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University Physics Volume 1

13.2 Gravitation Near Earth's Surface

University Physics Volume 113.2 Gravitation Near Earth's Surface
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  1. Preface
  2. Unit 1. Mechanics
    1. 1 Units and Measurement
      1. Introduction
      2. 1.1 The Scope and Scale of Physics
      3. 1.2 Units and Standards
      4. 1.3 Unit Conversion
      5. 1.4 Dimensional Analysis
      6. 1.5 Estimates and Fermi Calculations
      7. 1.6 Significant Figures
      8. 1.7 Solving Problems in Physics
      9. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    2. 2 Vectors
      1. Introduction
      2. 2.1 Scalars and Vectors
      3. 2.2 Coordinate Systems and Components of a Vector
      4. 2.3 Algebra of Vectors
      5. 2.4 Products of Vectors
      6. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    3. 3 Motion Along a Straight Line
      1. Introduction
      2. 3.1 Position, Displacement, and Average Velocity
      3. 3.2 Instantaneous Velocity and Speed
      4. 3.3 Average and Instantaneous Acceleration
      5. 3.4 Motion with Constant Acceleration
      6. 3.5 Free Fall
      7. 3.6 Finding Velocity and Displacement from Acceleration
      8. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    4. 4 Motion in Two and Three Dimensions
      1. Introduction
      2. 4.1 Displacement and Velocity Vectors
      3. 4.2 Acceleration Vector
      4. 4.3 Projectile Motion
      5. 4.4 Uniform Circular Motion
      6. 4.5 Relative Motion in One and Two Dimensions
      7. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    5. 5 Newton's Laws of Motion
      1. Introduction
      2. 5.1 Forces
      3. 5.2 Newton's First Law
      4. 5.3 Newton's Second Law
      5. 5.4 Mass and Weight
      6. 5.5 Newton’s Third Law
      7. 5.6 Common Forces
      8. 5.7 Drawing Free-Body Diagrams
      9. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    6. 6 Applications of Newton's Laws
      1. Introduction
      2. 6.1 Solving Problems with Newton’s Laws
      3. 6.2 Friction
      4. 6.3 Centripetal Force
      5. 6.4 Drag Force and Terminal Speed
      6. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    7. 7 Work and Kinetic Energy
      1. Introduction
      2. 7.1 Work
      3. 7.2 Kinetic Energy
      4. 7.3 Work-Energy Theorem
      5. 7.4 Power
      6. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    8. 8 Potential Energy and Conservation of Energy
      1. Introduction
      2. 8.1 Potential Energy of a System
      3. 8.2 Conservative and Non-Conservative Forces
      4. 8.3 Conservation of Energy
      5. 8.4 Potential Energy Diagrams and Stability
      6. 8.5 Sources of Energy
      7. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
    9. 9 Linear Momentum and Collisions
      1. Introduction
      2. 9.1 Linear Momentum
      3. 9.2 Impulse and Collisions
      4. 9.3 Conservation of Linear Momentum
      5. 9.4 Types of Collisions
      6. 9.5 Collisions in Multiple Dimensions
      7. 9.6 Center of Mass
      8. 9.7 Rocket Propulsion
      9. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    10. 10 Fixed-Axis Rotation
      1. Introduction
      2. 10.1 Rotational Variables
      3. 10.2 Rotation with Constant Angular Acceleration
      4. 10.3 Relating Angular and Translational Quantities
      5. 10.4 Moment of Inertia and Rotational Kinetic Energy
      6. 10.5 Calculating Moments of Inertia
      7. 10.6 Torque
      8. 10.7 Newton’s Second Law for Rotation
      9. 10.8 Work and Power for Rotational Motion
      10. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    11. 11 Angular Momentum
      1. Introduction
      2. 11.1 Rolling Motion
      3. 11.2 Angular Momentum
      4. 11.3 Conservation of Angular Momentum
      5. 11.4 Precession of a Gyroscope
      6. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    12. 12 Static Equilibrium and Elasticity
      1. Introduction
      2. 12.1 Conditions for Static Equilibrium
      3. 12.2 Examples of Static Equilibrium
      4. 12.3 Stress, Strain, and Elastic Modulus
      5. 12.4 Elasticity and Plasticity
      6. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    13. 13 Gravitation
      1. Introduction
      2. 13.1 Newton's Law of Universal Gravitation
      3. 13.2 Gravitation Near Earth's Surface
      4. 13.3 Gravitational Potential Energy and Total Energy
      5. 13.4 Satellite Orbits and Energy
      6. 13.5 Kepler's Laws of Planetary Motion
      7. 13.6 Tidal Forces
      8. 13.7 Einstein's Theory of Gravity
      9. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    14. 14 Fluid Mechanics
      1. Introduction
      2. 14.1 Fluids, Density, and Pressure
      3. 14.2 Measuring Pressure
      4. 14.3 Pascal's Principle and Hydraulics
      5. 14.4 Archimedes’ Principle and Buoyancy
      6. 14.5 Fluid Dynamics
      7. 14.6 Bernoulli’s Equation
      8. 14.7 Viscosity and Turbulence
      9. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
  3. Unit 2. Waves and Acoustics
    1. 15 Oscillations
      1. Introduction
      2. 15.1 Simple Harmonic Motion
      3. 15.2 Energy in Simple Harmonic Motion
      4. 15.3 Comparing Simple Harmonic Motion and Circular Motion
      5. 15.4 Pendulums
      6. 15.5 Damped Oscillations
      7. 15.6 Forced Oscillations
      8. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    2. 16 Waves
      1. Introduction
      2. 16.1 Traveling Waves
      3. 16.2 Mathematics of Waves
      4. 16.3 Wave Speed on a Stretched String
      5. 16.4 Energy and Power of a Wave
      6. 16.5 Interference of Waves
      7. 16.6 Standing Waves and Resonance
      8. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
    3. 17 Sound
      1. Introduction
      2. 17.1 Sound Waves
      3. 17.2 Speed of Sound
      4. 17.3 Sound Intensity
      5. 17.4 Normal Modes of a Standing Sound Wave
      6. 17.5 Sources of Musical Sound
      7. 17.6 Beats
      8. 17.7 The Doppler Effect
      9. 17.8 Shock Waves
      10. Chapter Review
        1. Key Terms
        2. Key Equations
        3. Summary
        4. Conceptual Questions
        5. Problems
        6. Additional Problems
        7. Challenge Problems
  4. A | Units
  5. B | Conversion Factors
  6. C | Fundamental Constants
  7. D | Astronomical Data
  8. E | Mathematical Formulas
  9. F | Chemistry
  10. G | The Greek Alphabet
  11. Answer Key
    1. Chapter 1
    2. Chapter 2
    3. Chapter 3
    4. Chapter 4
    5. Chapter 5
    6. Chapter 6
    7. Chapter 7
    8. Chapter 8
    9. Chapter 9
    10. Chapter 10
    11. Chapter 11
    12. Chapter 12
    13. Chapter 13
    14. Chapter 14
    15. Chapter 15
    16. Chapter 16
    17. Chapter 17
  12. Index

Learning Objectives

By the end of this section, you will be able to:
  • Explain the connection between the constants GG and gg
  • Determine the mass of an astronomical body from free-fall acceleration at its surface
  • Describe how the value of gg varies due to location and Earth’s rotation

In this section, we observe how Newton’s law of gravitation applies at the surface of a planet and how it connects with what we learned earlier about free fall. We also examine the gravitational effects within spherical bodies.

Weight

Recall that the acceleration of a free-falling object near Earth’s surface is approximately g=9.80m/s2g=9.80m/s2. The force causing this acceleration is called the weight of the object, and from Newton’s second law, it has the value mg. This weight is present regardless of whether the object is in free fall. We now know that this force is the gravitational force between the object and Earth. If we substitute mg for the magnitude of F12F12 in Newton’s law of universal gravitation, m for m1m1, and MEME for m2m2, we obtain the scalar equation

mg=GmMEr2mg=GmMEr2

where r is the distance between the centers of mass of the object and Earth. The average radius of Earth is about 6370 km. Hence, for objects within a few kilometers of Earth’s surface, we can take r=REr=RE (Figure 13.7). The mass m of the object cancels, leaving

g=GMEr2.g=GMEr2.
(13.2)

This explains why all masses free fall with the same acceleration. We have ignored the fact that Earth also accelerates toward the falling object, but that is acceptable as long as the mass of Earth is much larger than that of the object.

This figure shows an illustration of the earth, with a building on its surface. A cut away of a quarter of the earth shows several layers. The center of the earth is labeled C M, and the radius from the center to the building is labeled R E. An enlarged view of the building and a portion of the earth is also shown. In this view, we see that the arrow labeled R E terminates in the building, slightly above the surface of the earth.
Figure 13.7 We can take the distance between the centers of mass of Earth and an object on its surface to be the radius of Earth, provided that its size is much less than the radius of Earth.

Example 13.3

Masses of Earth and Moon Have you ever wondered how we know the mass of Earth? We certainly can’t place it on a scale. The values of g and the radius of Earth were measured with reasonable accuracy centuries ago.

  1. Use the standard values of g, RERE, and Equation 13.2 to find the mass of Earth.
  2. Estimate the value of g on the Moon. Use the fact that the Moon has a radius of about 1700 km (a value of this accuracy was determined many centuries ago) and assume it has the same average density as Earth, 5500kg/m35500kg/m3.

Strategy With the known values of g and RERE, we can use Equation 13.2 to find MEME. For the Moon, we use the assumption of equal average density to determine the mass from a ratio of the volumes of Earth and the Moon.

Solution

  1. Rearranging Equation 13.2, we have
    ME=gRE2G=9.80m/s2(6.37×106m)26.67×10−11N·m2/kg2=5.95×1024kg.ME=gRE2G=9.80m/s2(6.37×106m)26.67×10−11N·m2/kg2=5.95×1024kg.
  2. The volume of a sphere is proportional to the radius cubed, so a simple ratio gives us
    MMME=RM3RE3MM=((1.7×106m)3(6.37×106m)3)(5.95×1024kg)=1.1×1023kg.MMME=RM3RE3MM=((1.7×106m)3(6.37×106m)3)(5.95×1024kg)=1.1×1023kg.

    We now use Equation 13.2.
    gM=GMMrM2=(6.67×10−11N·m2/kg2)(1.1×1023kg)(1.7×106m)2=2.5m/s2gM=GMMrM2=(6.67×10−11N·m2/kg2)(1.1×1023kg)(1.7×106m)2=2.5m/s2

Significance As soon as Cavendish determined the value of G in 1798, the mass of Earth could be calculated. (In fact, that was the ultimate purpose of Cavendish’s experiment in the first place.) The value we calculated for g of the Moon is incorrect. The average density of the Moon is actually only 3340kg/m33340kg/m3 and g=1.6m/s2g=1.6m/s2 at the surface. Newton attempted to measure the mass of the Moon by comparing the effect of the Sun on Earth’s ocean tides compared to that of the Moon. His value was a factor of two too small. The most accurate values for g and the mass of the Moon come from tracking the motion of spacecraft that have orbited the Moon. But the mass of the Moon can actually be determined accurately without going to the Moon. Earth and the Moon orbit about a common center of mass, and careful astronomical measurements can determine that location. The ratio of the Moon’s mass to Earth’s is the ratio of [the distance from the common center of mass to the Moon’s center] to [the distance from the common center of mass to Earth’s center].

Later in this chapter, we will see that the mass of other astronomical bodies also can be determined by the period of small satellites orbiting them. But until Cavendish determined the value of G, the masses of all these bodies were unknown.

Example 13.4

Gravity above Earth’s Surface What is the value of g 400 km above Earth’s surface, where the International Space Station is in orbit?

Strategy Using the value of MEME and noting the radius is r=RE+400kmr=RE+400km, we use Equation 13.2 to find g.

From Equation 13.2 we have

g=GMEr2=6.67×10−11N·m2/kg25.96×1024kg(6.37×106+400×103m)2=8.67m/s2.g=GMEr2=6.67×10−11N·m2/kg25.96×1024kg(6.37×106+400×103m)2=8.67m/s2.

Significance We often see video of astronauts in space stations, apparently weightless. But clearly, the force of gravity is acting on them. Comparing the value of g we just calculated to that on Earth (9.80m/s2)(9.80m/s2), we see that the astronauts in the International Space Station still have 88% of their weight. They only appear to be weightless because they are in free fall. We will come back to this in Satellite Orbits and Energy.

Check Your Understanding 13.2

How does your weight at the top of a tall building compare with that on the first floor? Do you think engineers need to take into account the change in the value of g when designing structural support for a very tall building?

The Gravitational Field

Equation 13.2 is a scalar equation, giving the magnitude of the gravitational acceleration as a function of the distance from the center of the mass that causes the acceleration. But we could have retained the vector form for the force of gravity in Equation 13.1, and written the acceleration in vector form as

g=GMr2r^.g=GMr2r^.

We identify the vector field represented by gg as the gravitational field caused by mass MM. We can picture the field as shown Figure 13.8. The lines are directed radially inward and are symmetrically distributed about the mass.

This figure shows a three dimensional vector graph. The x, y, z coordinate system is shown. A spherical mass M is shown at the origin and vectors are shown pointing toward it. The arrows decrease in length as their distance from the origin increases. A box, aligned with the coordinate axes, is also shown.
Figure 13.8 A three-dimensional representation of the gravitational field created by mass MM. Note that the lines are uniformly distributed in all directions. (The box has been added only to aid in visualization.)

As is true for any vector field, the direction of gg is parallel to the field lines at any point. The strength of gg at any point is inversely proportional to the line spacing. Another way to state this is that the magnitude of the field in any region is proportional to the number of lines that pass through a unit surface area, effectively a density of lines. Since the lines are equally spaced in all directions, the number of lines per unit surface area at a distance r from the mass is the total number of lines divided by the surface area of a sphere of radius r, which is proportional to r2r2. Hence, this picture perfectly represents the inverse square law, in addition to indicating the direction of the field. In the field picture, we say that a mass m interacts with the gravitational field of mass M. We will use the concept of fields to great advantage in the later chapters on electromagnetism.

Apparent Weight: Accounting for Earth’s Rotation

As we saw in Applications of Newton’s Laws, objects moving at constant speed in a circle have a centripetal acceleration directed toward the center of the circle, which means that there must be a net force directed toward the center of that circle. Since all objects on the surface of Earth move through a circle every 24 hours, there must be a net centripetal force on each object directed toward the center of that circle.

Let’s first consider an object of mass m located at the equator, suspended from a scale (Figure 13.9). The scale exerts an upward force FsFs away from Earth’s center. This is the reading on the scale, and hence it is the apparent weight of the object. The weight (mg) points toward Earth’s center. If Earth were not rotating, the acceleration would be zero and, consequently, the net force would be zero, resulting in Fs=mgFs=mg. This would be the true reading of the weight.

An illustration of the earth, rotating on its north-south axis, with masses on spring scales shown at three locations. The radius of the earth is labeled as R E, its center is labeled as O. One spring scale is above the north pole. An upward force F S N and a downward force m g are shown acting on the mass on this spring scale. A dashed line is shown from the center of the earth to the north pole. Another spring scale is shown to the right of the equator and a dashed line connects the center of the earth to the equator on the right side of the earth. The forces on the mass on this second spring scale are shown as a force F S E to the right and m g to the left. A third spring scale is shown at an angle lambda to the horizontal. A dashed line at this angle is shown from the center to the surface of the earth. The horizontal distance from the surface of the earth at this angle lambda to the vertical dashed line connecting the center to the north pole is labeled as r. The point on the dashed vertical line where r meets it is labeled P. Three forces are shown for the third mass. One force is labeled F S and points radially outward. A second force, labeled m g points radially inward. A third force, labeled F c, points horizontally to the left.
Figure 13.9 For a person standing at the equator, the centripetal acceleration (ac)(ac) is in the same direction as the force of gravity. At latitude λλ, the angle the between acac and the force of gravity is λλ and the magnitude of acac decreases with cosλcosλ.

With rotation, the sum of these forces must provide the centripetal acceleration, acac. Using Newton’s second law, we have

F=Fsmg=macwhereac=v2r.F=Fsmg=macwhereac=v2r.
(13.3)

Note that acac points in the same direction as the weight; hence, it is negative. The tangential speed v is the speed at the equator and r is RERE. We can calculate the speed simply by noting that objects on the equator travel the circumference of Earth in 24 hours. Instead, let’s use the alternative expression for acac from Motion in Two and Three Dimensions. Recall that the tangential speed is related to the angular speed (ω)(ω) by v=rωv=rω. Hence, we have ac=rω2ac=rω2. By rearranging Equation 13.3 and substituting r=REr=RE, the apparent weight at the equator is

Fs=m(gREω2).Fs=m(gREω2).

The angular speed of Earth everywhere is

ω=2πrad24hr×3600s/hr=7.27×10−5rad/s.ω=2πrad24hr×3600s/hr=7.27×10−5rad/s.

Substituting for the values or RERE and ωω, we have REω2=0.0337m/s2REω2=0.0337m/s2. This is only 0.34% of the value of gravity, so it is clearly a small correction.

Example 13.5

Zero Apparent Weight How fast would Earth need to spin for those at the equator to have zero apparent weight? How long would the length of the day be?

Strategy Using Equation 13.3, we can set the apparent weight (FsFs) to zero and determine the centripetal acceleration required. From that, we can find the speed at the equator. The length of day is the time required for one complete rotation.

Solution From Equation 13.2, we have F=Fsmg=macF=Fsmg=mac, so setting Fs=0Fs=0, we get g=acg=ac. Using the expression for acac, substituting for Earth’s radius and the standard value of gravity, we get

ac=v2r=gv=gr=(9.80m/s2)(6.37×106m)=7.91×103m/s.ac=v2r=gv=gr=(9.80m/s2)(6.37×106m)=7.91×103m/s.

The period T is the time for one complete rotation. Therefore, the tangential speed is the circumference divided by T, so we have

v=2πrTT=2πrv=2π(6.37×106m)7.91×103m/s=5.06×103s.v=2πrTT=2πrv=2π(6.37×106m)7.91×103m/s=5.06×103s.

This is about 84 minutes.

Significance We will see later in this chapter that this speed and length of day would also be the orbital speed and period of a satellite in orbit at Earth’s surface. While such an orbit would not be possible near Earth’s surface due to air resistance, it certainly is possible only a few hundred miles above Earth.

Results Away from the Equator

At the poles, ac0ac0 and Fs=mgFs=mg, just as is the case without rotation. At any other latitude λλ, the situation is more complicated. The centripetal acceleration is directed toward point P in the figure, and the radius becomes r=REcosλr=REcosλ. The vector sum of the weight and FsFs must point toward point P, hence FsFs no longer points away from the center of Earth. (The difference is small and exaggerated in the figure.) A plumb bob will always point along this deviated direction. All buildings are built aligned along this deviated direction, not along a radius through the center of Earth. For the tallest buildings, this represents a deviation of a few feet at the top.

It is also worth noting that Earth is not a perfect sphere. The interior is partially liquid, and this enhances Earth bulging at the equator due to its rotation. The radius of Earth is about 30 km greater at the equator compared to the poles. It is left as an exercise to compare the strength of gravity at the poles to that at the equator using Equation 13.2. The difference is comparable to the difference due to rotation and is in the same direction. Apparently, you really can lose “weight” by moving to the tropics.

Gravity Away from the Surface

Earlier we stated without proof that the law of gravitation applies to spherically symmetrical objects, where the mass of each body acts as if it were at the center of the body. Since Equation 13.2 is derived from Equation 13.1, it is also valid for symmetrical mass distributions, but both equations are valid only for values of rRErRE. As we saw in Example 13.4, at 400 km above Earth’s surface, where the International Space Station orbits, the value of g is 8.67m/s28.67m/s2. (We will see later that this is also the centripetal acceleration of the ISS.)

For r<REr<RE, Equation 13.1 and Equation 13.2 are not valid. However, we can determine g for these cases using a principle that comes from Gauss’s law, which is a powerful mathematical tool that we study in more detail later in the course. A consequence of Gauss’s law, applied to gravitation, is that only the mass within r contributes to the gravitational force. Also, that mass, just as before, can be considered to be located at the center. The gravitational effect of the mass outside r has zero net effect.

Two very interesting special cases occur. For a spherical planet with constant density, the mass within r is the density times the volume within r. This mass can be considered located at the center. Replacing MEME with only the mass within r, M=ρ×(volume of a sphere)M=ρ×(volume of a sphere), and RERE with r, Equation 13.2 becomes

g=GMERE2=Gρ(4/3πr3)r2=43Gρπr.g=GMERE2=Gρ(4/3πr3)r2=43Gρπr.

The value of g, and hence your weight, decreases linearly as you descend down a hole to the center of the spherical planet. At the center, you are weightless, as the mass of the planet pulls equally in all directions. Actually, Earth’s density is not constant, nor is Earth solid throughout. Figure 13.10 shows the profile of g if Earth had constant density and the more likely profile based upon estimates of density derived from seismic data.

A section of the earth is illustrated, showing several layers inside the earth. A legend indicates that the layers are, from the surface working inward, the Upper mantle in pink, lower mantle in red, outer core in orange, and inner core in tan. The upper mantle is much thinner than the lower mantle and outer core, which are approximately the same thickness, and the inner core radius is a greater than the upper mantle thickness but less than that of the outer core. Below this illustration is a graph of acceleration in m per second squared as a function of radius in 1000 k m. The vertical scale is from 0 to 12 meters per second squared and the horizontal scale is from 0 to 14 thousand kilometers. Vertical bars using the same color scheme as the illustration of the earth are shown aligned with the illustration. The inner core extends from 0 to a little over 1000 k m. The outer core extends to just under 4000 k m. The lower mantle to just under 6000 k m. The upper mantle extends to just over 6000 k m. A blue curve, labeled P R E M, starts at the origin and rises almost linearly to over 10 m per second squared at the outer edge of the outer core. The curve then decreases to under 10 at the outer edge of the upper mantle. The curve then decreases more rapidly, but with slope that is decreasing with radius. A second green curve is labeled “Constant decay” and is a straight line from the origin of the graph to the point at a radius of just over 6000 k m (the surface) and just under 10 (the value of the blue curve at the surface).
Figure 13.10 For r<REr<RE, the value of g for the case of constant density is the straight green line. The blue line from the PREM (Preliminary Reference Earth Model) is probably closer to the actual profile for g.

The second interesting case concerns living on a spherical shell planet. This scenario has been proposed in many science fiction stories. Ignoring significant engineering issues, the shell could be constructed with a desired radius and total mass, such that g at the surface is the same as Earth’s. Can you guess what happens once you descend in an elevator to the inside of the shell, where there is no mass between you and the center? What benefits would this provide for traveling great distances from one point on the sphere to another? And finally, what effect would there be if the planet was spinning?

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