---
title: "Universal Gravitation and Weight"
book: "High School Physics"
subject: physics
language: en
chapter: 4
exercises: 15
source: https://one-course.com/books/physics/2/en/chapter/4-universal-gravitation-and-weight
---

# Chapter 4 — Universal Gravitation and Weight

Drop an apple: it falls. The Moon, sixty Earth radii up, never seems to. Newton’s great insight is that the Moon *is* falling — about 1.4 millimetres every second, exactly the amount an attraction weakening as the square of the distance predicts. One formula, with one universal constant, governs the apple, the Moon, the tides and the planets. The first volume described [gravitation](#def-g10-universal-gravitation-force) with words; this chapter measures it.

## 4.1 The law of universal gravitation

**Definition 4.1 (Gravitational force).**

Any two bodies attract each other, whatever they are made of and however far apart they sit. This attraction is the *gravitational force*, and the phenomenon is *gravitation*. It needs no contact, no rope and no medium, and it is *mutual*: each body pulls the other.

**Theorem 4.2 (Law of universal gravitation).**

Two bodies of masses $m_1$ and $m_2$ (in $\mathrm{kg}$), whose centers are a distance $d$ apart (in $\mathrm{m}$), attract each other with two forces directed along the line joining the centers, each pointing toward the other body, of equal magnitude

$$
F = G\,\frac{m_1 m_2}{d^2}
\qquad \text{(in $\mathrm{N}$)},
$$

where $G$ is the same constant for every pair of bodies in the universe.

**Proof.** *Admitted at this level.* ∎

**Remark 4.3 (Where the law comes from).**

Newton distilled this law from the observed motion of the planets (Kepler’s laws); the honest deduction is carried out in the Year 1 volume. [Chapter 27](https://one-course.com/books/physics/2/en/chapter/27-satellites-and-planetary-motion#ch-g12-satellites-kepler) will already put the law to work on [satellites](#def-g10-universal-gravitation-satellite) and planets.

**Definition 4.4 (The gravitational constant).**

The constant

$$
G = 6.67 \times 10^{-11}\,\mathrm{N}\,\mathrm{m}^{2}/\mathrm{kg}^{2}
$$

is the *gravitational constant*. Its minuscule value is the reason gravity between everyday objects is imperceptible: only when at least one mass is astronomical does $G m_1 m_2 / d^2$ amount to anything.

![The two forces of a gravitational pair: along the line of centers, toward the other body, with the same magnitude F = G m_1 m_2 / d2 even when the masses are wildly unequal.](https://one-course.com/images/onecourse/chapters/physics-2/g10-universal-gravitation/fig-a7b3c3c09a89.svg)

*The two forces of a gravitational pair: along the line of centers, toward the other body, with the *same* magnitude $F = G m_1 m_2 / d^2$ even when the masses are wildly unequal.*

**Remark 4.5 (Reading the formula).**

Four features deserve attention.

- *Mutual and equal.* The Earth pulls you with your [weight](#def-g10-universal-gravitation-weight) — and you pull the Earth with exactly the same force. (The Earth just responds less: it is about $10^{23}$ times heavier.)
- *Inverse square.* Doubling $d$ divides the force by $4$ ; moving ten times farther divides it by $100$ .
- *Distance between centers.* For spherical bodies — stars, planets, cannonballs — $d$ is measured center to center, not surface to surface.
- *Both masses matter.* Doubling either mass doubles the force; the formula is symmetric in $m_1$ and $m_2$ .

**Example 4.6 (Two friends).**

Two $70\,\mathrm{kg}$ friends stand with their centers $1.0\,\mathrm{m}$ apart:

$$
F = 6.67 \times 10^{-11} \times \frac{70 \times 70}{1.0^2}
\approx 3.3 \times 10^{-7}\,\mathrm{N}.
$$

Each friend’s [weight](#def-g10-universal-gravitation-weight) is about $6.9 \times 10^{2}\,\mathrm{N}$ — two *billion* times larger. Their mutual attraction is real, but hopeless to feel.

**Example 4.7 (The Earth holds the Moon).**

With $m_1 = 5.97 \times 10^{24}\,\mathrm{kg}$ (Earth), $m_2 = 7.35 \times 10^{22}\,\mathrm{kg}$ (Moon) and $d = 3.84 \times 10^{8}\,\mathrm{m}$:

$$
F = 6.67 \times 10^{-11} \times
\frac{5.97 \times 10^{24} \times 7.35 \times 10^{22}}{(3.84 \times 10^{8})^2}
\approx 2.0 \times 10^{20}\,\mathrm{N}.
$$

And the Moon pulls the Earth back with the same $2.0 \times 10^{20}\,\mathrm{N}$ — a pull the oceans answer twice a day, as the tides.

**Method 4.8 (Computing a gravitational force).**

1. Convert the masses to [kilograms](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) and the center-to-center distance to meters.
2. Apply $F = G m_1 m_2 / d^2$ .
3. Check the power of ten separately from the digits, as in [Chapter 1](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#ch-g10-orders-of-magnitude) : [gravitational forces](#def-g10-universal-gravitation-force) range from $10^{-7}$ newtons (two people a [metre](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) apart) to $10^{22}$ newtons (Sun on Earth), so a misplaced [exponent](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-scinot) is easy to catch.

## 4.2 Weight and the strength of gravity

**Definition 4.9 (Weight).**

The *weight* $\vect P$ of an object at the surface of a star (a planet, a moon, …) is the [gravitational force](#def-g10-universal-gravitation-force) the star exerts on it. It points toward the star’s center — the direction we call *vertical* — and is measured in newtons.

**Proposition 4.10 (Weight at the surface of a star).**

At the surface of a spherical star of mass $M$ and radius $R$, an object of mass $m$ has [weight](#def-g10-universal-gravitation-weight)

$$
P = m\,g,
\qquad\text{where}\qquad
g = \frac{G M}{R^2}
$$

depends only on the star, not on the object.

**Proof.** The object’s center and the star’s center are a distance $R$ apart, so the law of universal [gravitation](#def-g10-universal-gravitation-force) ([Theorem 4.2](#thm-g10-universal-gravitation-law)) gives $P = G M m / R^2 = m \times \left(G M / R^2\right)$. The bracket is the same for every object at the surface: call it $g$. ∎

**Definition 4.11 (Gravitational field strength).**

The quantity $g = G M / R^2$, in newtons per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit), is the *gravitational field strength* at the star’s surface: the star pulls on each [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) with $g$ newtons. On Earth, $g = 9.81\,\mathrm{N}/\mathrm{kg}$.

**Example 4.12 (Computing ggg).**

For the Earth ($M = 5.97 \times 10^{24}\,\mathrm{kg}$, $R = 6.37 \times 10^{6}\,\mathrm{m}$):

$$
g = \frac{6.67 \times 10^{-11} \times 5.97 \times 10^{24}}{(6.37 \times 10^{6})^2}
= \frac{3.98 \times 10^{14}}{4.06 \times 10^{13}}
\approx 9.81\,\mathrm{N}/\mathrm{kg}.
$$

For the Moon ($M = 7.35 \times 10^{22}\,\mathrm{kg}$, $R = 1.74 \times 10^{6}\,\mathrm{m}$) the same computation gives $g_{\text{Moon}} \approx 1.62\,\mathrm{N}/\mathrm{kg}$ — six times less: the Moon is far lighter, and being smaller does not make up for it. For Mars, $g_{\text{Mars}} \approx 3.73\,\mathrm{N}/\mathrm{kg}$.

![Surface gravitational field strength on four worlds: the same 1\, kg bag of sugar weighs 1.6\, N on the Moon and 25\, N on Jupiter.](https://one-course.com/images/onecourse/chapters/physics-2/g10-universal-gravitation/fig-7dc8c2270cf9.svg)

*Surface [gravitational field strength](#def-g10-universal-gravitation-fieldstrength) on four worlds: the same $1\,\mathrm{kg}$ bag of sugar weighs $1.6\,\mathrm{N}$ on the Moon and $25\,\mathrm{N}$ on Jupiter.*

![“Down” is a local notion: at every point of the globe the weight vector points toward the center O. Two antipodean walkers both stand upright — feet toward each other.](https://one-course.com/images/onecourse/chapters/physics-2/g10-universal-gravitation/fig-8c99b4890637.svg)

*“Down” is a local notion: at every point of the globe the [weight](#def-g10-universal-gravitation-weight) vector points toward the center $O$. Two antipodean walkers both stand upright — feet toward each other.*

**Remark 4.13 (Why astronauts bounce).**

An astronaut of mass $120\,\mathrm{kg}$ (body plus suit) weighs $120 \times 9.81 \approx 1180\,\mathrm{N}$ on Earth but only $120 \times 1.62 \approx 194\,\mathrm{N}$ on the Moon. Muscles trained under $1180\,\mathrm{N}$ suddenly carry a sixth of the load: hence the famous slow, bounding lunar gait. The mass — and with it the effort needed to *stop* or *turn* — is unchanged, which is why lunar astronauts fell over so often.

## 4.3 Mass or weight? The balance and the spring scale

Everyday language says a sack of flour “weighs three kilos”. Physics splits that sentence in two.

**Remark 4.14 (Mass is not weight).**

- The *mass* $m$ measures the quantity of matter, in [kilograms](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) . It is a property of the object alone: the same on Earth, on the Moon, or adrift in deep space.
- The *[weight](#def-g10-universal-gravitation-weight)* $P = mg$ is a force, in newtons, exerted *by a star* on the object. It changes from star to star with $g$ — and fades away far from every star.

Confusing them is harmless at the market and fatal in a physics problem: the [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) is not a [unit](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) of force.

**Method 4.15 (The balance and the spring scale).**

- A *beam balance* compares the object with standard masses: both pans’ [weights](#def-g10-universal-gravitation-weight) scale by the same $g$ , so the comparison measures the *mass* — same verdict on any star.
- A *spring scale* measures the force stretching its spring: it reads the *[weight](#def-g10-universal-gravitation-weight)* , in newtons, and its reading changes from star to star. To recover the mass, divide by the local field strength: $m = P/g$ .

**Example 4.16 (Flour on the Moon).**

A $3.0\,\mathrm{kg}$ sack of flour balances against $3.0\,\mathrm{kg}$ of standard masses on Earth *and* on the Moon. A spring scale, however, reads $3.0 \times 9.81 \approx 29\,\mathrm{N}$ on Earth and $3.0 \times 1.62 \approx 4.9\,\mathrm{N}$ on the Moon. A merchant selling “by the newton” on the Moon would hand out six times the flour — trade, like science, runs on mass.

## 4.4 Falling around the Earth: Newton’s cannon

Throw a stone horizontally: gravity bends its path into an arc and it lands a few meters away. Throw it faster: it lands farther. Newton’s thought experiment pushes the idea to its limit. The Earth is round, and its surface drops about $5\,\mathrm{m}$ below the horizontal for every $8\,\mathrm{km}$ traveled; a freely falling body drops $4.9\,\mathrm{m}$ in its first second ([Chapter 26](https://one-course.com/books/physics/2/en/chapter/26-free-fall-and-projectile-motion#ch-g12-projectile-motion) will establish this). So a projectile skimming the Earth at $8\,\mathrm{km}/\mathrm{s}$ falls exactly as fast as the ground curves away: it falls forever without ever landing.

**Definition 4.17 (Satellite and orbit).**

A *satellite* of a star is a body that falls around the star without ever reaching its surface; the path it repeats is its *orbit*.

![Newton’s cannon: fired faster and faster from a mountaintop, the ball lands farther and farther — until, at about 7.9\, km/ s, the ground curves away as fast as the ball falls, and it orbits.](https://one-course.com/images/onecourse/chapters/physics-2/g10-universal-gravitation/fig-43cae093a556.svg)

*Newton’s cannon: fired faster and faster from a mountaintop, the ball lands farther and farther — until, at about $7.9\,\mathrm{km}/\mathrm{s}$, the ground curves away as fast as the ball falls, and it [orbits](#def-g10-universal-gravitation-satellite).*

**Remark 4.18 (The Moon is a falling stone).**

The Moon is the Earth’s natural [satellite](#def-g10-universal-gravitation-satellite): it falls toward us by about $1.4\,\mathrm{mm}$ every second, and its sideways motion carries it around before it can come any closer ([Exercise 4.15](#exo-g10-universal-gravitation-15) lets you redo Newton’s own check of this number). The astronauts of an orbiting station are in the same free fall as their ship — that, and not any absence of gravity, is why they float. [Gravitation](#def-g10-universal-gravitation-force) shapes every trajectory, from the stone’s arc to the planet’s ellipse; the quantitative story of [orbits](#def-g10-universal-gravitation-satellite) is told in [Chapter 27](https://one-course.com/books/physics/2/en/chapter/27-satellites-and-planetary-motion#ch-g12-satellites-kepler).

**Notation 4.19 (Data card).**

Unless an exercise says otherwise, use $G = 6.67 \times 10^{-11}\,\mathrm{N}\,\mathrm{m}^{2}/\mathrm{kg}^{2}$ and:

|  | mass ($\mathrm{kg}$) | radius ($\mathrm{m}$) | $g$ ($\mathrm{N}/\mathrm{kg}$) |
| --- | --- | --- | --- |
| Earth | $5.97 \times 10^{24}$ | $6.37 \times 10^{6}$ | 9.81 |
| Moon | $7.35 \times 10^{22}$ | $1.74 \times 10^{6}$ | 1.62 |
| Mars | $6.42 \times 10^{23}$ | $3.39 \times 10^{6}$ | 3.73 |
| Sun | $1.99 \times 10^{30}$ | — | — |

Earth–Moon distance: $3.84 \times 10^{8}\,\mathrm{m}$; Earth–Sun distance: $1.496 \times 10^{11}\,\mathrm{m}$ (center to center).

## 4.5 Exercises

**Exercise 4.1 ★.**

Two $60\,\mathrm{kg}$ dance partners hold each other with their centers $0.80\,\mathrm{m}$ apart.

1. Compute their mutual gravitational attraction.
2. Compare it with the [weight](#def-g10-universal-gravitation-weight) of a $2.5\,\mathrm{mg}$ mosquito.

**Solution of Exercise 4.1.**

*1.* $F = 6.67 \times 10^{-11} \times \dfrac{60 \times 60}{0.80^2}
= \dfrac{2.40 \times 10^{-7}}{0.64} \approx 3.8 \times 10^{-7}\,\mathrm{N}$.

*2.* The mosquito’s [weight](#def-g10-universal-gravitation-weight) is $P = 2.5 \times 10^{-6} \times 9.81 \approx 2.5 \times 10^{-5}\,\mathrm{N}$ — about $65$ times *larger* than the dancers’ mutual attraction. Gravity between people is weaker than a mosquito’s [weight](#def-g10-universal-gravitation-weight).

**Exercise 4.2 ★.**

A student has a mass of $55\,\mathrm{kg}$.

1. Compute her [weight](#def-g10-universal-gravitation-weight) on Earth.
2. She travels to the Moon. What are her mass and her [weight](#def-g10-universal-gravitation-weight) there?

**Solution of Exercise 4.2.**

*1.* $P = mg = 55 \times 9.81 \approx 5.4 \times 10^{2}\,\mathrm{N}$.

*2.* Her mass is unchanged: $55\,\mathrm{kg}$ (same quantity of matter). Her [weight](#def-g10-universal-gravitation-weight) becomes $P = 55 \times 1.62 \approx 89\,\mathrm{N}$ — six times less.

**Exercise 4.3 ★.**

1. From the data card, recompute the [gravitational field strength](#def-g10-universal-gravitation-fieldstrength) at the surface of Mars.
2. A $900\,\mathrm{kg}$ rover is sent there. Compute its [weight](#def-g10-universal-gravitation-weight) on Mars and its [weight](#def-g10-universal-gravitation-weight) on Earth.

**Solution of Exercise 4.3.**

*1.* $g_{\text{Mars}} = \dfrac{G M}{R^2}
= \dfrac{6.67 \times 10^{-11} \times 6.42 \times 10^{23}}{(3.39 \times 10^{6})^2}
= \dfrac{4.28 \times 10^{13}}{1.15 \times 10^{13}} \approx 3.73\,\mathrm{N}/\mathrm{kg}$.

*2.* On Mars: $P = 900 \times 3.73 \approx 3.4 \times 10^{3}\,\mathrm{N}$. On Earth: $P = 900 \times 9.81 \approx 8.8 \times 10^{3}\,\mathrm{N}$ — the rover weighs about $2.6$ times less on Mars, with the same mass.

**Exercise 4.4 ★.**

Using the data card, compute the force exerted by the Earth on the Moon. What force does the Moon exert on the Earth?

**Solution of Exercise 4.4.**

$$
F = 6.67 \times 10^{-11} \times
\frac{5.97 \times 10^{24} \times 7.35 \times 10^{22}}{(3.84 \times 10^{8})^2}
= \frac{2.93 \times 10^{37}}{1.47 \times 10^{17}}
\approx 2.0 \times 10^{20}\,\mathrm{N}.
$$

The Moon exerts on the Earth a force of the *same* magnitude, $2.0 \times 10^{20}\,\mathrm{N}$, in the opposite direction: [gravitation](#def-g10-universal-gravitation-force) is mutual.

**Exercise 4.5 ★.**

Two bodies attract each other with a force $F_0$. What does the force become if:

1. the distance between centers is doubled;
2. the distance is halved;
3. both masses are doubled (same distance);
4. one mass is tripled *and* the distance is tripled?

**Solution of Exercise 4.5.**

*1.* Distance doubled: $d^2$ is multiplied by $4$, so $F = F_0/4$.

*2.* Distance halved: $F = 4F_0$.

*3.* Both masses doubled: $m_1 m_2$ is multiplied by $4$, so $F = 4F_0$.

*4.* Numerator $\times 3$, denominator $\times 9$: $F = F_0/3$.

**Exercise 4.6 ★★.**

Two loaded supertankers of $5.0 \times 10^{8}\,\mathrm{kg}$ each are moored with their centers $100\,\mathrm{m}$ apart.

1. Compute their mutual gravitational attraction.
2. What mass has a [weight](#def-g10-universal-gravitation-weight) equal to this force on Earth?
3. The force is surprisingly large — yet the tankers show no inclination to drift together. Compute the acceleration $a = F/m$ it gives one tanker and comment.

**Solution of Exercise 4.6.**

*1.* $F = 6.67 \times 10^{-11} \times
\dfrac{(5.0 \times 10^{8})^2}{100^2}
= 6.67 \times 10^{-11} \times \dfrac{2.5 \times 10^{17}}{1.0 \times 10^{4}}
\approx 1.7 \times 10^{3}\,\mathrm{N}$.

*2.* $m = F/g = 1667/9.81 \approx 1.7 \times 10^{2}\,\mathrm{kg}$: the two ships attract each other with the [weight](#def-g10-universal-gravitation-weight) of a large motorcycle.

*3.* $a = F/m = 1.7 \times 10^{3}/5.0 \times 10^{8} \approx
3.3 \times 10^{-6}\,\mathrm{m}/\mathrm{s}^{2}$. Even unopposed, the tankers would take about five days to pick up walking pace; in practice, water resistance and moorings swamp the attraction completely.

**Exercise 4.7 ★★.**

A lunar shop sells a $3.0\,\mathrm{kg}$ bag of rice.

1. What do a beam balance and a spring scale indicate for this bag on Earth? On the Moon?
2. A customer pays for “ $3.0\,\mathrm{kg}$ ”. Which instrument guarantees a fair deal on any world, and why?

**Solution of Exercise 4.7.**

*1.* The beam balance indicates $3.0\,\mathrm{kg}$ on both worlds: the bag and the standard masses see their [weights](#def-g10-universal-gravitation-weight) divided by the same factor, so the comparison is unchanged. The spring scale reads the [weight](#def-g10-universal-gravitation-weight): $3.0 \times 9.81 \approx 29\,\mathrm{N}$ on Earth, $3.0 \times 1.62 \approx 4.9\,\mathrm{N}$ on the Moon.

*2.* The balance: it measures mass, which is what the customer is buying. A spring scale calibrated in “[kilograms](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit)” on Earth would read $4.9/9.81 \approx 0.50\,\mathrm{kg}$ for the same bag on the Moon — the shopkeeper would give away six bags for the price of one.

**Exercise 4.8 ★★.**

The International Space Station flies at an altitude of $400\,\mathrm{km}$.

1. Compute the Earth’s [gravitational field strength](#def-g10-universal-gravitation-fieldstrength) at that altitude. (Careful: what is the distance to the Earth’s *center* ?)
2. Express it as a percentage of the surface value.
3. The astronauts on board float. Reconcile this with your answer.

**Solution of Exercise 4.8.**

*1.* Distance to the center: $d = R + h = 6.37 \times 10^{6} + 4.0 \times 10^{5} = 6.77 \times 10^{6}\,\mathrm{m}$. Then $g = \dfrac{6.67 \times 10^{-11} \times 5.97 \times 10^{24}}{(6.77 \times 10^{6})^2}
= \dfrac{3.98 \times 10^{14}}{4.58 \times 10^{13}} \approx 8.69\,\mathrm{N}/\mathrm{kg}$.

*2.* $8.69/9.81 \approx 89\%$ of the surface value.

*3.* Gravity is nearly full strength up there: the astronauts float because the station and everything in it are *falling together* around the Earth (free fall), not because gravity has vanished.

**Exercise 4.9 ★★.**

At the surface of Venus, $g = 8.87\,\mathrm{N}/\mathrm{kg}$, and the planet’s radius is $6.05 \times 10^{6}\,\mathrm{m}$. Deduce the mass of Venus and compare it with the Earth’s.

**Solution of Exercise 4.9.**

From $g = GM/R^2$,

$$
M = \frac{g R^2}{G}
= \frac{8.87 \times (6.05 \times 10^{6})^2}{6.67 \times 10^{-11}}
= \frac{3.25 \times 10^{14}}{6.67 \times 10^{-11}}
\approx 4.87 \times 10^{24}\,\mathrm{kg},
$$

about $0.8$ times the Earth’s mass — Venus is nearly the Earth’s twin in size and mass.

**Exercise 4.10 ★★.**

1. Compute the force exerted by the Sun on $1.0\,\mathrm{kg}$ of sea water, then the force exerted by the Moon on the same [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) .
2. The Sun pulls harder — by what factor?
3. Yet the Moon dominates the tides. The tide is driven not by the pull itself but by the *difference* between the pulls on the near and far sides of the Earth. Explain, without computing, why the nearby Moon can beat the distant Sun on that criterion.

**Solution of Exercise 4.10.**

*1.* Sun: $F = \dfrac{6.67 \times 10^{-11} \times 1.99 \times 10^{30}}{(1.496 \times 10^{11})^2}
\approx 5.9 \times 10^{-3}\,\mathrm{N}$. Moon: $F = \dfrac{6.67 \times 10^{-11} \times 7.35 \times 10^{22}}{(3.84 \times 10^{8})^2}
\approx 3.3 \times 10^{-5}\,\mathrm{N}$.

*2.* The Sun pulls about $5.9 \times 10^{-3}/3.3 \times 10^{-5} \approx 180$ times harder.

*3.* The Earth’s diameter is a much larger *fraction* of the Earth–Moon distance ($\approx 3\%$) than of the Earth–Sun distance ($\approx 0.01\%$), so the Moon’s pull changes far more from the near side to the far side of the globe. Tides feed on that difference — and there the Moon wins.

**Exercise 4.11 ★★.**

1. A planet has twice the Earth’s mass and twice its radius. Express its surface field strength in terms of the Earth’s $g$ , then in $\mathrm{N}/\mathrm{kg}$ .
2. What radius would a planet of the Earth’s mass need for its surface field strength to be $2g$ ?

**Solution of Exercise 4.11.**

*1.* $g' = \dfrac{G (2M)}{(2R)^2} = \dfrac{2}{4}\,\dfrac{GM}{R^2}
= \dfrac{g}{2} \approx 4.9\,\mathrm{N}/\mathrm{kg}$: the doubled radius wins over the doubled mass.

*2.* We need $\dfrac{GM}{R'^2} = 2\,\dfrac{GM}{R^2}$, so $R'^2 = R^2/2$ and $R' = R/\sqrt{2} \approx 4.5 \times 10^{6}\,\mathrm{m}$ — about $4500\,\mathrm{km}$.

**Exercise 4.12 ★★★.**

Somewhere on the Earth–Moon line, the two pulls on a space probe cancel. Let $x$ be the distance from the Earth’s center to that point and $D$ the Earth–Moon distance.

1. Show that at that point $\left(\dfrac{x}{D - x}\right)^{2}  = \dfrac{M_{\text{Earth}}}{M_{\text{Moon}}}$ .
2. Deduce $x$ . What fraction of the trip to the Moon is that?

**Solution of Exercise 4.12.**

*1.* Equal pulls per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit): $\dfrac{G M_{\text{Earth}}}{x^2} = \dfrac{G M_{\text{Moon}}}{(D-x)^2}$. Cross-multiplying and dividing by $G$: $\left(\dfrac{x}{D-x}\right)^2 = \dfrac{M_{\text{Earth}}}{M_{\text{Moon}}}$.

*2.* $\dfrac{x}{D-x}
= \sqrt{\dfrac{5.97 \times 10^{24}}{7.35 \times 10^{22}}} = \sqrt{81.2} \approx
9.0$, so $x = 9.0\,(D - x)$, i.e. $x = \dfrac{9.0}{10.0}\,D
\approx 0.90 \times 3.84 \times 10^{8} \approx 3.5 \times 10^{8}\,\mathrm{m}$. The balance point sits $90\%$ of the way to the Moon: the Earth’s pull dominates almost the whole trip.

**Exercise 4.13 ★★★.**

Newton’s cannon, with numbers. A projectile skims the Earth horizontally at speed $v$.

1. After $x = 8.0\,\mathrm{km}$ of horizontal travel, the spherical Earth has “dropped away” by a height $h$ satisfying $(R + h)^2 = R^2 + x^2$ . Using $(R + h)^2 \approx R^2 + 2Rh$ for small $h$ , show that $h \approx x^2 / (2R)$ and compute $h$ .
2. A freely falling body drops $4.9\,\mathrm{m}$ in its first second. Compare with $h$ and deduce the speed at which the projectile never lands.
3. Compute the duration of one full [orbit](#def-g10-universal-gravitation-satellite) at that speed, skimming the surface.

**Solution of Exercise 4.13.**

*1.* Expanding: $R^2 + 2Rh + h^2 = R^2 + x^2$; since $h$ is tiny compared with $R$, drop $h^2$: $2Rh \approx x^2$, so $h \approx \dfrac{x^2}{2R}
= \dfrac{(8.0 \times 10^{3})^2}{2 \times 6.37 \times 10^{6}}
= \dfrac{6.4 \times 10^{7}}{1.27 \times 10^{7}} \approx 5.0\,\mathrm{m}$.

*2.* In one second the projectile falls $4.9\,\mathrm{m}$ — almost exactly the $5.0\,\mathrm{m}$ the ground drops away over $8.0\,\mathrm{km}$. So at $v \approx 8.0\,\mathrm{km}/\mathrm{s}$ the fall never catches the ground: the projectile [orbits](#def-g10-universal-gravitation-satellite).

*3.* $T = \dfrac{2\pi R}{v}
= \dfrac{2\pi \times 6.37 \times 10^{6}}{8.0 \times 10^{3}}
\approx 5.0 \times 10^{3}\,\mathrm{s} \approx 83\,\mathrm{min}$ — close to the roughly $90\,\mathrm{min}$ of real [low-orbit](#def-g10-universal-gravitation-satellite) [satellites](#def-g10-universal-gravitation-satellite), which fly a little higher.

**Exercise 4.14 ★★★.**

A neutron star packs $M = 2.8 \times 10^{30}\,\mathrm{kg}$ (1.4 times the Sun’s mass) into a radius of $12\,\mathrm{km}$.

1. Compute the [gravitational field strength](#def-g10-universal-gravitation-fieldstrength) at its surface.
2. What would a $70\,\mathrm{kg}$ human weigh there? Compare with their [weight](#def-g10-universal-gravitation-weight) on Earth.
3. What is the [weight](#def-g10-universal-gravitation-weight) , there, of a $1.0\,\mathrm{mg}$ grain of sand? What mass has that [weight](#def-g10-universal-gravitation-weight) on Earth?

**Solution of Exercise 4.14.**

*1.* $g = \dfrac{6.67 \times 10^{-11} \times 2.8 \times 10^{30}}
{(1.2 \times 10^{4})^2} = \dfrac{1.87 \times 10^{20}}{1.44 \times 10^{8}}
\approx 1.3 \times 10^{12}\,\mathrm{N}/\mathrm{kg}.$

*2.* $P = 70 \times 1.3 \times 10^{12} \approx 9.1 \times 10^{13}\,\mathrm{N}$, versus $6.9 \times 10^{2}\,\mathrm{N}$ on Earth: about $1.3 \times 10^{11}$ times more. No structure made of atoms survives standing there.

*3.* $P = 1.0 \times 10^{-6} \times 1.3 \times 10^{12} \approx
1.3 \times 10^{6}\,\mathrm{N}$. On Earth that is the [weight](#def-g10-universal-gravitation-weight) of $m = 1.3 \times 10^{6}/9.81 \approx 1.3 \times 10^{5}\,\mathrm{kg}$ — a grain of sand weighing as much as a hundred-tonne locomotive.

**Exercise 4.15 ★★★.**

Newton’s Moon test (1666). The Moon’s [orbit](#def-g10-universal-gravitation-satellite) radius is about $60$ Earth radii.

1. By what factor is the Earth’s pull per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) weaker at the Moon than at the Earth’s surface, if gravity follows the inverse square?
2. Near the surface, a falling body drops $4.9\,\mathrm{m}$ in its first second. How far should the Moon fall toward the Earth each second?
3. Check against the [orbit](#def-g10-universal-gravitation-satellite) : the Moon covers its circle of radius $d = 3.84 \times 10^{8}\,\mathrm{m}$ in $T = 27.3$ days. Compute its speed $v$ , the distance $x$ it covers in one second, then the fall $h \approx x^2/(2d)$ (as in [Exercise 4.13](#exo-g10-universal-gravitation-13) ).
4. Compare the answers of questions 2 and 3, and state what Newton concluded.

**Solution of Exercise 4.15.**

*1.* The distance is $60$ times larger, so the pull per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) is $60^2 = 3600$ times weaker.

*2.* The fall in one second scales the same way: $4.9/3600 \approx 1.4 \times 10^{-3}\,\mathrm{m}$ — about $1.4\,\mathrm{mm}$.

*3.* $T = 27.3 \times 86\,400\,\mathrm{s} = 2.36 \times 10^{6}\,\mathrm{s}$, so $v = \dfrac{2\pi \times 3.84 \times 10^{8}}{2.36 \times 10^{6}} \approx
1.02 \times 10^{3}\,\mathrm{m}/\mathrm{s}$, and $x = 1.02 \times 10^{3}\,\mathrm{m}$ in one second. The fall is $h \approx \dfrac{x^2}{2d}
= \dfrac{(1.02 \times 10^{3})^2}{2 \times 3.84 \times 10^{8}}
\approx 1.4 \times 10^{-3}\,\mathrm{m}$.

*4.* The two numbers agree: the Moon falls toward the Earth each second exactly as much as inverse-square gravity, calibrated on a falling apple, predicts. Newton concluded that the force holding the Moon *is* the force that drops the apple — gravity is universal.

## 4.6 Problem: Weighing the Earth

**Problem 4.1.**

Weekend problem — from two lead spheres in a shed to the mass of the Earth and then of the Sun: what one small constant, measured once, is worth

In 1798 Henry Cavendish suspended a light rod carrying two small lead spheres from a thin wire, brought two big lead spheres close, and measured the almost nonexistent twist of the wire. The newspapers said he had *weighed the Earth* — and they were right: once $G$ is known, the Earth’s own $g$ and radius hand over its mass, and the Earth’s yearly [orbit](#def-g10-universal-gravitation-satellite) hands over the Sun’s. This problem retraces the whole chain. Use the data card throughout.

**Part I — The feeblest force.**

1. The Eiffel Tower’s iron has a mass of about $7.3 \times 10^{6}\,\mathrm{kg}$ . A $55\,\mathrm{kg}$ tourist stands $100\,\mathrm{m}$ from its center of mass. Compute the tower’s pull on the tourist.
2. Compare it with the [weight](#def-g10-universal-gravitation-weight) of a $1.0\,\mathrm{mg}$ grain of sand.
3. Proportionality drill: what happens to a [gravitational force](#def-g10-universal-gravitation-force) if (a) the distance is multiplied by $10$ ; (b) both masses are multiplied by $1000$ ; (c) both masses *and* the distance are multiplied by $1000$ ?
4. Compute the Earth’s pull on a $1.00\,\mathrm{kg}$ object at its surface, from $M$ , $R$ and $G$ . What everyday name and symbol does this number carry?
5. Gravity is by far the feeblest interaction you have met — and yet it runs the universe. Explain in one or two sentences why the Earth’s pull on you dominates your neighbor’s.

**Part II — Cavendish’s balance.** In the torsion balance, a big sphere of mass $m_1 = 158\,\mathrm{kg}$ attracts a small one of mass $m_2 = 0.73\,\mathrm{kg}$; their centers are $d = 0.23\,\mathrm{m}$ apart.

6. With the modern value of $G$ , compute the force between the two spheres.
7. Compute the [weight](#def-g10-universal-gravitation-weight) of the small sphere and the ratio of the two forces. Why did Cavendish need a torsion wire rather than any ordinary scale?
8. Cavendish’s measured twist corresponds (in modern [units](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) ) to $F = 1.47 \times 10^{-7}\,\mathrm{N}$ . Deduce his value of $G$ and compare it with today’s.
9. With $G = 6.67 \times 10^{-11}\,\mathrm{N}\,\mathrm{m}^{2}/\mathrm{kg}^{2}$ , $g = 9.81\,\mathrm{N}/\mathrm{kg}$ and $R = 6.37 \times 10^{6}\,\mathrm{m}$ , deduce the mass of the Earth. (This is the step the newspapers celebrated.)
10. Deduce the Earth’s average density $\rho = M / V$ , with $V = \frac43 \pi R^3$ . Surface rocks have densities around $2.7 \times 10^{3}\,\mathrm{kg}/\mathrm{m}^{3}$ : what does the comparison reveal about the deep interior?

**Part III — Other worlds.**

11. From the data card, recompute the Moon’s surface field strength.
12. On Earth, a good push-off lifts your center of mass by $0.50\,\mathrm{m}$ . For the same push-off, the height reached is inversely proportional to $g$ (as the energy chapter, [Chapter 9](https://one-course.com/books/physics/2/en/chapter/9-energy-forms-and-conservation#ch-g10-energy-conservation) , will justify). How high does the same jump carry you on the Moon?
13. Mercury: $M = 3.30 \times 10^{23}\,\mathrm{kg}$ , $R = 2.44 \times 10^{6}\,\mathrm{m}$ . Compute its surface field strength and compare with Mars. Mercury is much smaller than Mars — how can the two values be so close?
14. At what altitude above the Earth’s surface has the field strength dropped to half its surface value?
15. At what distance from the Earth’s center does the Earth’s pull per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) fall to the Moon’s surface value, $1.62\,\mathrm{N}/\mathrm{kg}$ ? Express it in Earth radii.

**Part IV — Weighing the Sun.** The Earth travels a near-circular [orbit](#def-g10-universal-gravitation-satellite) of radius $d = 1.496 \times 10^{11}\,\mathrm{m}$ in one year, $T = 3.156 \times 10^{7}\,\mathrm{s}$. Take as given (it is proved in [Chapter 27](https://one-course.com/books/physics/2/en/chapter/27-satellites-and-planetary-motion#ch-g12-satellites-kepler)) that a body on a circular path of radius $d$ at speed $v$ needs a pull of $v^2/d$ newtons per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) toward the center.

16. Compute the Earth’s orbital speed $v$ .
17. Deduce the pull per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) that the Sun exerts on the Earth.
18. That pull is also $G M_{\text{Sun}} / d^2$ . Deduce the mass of the Sun.
19. How many Earths is that? Compare $M_{\text{Sun}}$ with $M_{\text{Earth}}$ .
20. Finale. Cavendish’s spheres, the Earth, the Sun: one constant $G$ served for all three. State in one sentence what the word *universal* in “universal [gravitation](#def-g10-universal-gravitation-force) ” bought us in this problem.

**Solution of Problem 4.1.**

**1.** $F = 6.67 \times 10^{-11} \times
\dfrac{7.3 \times 10^{6} \times 55}{100^2} \approx 2.7 \times 10^{-6}\,\mathrm{N}$.

**2.** The sand grain weighs $1.0 \times 10^{-6} \times 9.81 \approx 9.8 \times 10^{-6}\,\mathrm{N}$: the whole Eiffel Tower pulls the tourist about $3.7$ times *less* than the [weight](#def-g10-universal-gravitation-weight) of a grain of sand.

**3.** (a) Distance $\times 10$: force divided by $100$. (b) Both masses $\times 1000$: force multiplied by $10^6$. (c) Masses $\times 1000$ and distance $\times 1000$: $10^6 / 10^6$ — the force is unchanged.

**4.** $F = \dfrac{6.67 \times 10^{-11} \times 5.97 \times 10^{24} \times
1.00}{(6.37 \times 10^{6})^2} \approx 9.81\,\mathrm{N}$: the [weight](#def-g10-universal-gravitation-weight) of one [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) — this is exactly the field strength $g = 9.81\,\mathrm{N}/\mathrm{kg}$.

**5.** Gravity is feeble per [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) but only ever *attracts*, so the pulls of all $5.97 \times 10^{24}$ [kilograms](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) of Earth add up in the same direction — and an astronomical mass beats a neighborly one by twenty-two powers of ten.

**6.** $F = 6.67 \times 10^{-11} \times \dfrac{158 \times 0.73}{0.23^2}
= 6.67 \times 10^{-11} \times \dfrac{115.3}{0.0529}
\approx 1.5 \times 10^{-7}\,\mathrm{N}$.

**7.** The small sphere weighs $0.73 \times 9.81 \approx 7.2\,\mathrm{N}$ — about $5 \times 10^{7}$ times the attraction to be detected. No pan scale resolves one part in fifty million; a fine torsion wire, which twists visibly under nanonewton-scale torques, can.

**8.** $G = \dfrac{F d^2}{m_1 m_2}
= \dfrac{1.47 \times 10^{-7} \times 0.0529}{115.3}
\approx 6.74 \times 10^{-11}\,\mathrm{N}\,\mathrm{m}^{2}/\mathrm{kg}^{2}$ — within about $1\%$ of the modern $6.67 \times 10^{-11}$, from a wooden shed in 1798.

**9.** From $g = G M / R^2$:

$$
M = \frac{g R^2}{G}
= \frac{9.81 \times (6.37 \times 10^{6})^2}{6.67 \times 10^{-11}}
\approx 5.97 \times 10^{24}\,\mathrm{kg}.
$$

Six million billion billion [kilograms](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit): the Earth, weighed.

**10.** $V = \frac43 \pi R^3 = \frac43 \pi
(6.37 \times 10^{6})^3 \approx 1.08 \times 10^{21}\,\mathrm{m}^{3}$, so $\rho = 5.97 \times 10^{24}/1.08 \times 10^{21} \approx 5.5 \times 10^{3}\,\mathrm{kg}/\mathrm{m}^{3}$ — twice the density of surface rock. The interior must hide something much denser than granite: the Earth has a heavy (iron) core.

**11.** $g_{\text{Moon}} = \dfrac{6.67 \times 10^{-11} \times
7.35 \times 10^{22}}{(1.74 \times 10^{6})^2} = \dfrac{4.90 \times 10^{12}}
{3.03 \times 10^{12}} \approx 1.62\,\mathrm{N}/\mathrm{kg}$.

**12.** Height $\propto 1/g$: $h = 0.50 \times \dfrac{9.81}{1.62} \approx 3.0\,\mathrm{m}$ — a standing jump over a basketball hoop, in slow motion.

**13.** $g_{\text{Mercury}} = \dfrac{6.67 \times 10^{-11} \times
3.30 \times 10^{23}}{(2.44 \times 10^{6})^2} = \dfrac{2.20 \times 10^{13}}
{5.95 \times 10^{12}} \approx 3.70\,\mathrm{N}/\mathrm{kg}$ — almost exactly Mars’s $3.73\,\mathrm{N}/\mathrm{kg}$. Mercury has less mass, but its smaller radius (a smaller $R^2$ below) compensates: it is a much denser world.

**14.** Half the field strength requires $(R + h)^2 = 2 R^2$, so $R + h = R\sqrt{2}$ and $h = (\sqrt{2} - 1) R \approx 0.414 \times 6.37 \times 10^{6}
\approx 2.6 \times 10^{6}\,\mathrm{m}$ — about $2600\,\mathrm{km}$ up.

**15.** $\dfrac{G M_{\text{Earth}}}{d^2} = 1.62$ gives $d = \sqrt{\dfrac{6.67 \times 10^{-11} \times 5.97 \times 10^{24}}{1.62}}
= \sqrt{2.46 \times 10^{14}} \approx 1.57 \times 10^{7}\,\mathrm{m} \approx 2.5$ Earth radii. From only one and a half radii above the ground, the Earth pulls no harder than the Moon’s surface does.

**16.** $v = \dfrac{2\pi d}{T}
= \dfrac{2\pi \times 1.496 \times 10^{11}}{3.156 \times 10^{7}}
\approx 2.98 \times 10^{4}\,\mathrm{m}/\mathrm{s}$ — thirty kilometers every second.

**17.** $\dfrac{v^2}{d} = \dfrac{(2.98 \times 10^{4})^2}{1.496 \times 10^{11}}
\approx 5.9 \times 10^{-3}\,\mathrm{N}/\mathrm{kg}$: the Sun pulls each [kilogram](https://one-course.com/books/physics/2/en/chapter/1-orders-of-magnitude-measuring-the-universe#def-g10-orders-of-magnitude-unit) of the Earth with about six millinewtons.

**18.** $\dfrac{G M_{\text{Sun}}}{d^2} = \dfrac{v^2}{d}$ gives

$$
M_{\text{Sun}} = \frac{v^2 d}{G}
= \frac{8.87 \times 10^{8} \times 1.496 \times 10^{11}}{6.67 \times 10^{-11}}
\approx 1.99 \times 10^{30}\,\mathrm{kg}.
$$

**19.** $\dfrac{1.99 \times 10^{30}}{5.97 \times 10^{24}} \approx
3.3 \times 10^{5}$: the Sun is a third of a million Earths.

**20.** Because the same $G$ governs every pair of masses, measuring it once between two lead spheres in a shed let us put on the scales first the planet under our feet, then the star we [orbit](#def-g10-universal-gravitation-satellite) — that is what *universal* is worth.