frac{1}{2} \times 3} = \sqrt{\frac{3}{2}} = \sqrt{1.5} \approx 1.2247$$
$$v_{e,p} = 1.2247 \times 11.2\,\text{km/s} \approx 13.72\,\text{km/s}$$
Final Answer: The escape velocity on the planet is approximately $13.72\,\text{km/s}$.
Example 4
(a) Derive the expression for the acceleration due to gravity at depth d below Earth's surface. (b) At what depth does the value of g become half of its surface value? Compare this with the height at which g becomes half.
Step-by-Step Solution:
Part (a): Derivation of $g_d$:
Assuming Earth is a uniform sphere of radius $R$ and density $\rho$.
On the surface: $g = \frac{4}{3}\pi G \rho R$.
At depth $d$, the distance from the center is $r = R - d$. The spherical shell of thickness $d$ exerts zero net force at any internal point.
The mass of the inner sphere of radius $(R - d)$ is $M' = \frac{4}{3}\pi (R - d)^3 \rho$.
Gravitational acceleration at depth $d$ is:
$$g_d = \frac{GM'}{(R - d)^2} = \frac{G \left(\frac{4}{3}\pi (R - d)^3 \rho\right)}{(R - d)^2} = \frac{4}{3}\pi G \rho (R - d)$$
Dividing $g_d$ by $g$:
$$\frac{g_d}{g} = \frac{R - d}{R} = 1 - \frac{d}{R} \implies g_d = g\left(1 - \frac{d}{R}\right)$$
Part (b): Depth where $g_d = g/2$:
$$\frac{g}{2} = g\left(1 - \frac{d}{R}\right) \implies 1 - \frac{d}{R} = \frac{1}{2} \implies d = \frac{R}{2} = 3200\,\text{km}$$
Height where $g_h = g/2$:
$$\frac{g}{2} = \frac{g}{\left(1 + \frac{h}{R}\right)^2} \implies \left(1 + \frac{h}{R}\right)^2 = 2 \implies 1 + \frac{h}{R} = \sqrt{2}$$
$$h = (\sqrt{2} - 1)R \approx 0.414 R \approx 2650\,\text{km}$$
Comparison: The required depth ($d = 0.5R$) is greater than the required height ($h = 0.414R$) because gravity falls off more slowly with depth (linearly) than with height (inverse-square).
Example 5
A satellite of mass m revolves around Earth in a circular orbit at a height h = R above the surface. (a) Find its orbital speed and orbital period in terms of g and R. (b) Find the minimum additional kinetic energy required to impart to this satellite so that it escapes Earth's gravitational field.
Step-by-Step Solution:
Part (a): Orbital speed and period:
Radius of orbit is $r = R + h = R + R = 2R$.
Orbital speed:
$$v_o = \sqrt{\frac{GM}{r}} = \sqrt{\frac{g R^2}{2R}} = \sqrt{\frac{gR}{2}}$$
Orbital period:
$$T = \frac{2\pi r}{v_o} = \frac{2\pi (2R)}{\sqrt{gR/2}} = 4\pi R \sqrt{\frac{2}{gR}} = 4\pi\sqrt{\frac{2R}{g}}$$
Part (b): Minimum additional kinetic energy to escape:
Total mechanical energy in orbit of radius $r = 2R$ is:
$$E = -\frac{GMm}{2r} = -\frac{GMm}{2(2R)} = -\frac{GMm}{4R} = -\frac{mgR}{4}$$
To escape to infinity, the total mechanical energy must be at least zero ($E_{\text{final}} \ge 0$).
Therefore, the energy that must be added to the satellite is the binding energy:
$$\Delta E = 0 - E = +\frac{mgR}{4}$$
Final Answer: (a) $v_o = \sqrt{\frac{gR}{2}}$, $T = 4\pi\sqrt{\frac{2R}{g}}$; (b) Additional energy required = $\frac{1}{4}mgR$.
Example 6
(a) State and prove Kepler's Second Law of Planetary Motion using the principle of conservation of angular momentum. (b) A planet revolves around the Sun in an elliptical orbit. If the ratio of its maximum distance (aphelion) to its minimum distance (perihelion) from the Sun is 3:1, calculate: (i) the ratio of its orbital speeds at perihelion and aphelion, and (ii) the ratio of its areal velocities at these two positions.
Step-by-Step Solution:
Part (a): Statement and Proof of Kepler's Second Law:
Statement: The radius vector drawn from the Sun to a planet sweeps out equal areas in equal intervals of time; that is, the areal velocity $\frac{dA}{dt}$ is constant.

Proof: Let a planet of mass $m$ be at position $\vec{r}$ relative to the Sun at time $t$.
In a small time interval $dt$, the planet moves through displacement $d\vec{r} = \vec{v}\,dt$.
The area swept out by the radius vector is the area of the differential triangle:
$$d\vec{A} = \frac{1}{2}(\vec{r} \times d\vec{r}) = \frac{1}{2}(\vec{r} \times \vec{v}\,dt)$$
Dividing both sides by $dt$ gives the areal velocity:
$$\frac{d\vec{A}}{dt} = \frac{1}{2}(\vec{r} \times \vec{v}) = \frac{\vec{r} \times (m\vec{v})}{2m} = \frac{\vec{L}}{2m}$$
where $\vec{L} = \vec{r} \times \vec{p}$ is the orbital angular momentum of the planet about the Sun.
The gravitational force $\vec{F}_g = -G\frac{M_s m}{r^2}\hat{r}$ acts radially toward the Sun. The torque about the Sun is:
$$\vec{\tau} = \vec{r} \times \vec{F}_g = \vec{r} \times \left(-G\frac{M_s m}{r^2}\hat{r}\right) = 0$$
Since $\vec{\tau} = \frac{d\vec{L}}{dt} = 0$, the angular momentum $\vec{L}$ is strictly constant in time.
Therefore, $\frac{dA}{dt} = \frac{L}{2m} = \text{constant}$. Hence proved.

Part (b): Calculations:
Given: $\frac{r_a}{r_p} = \frac{3}{1} \implies r_a = 3r_p$.
1. Ratio of orbital speeds:
At perihelion and aphelion, the velocity vectors are perpendicular to the radius vectors ($|\vec{r} \times \vec{v}| = r v$).
By conservation of angular momentum ($L_p = L_a$):
$$m v_p r_p = m v_a r_a \implies \frac{v_p}{v_a} = \frac{r_a}{r_p} = \frac{3}{1} = 3$$
2. Ratio of areal velocities:
By Kepler's Second Law, areal velocity is constant at all points of the orbit:
$$\left(\frac{dA}{dt}\right)_p = \left(\frac{dA}{dt}\right)_a \implies \text{Ratio} = 1:1 = 1$$
Final Answer: (i) $v_p : v_a = 3 : 1$; (ii) Ratio of areal velocities = $1 : 1$.

Common Misconceptions & Examiner Traps

Common Misconception

Applying the linear approximation g_h ≈ g(1 - 2h/R) when altitude h is large (e.g. h = R or h = 1000 km).

Scientific Reality & Correction

The formula $g_h \approx g(1 - 2h/R)$ is a first-order Taylor expansion valid ONLY when $h \ll R$ (typically $h < 300\,\text{km}$, or $h < 5\% R$). For larger altitudes, you MUST use the exact formula $g_h = g\left(1 + \frac{h}{R}\right)^{-2} = \frac{g R^2}{(R+h)^2}$.

Common Misconception

Thinking astronauts in the International Space Station float because there is "zero gravity" in space.

Scientific Reality & Correction

At ISS altitude ($h \approx 400\,\text{km}$), the acceleration due to gravity is $g_h \approx 8.7\,\text{m/s}^2$ (~89% of surface gravity!). Weightlessness occurs because the space station and astronauts are in continuous free fall toward Earth with the exact same acceleration. The normal contact force is zero ($N = 0$).

Common Misconception

Assuming escape velocity depends on the angle of launch.

Scientific Reality & Correction

Escape velocity $v_e = \sqrt{2gR}$ is derived strictly from scalar mechanical energy conservation ($E = K + U = 0$). Kinetic energy $K = \frac{1}{2}mv^2$ depends only on speed, not direction. A projectile launched at $30^\circ, 45^\circ,$ or $90^\circ$ has the same escape speed (neglecting atmospheric resistance and obstacles).

Common Misconception

Believing that the total energy of an orbiting satellite can be positive.

Scientific Reality & Correction

For any gravitationally bound system, the total mechanical energy is strictly negative: $E = -\frac{GMm}{2r} = -K = \frac{U}{2} < 0$. A negative energy signifies that the satellite is trapped in an elliptical or circular orbit. If $E = 0$, the orbit is parabolic (escape). If $E > 0$, the orbit is hyperbolic (unbound flyby).

Common Misconception

Equating the rate of decrease of g with height and depth.

Scientific Reality & Correction

For a small distance $x$ ($x \ll R$), the decrease in $g$ with height is $\Delta g_h = \frac{2x}{R}g$, while with depth it is $\Delta g_d = \frac{x}{R}g$. Therefore, $\Delta g_h = 2\Delta g_d$. Gravity decreases TWICE as fast when moving upward into space as when moving downward into a mine.

Gravitation & Orbital Dynamics Visual Infographic

Gravitation: Fundamental Laws, Variations & Orbital Mechanics WBCHSE Physics Class 11 • Kepler's Laws, Variations of g, Escape Velocity & Satellites G 1. Universal Law & Kepler's Laws Newton's Law: F = G · (m₁m₂) / r² Kepler's 3rd Law: T² ∝ a³ (T²/a³ = const) Areal Velocity: dA/dt = L/(2m) = const g 2. Variations of Acceleration (g) Altitude (h << R): g_h ≈ g(1 - 2h/R) Depth (d): g_d = g(1 - d/R) [Center g = 0] Latitude (λ): g_λ = g - ω²R cos²λ [Min at equator] U 3. Gravitational Field & Energy Potential: V = -GM / r (Always negative) Potential Energy: U = -GMm / r Work to Height h: ΔU = mgh / (1 + h/R) v_e 4. Escape Velocity & Satellites Escape Velocity: v_e = √(2gR) ≈ 11.2 km/s Orbital Velocity: v_o = √(gR) | v_e = √2 · v_o Geostationary: h ≈ 35,800 km, T = 24 hrs TargetExams Gold Standard Series • West Bengal Council of Higher Secondary Education

Chapter Summary & 10 Key Takeaways

Takeaway 1
Kepler's Second Law states that areal velocity is constant (dA/dt = L/2m), which is a direct consequence of angular momentum conservation under central gravitational force.
Takeaway 2
Newton's Universal Law of Gravitation (F = G·m₁m₂/r²) is an inverse-square central force that is always attractive, conservative, and independent of the intervening medium.
Takeaway 3
The universal gravitational constant G has magnitude 6.674 × 10⁻¹¹ N·m²/kg² and dimensions [M⁻¹ L³ T⁻²], experimentally measured by Henry Cavendish.
Takeaway 4
On Earth's surface, acceleration due to gravity is g = GM/R² = 4/3 πGρR ≈ 9.8 m/s².
Takeaway 5
With altitude, g decreases inversely with (R+h)²; for h ≪ R, the approximation is g_h ≈ g(1 - 2h/R).
Takeaway 6
With depth, g decreases linearly: g_d = g(1 - d/R), becoming zero at the center of the Earth.
Takeaway 7
Due to Earth's diurnal rotation, apparent gravity varies with latitude: g_λ = g - ω²R cos²λ, being minimum at the equator and maximum at the poles.
Takeaway 8
Gravitational potential V = -GM/r is a negative scalar that reaches zero at infinity, and gravitational potential energy is U = -GMm/r.
Takeaway 9
Escape velocity from Earth's surface is v_e = √(2gR) ≈ 11.2 km/s, completely independent of the projectile's mass and angle of projection.
Takeaway 10
For circular satellite orbits, orbital velocity is v_o = √(gR) ≈ 7.92 km/s; escape velocity relates to orbital speed by v_e = √2 · v_o; geostationary satellites orbit at h ≈ 35,800 km with T = 24 hours.

Check Your Understanding (Diagnostic Practice Questions)

Diagnostic questions testing core conceptual clarity. Answers are hidden initially — solve each problem first, then click to reveal the step-by-step verified solution.

1
If the radius of the Earth were to shrink by 1% while its mass remained unchanged, by what percentage would the acceleration due to gravity on its surface change?
Reveal Answer & Explanation
Answer:
Use fractional differentiation: dg/g = -2 dR/R for small percentage changes.
2
Show that the orbital period of revolution of a satellite orbiting close to the surface of a planet depends only on the mean density ρ of the planet.
Reveal Answer & Explanation
Answer:
Substitute M = 4/3 πR³ρ into Kepler's formula T = 2π√(R³/GM).
3
What would be the duration of the day if the Earth were to rotate with an angular speed such that bodies on the equator felt completely weightless?
Reveal Answer & Explanation
Answer:
Set g - ω²R = 0 and solve for T = 2π/ω.
4
A body weighs 63 N on the surface of the Earth. What is the gravitational force on it at an altitude equal to half the radius of the Earth?
Reveal Answer & Explanation
Answer:
Use F_h = F_0 · [R / (R + h)]² with h = R/2.
5
Why does an artificial satellite not require any fuel or engine propulsion to maintain its circular orbit around the Earth?
Reveal Answer & Explanation
Answer:
Consider the angle between gravitational force and displacement and the absence of friction in space.
Finished Studying This Chapter?
READY TO PRACTICE?

Timed CBT Practice Tests (Exam Simulator)

Put your concepts to the test with official curriculum-aligned Foundation and Advanced practice tests. Get instant accuracy scores, time metrics, and step-by-step verified explanations.

STAY UPDATED

Get the Latest Updates

New test series, syllabus updates, exam notifications and more.

Syllabus
Updates
Exam
Alerts
Study
Resources