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Quizzes > High School Quizzes > Science

Gravitation AP Physics Practice Quiz

Review key concepts for exam success

Difficulty: Moderate
Grade: Grade 12
Study OutcomesCheat Sheet
Paper art depicting trivia for the Gravitation AP Challenge, a physics practice quiz.

Which equation correctly represents Newton's law of universal gravitation?
F = (m1 * m2) / r^2
F = G * (m1 * m2) * r^2
F = G * (m1 + m2) / r^2
F = G * (m1 * m2) / r^2
Newton's law of universal gravitation states that the gravitational force between two masses is given by F = G * (m1*m2) / r^2. This equation shows that the force is directly proportional to the product of the masses and inversely proportional to the square of the distance separating them.
What is the approximate value of gravitational acceleration at Earth's surface?
1.6 m/s^2
3.0 m/s^2
15.0 m/s^2
9.8 m/s^2
The gravitational acceleration at the Earth's surface is approximately 9.8 m/s^2. This value is derived from the gravitational force acting on objects in free-fall near Earth.
Which expression best defines gravitational potential energy near Earth's surface?
U = m v
U = G * (m1*m2)/r
U = mgh
U = ½ m v²
Gravitational potential energy near Earth's surface is given by U = mgh, where m is the mass, g is the acceleration due to gravity, and h is the height above a reference level. This formula quantifies the energy an object possesses due to its position in a gravitational field.
For an object in orbit around Earth, which force acts as the centripetal force?
Gravitational force
Electrostatic force
Frictional force
Magnetic force
In orbital motion, the gravitational force exerted by Earth provides the necessary centripetal force to keep a satellite in its curved path. Without this force, the object would continue moving in a straight line according to Newton's first law.
Which statement best distinguishes weight from mass?
Mass is an intrinsic property of matter, while weight is the force due to gravity acting on that mass.
Mass is measured in newtons and weight in kilograms.
Weight is a measure of the amount of matter, while mass varies with gravity.
Weight remains constant regardless of location while mass does not.
Mass is an inherent property of an object and does not change regardless of its location. Weight, however, is the force exerted on that mass by gravity and varies depending on the gravitational field strength.
How does the gravitational force between two masses change if the distance between them is doubled?
It doubles.
It remains unchanged.
It decreases by a factor of 4.
It decreases by a factor of 2.
According to the inverse-square law, the gravitational force is inversely proportional to the square of the distance between the two masses. When the distance is doubled, the force becomes 1/(2^2) = 1/4 of its original value.
Which statement about gravitational fields is true?
It is the mass times the gravitational force.
It is only defined for objects in free fall.
Gravitational field strength at a point is the gravitational force per unit mass.
It is the gravitational potential energy per unit mass.
The gravitational field strength is defined as the gravitational force experienced by a unit mass placed at a specific point in space. This measure allows one to understand the influence of gravity independent of the mass experiencing it.
Kepler's third law relates the orbital period of a planet to which of the following?
The average distance from the Sun (semi-major axis).
The orbital eccentricity.
The planet's mass.
The planet's speed.
Kepler's third law states that the square of a planet's orbital period is proportional to the cube of the semi-major axis of its orbit. This relationship emphasizes the dependence on distance rather than the mass or speed of the planet.
What is the primary reason satellites in low Earth orbit experience atmospheric drag?
Solar radiation pressure.
Gravitational pull from the Moon.
Residual atmospheric particles in the upper atmosphere.
Magnetic forces exerted by the Earth.
Satellites in low Earth orbit encounter trace amounts of atmospheric particles, which create a drag force. This atmospheric drag slows down the satellite over time, requiring periodic adjustments to maintain its orbit.
In a two-body system where one mass is much larger than the other (M >> m), how does the gravitational force on the smaller mass depend on the larger mass?
It is independent of the large mass.
It is proportional to the square of the large mass.
It is inversely proportional to the large mass.
It is directly proportional to the large mass.
When one mass is significantly larger than the other, the gravitational force on the smaller mass scales linearly with the larger mass. This simplifies many orbital dynamics calculations, such as those used for planets orbiting a star.
Why is the gravitational force inside a uniform spherical shell zero?
There is no mass inside the shell.
The gravitational constant is not effective inside the shell.
Due to the shell theorem, the gravitational forces cancel out at any point inside.
The forces are too weak to measure.
Newton's shell theorem demonstrates that inside a uniform spherical shell, all gravitational forces exerted by different parts of the shell cancel one another out. This cancellation results in a net gravitational force of zero at any interior point.
How is escape velocity from a celestial body derived, and what does it represent?
It is the speed required to maintain a circular orbit.
It is based on mass ratios and represents the maximum possible orbital speed.
It is derived from the inverse-square law and represents the speed at which gravitational force increases.
It is derived from energy conservation and represents the minimum speed needed to overcome gravitational pull.
Escape velocity is calculated by equating an object's kinetic energy to the gravitational potential energy needed to escape the gravitational field. This yields the minimum speed required for an object to break free without additional propulsion.
At which point in an elliptical orbit is the gravitational force on a planet strongest?
At the farthest point (apoapsis).
At the midpoint between periapsis and apoapsis.
At the closest approach (periapsis).
Everywhere equally.
In an elliptical orbit, the gravitational force is strongest at periapsis, where the distance between the planet and the star is minimal. The inverse-square nature of gravity causes the force to increase significantly as the distance decreases.
If a spacecraft transitions from a lower to a higher orbit around Earth, what happens to its gravitational potential energy and kinetic energy?
Its gravitational potential energy increases while its kinetic energy decreases.
Both potential and kinetic energies increase.
Both potential and kinetic energies decrease.
Potential energy decreases while kinetic energy increases.
When a spacecraft moves to a higher orbit, it gains gravitational potential energy due to the increased distance from Earth. At the same time, a higher orbit requires a lower orbital speed, which means that the spacecraft's kinetic energy decreases.
During a gravity assist (slingshot maneuver), how does a spacecraft gain speed?
It receives additional gravitational force that permanently increases its speed.
It loses momentum to the planet's atmosphere.
It gains speed by converting the planet's orbital momentum into its own kinetic energy.
It generates thrust using its engines.
A gravity assist maneuver uses the motion and gravitational field of a planet to alter a spacecraft's trajectory and boost its speed. Essentially, the spacecraft borrows a small amount of the planet's momentum, increasing its kinetic energy without using extra fuel.
Using conservation of energy, which expression represents the escape velocity from a planet of mass M and radius R?
vₑ = 2GM/R
vₑ = √(2GM/R)
vₑ = √(GM/2R)
vₑ = √(GM/R)
Escape velocity is derived by setting the kinetic energy equal to the gravitational potential energy required to escape the gravitational field. The resulting formula, vₑ = √(2GM/R), indicates the minimum speed needed for an object to overcome a planet's gravity without further propulsion.
How does gravitational binding energy relate to the stability of a celestial body?
It is the energy required to disperse the body's mass against gravitational attraction.
It is the measure of gravitational force at the surface.
It represents the energy produced by nuclear fusion in the body.
It is the energy lost due to friction within the body.
Gravitational binding energy quantifies the energy necessary to separate all parts of a celestial body against its own gravity. A higher binding energy signifies a more stable structure, as more energy would be required to disperse the mass.
For a non-uniform spherical mass distribution, how is the gravitational potential at a point outside the sphere generally computed?
By summing the volumes of each spherical shell.
By only considering the mass on the surface.
By ignoring the contributions of the inner layers.
By integrating the contributions of infinitesimal mass elements and often treating the mass as if concentrated at the center.
When dealing with a non-uniform mass distribution, the gravitational potential is obtained by integrating the contributions from all differential mass elements. For points outside the sphere, the integration often simplifies to treating the entire mass as if it were concentrated at the center.
In a binary star system with two stars of comparable mass, where is the system's center of mass located?
It lies approximately midway between the two stars.
It is located near the larger star.
It is positioned outside of the space between the stars.
It is at the surface of one of the stars.
For binary star systems with comparable masses, the center of mass is roughly equidistant from the two stars. This point becomes the pivot around which both stars orbit, and it is essential for analyzing their orbital dynamics.
Which phenomenon provides indirect evidence for the existence of gravitational waves?
Variations in Earth's day length.
The observed decay of the orbital period in binary pulsar systems.
The exact timing of solar eclipses.
Changes in ocean tides.
The decay in the orbital period of binary pulsars has been observed and matches predictions from General Relativity that energy is lost in the form of gravitational waves. This indirect evidence supports the existence of gravitational waves and their role in influencing orbital dynamics.
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Study Outcomes

  1. Analyze the fundamentals of gravitational force between objects.
  2. Apply Newton's law of universal gravitation in problem-solving scenarios.
  3. Evaluate the effects of gravitational interactions on orbital motion.
  4. Calculate escape velocity and gravitational potential energy.
  5. Interpret the role of gravitational principles in real-world physics applications.

Gravitation AP Physics Review Cheat Sheet

  1. Newton's Universal Law of Gravitation - This fundamental law tells us every object attracts every other with a force that depends on both masses and how far apart they are, following F = G(m₝m₂)/r². It's the backbone of everything from falling apples to orbiting planets, so mastering it feels like unlocking the secrets of the cosmos! Read more on OpenStax
  2. Gravitational Field Strength (g) - Field strength is the force you'll feel per kilogram of mass at a point in space, calculated by g = GM/r². Whether you're on the Moon or Mars, this formula helps you predict how objects speed up or float away, making physics feel like a cosmic playground. Check out Spark!.Me
  3. Gravitational Potential Energy (U) - Defined as U = -GMm/r, this energy measures the work required to bring a mass from infinity to a distance r. The negative sign means energy is released when masses come together, like a cosmic hug. Understanding U is key to fun exercises like calculating how much fuel a spacecraft needs! Explore Fiveable's guide
  4. Escape Velocity - To break free from a planet's pull, an object needs at least vescape = √(2GM/r). It's the "speed limit" where rockets punch through gravity in a single bound, roughly 11.2 km/s from Earth - definitely not a Sunday drive! This concept shows why space travel is such an epic adventure. Learn more on Fiveable
  5. Orbital Velocity - To circle a planet in a graceful orbit, you need vorbit = √(GM/r). Hitting this sweet spot gives satellites just enough sideways speed to keep them zipping around Earth without crashing or flying off to space pizza parties. It's like throwing a ball so fast it never lands! See Fiveable's notes
  6. Kepler's Third Law - This law shows that the square of an orbit's period (T²) is proportional to the cube of its semi-major axis (r³). Basically, planets farther from the Sun take longer to complete their celestial race, making the Solar System feel like a cosmic marathon! It's a beautiful blend of geometry and motion. Dive into Fiveable
  7. Gravitational Potential (V) - Potential V = -GM/r gives the energy per unit mass at a point, painting a picture of gravity wells and hills like a roller-coaster landscape. It's super handy for calculating energy shifts when you drop or launch objects in a field. Once you master V, even warp drives feel almost within reach! Spark!.Me has details
  8. Acceleration Due to Gravity at Earth's Surface - The famous g ≈ 9.8 m/s² is the acceleration any object free-falls with near Earth's crust - yes, apples and astronauts obey it alike! It's the superstar constant for countless motion problems, making it your backstage pass to Newton's universe. Knowing g by heart is like owning the key to gravity. More at Fiveable
  9. Gravitational Field of a Spherical Shell - Inside a uniform shell, gravity cancels out to zero, so you could float serenely at its center; outside, it acts as if all the mass is squished at the core with g = GM/r². This mind-bender shows how symmetry simplifies complexity and helps you tackle puzzles about planets and hollow spaceships! Check Fiveable
  10. Superposition Principle for Gravitational Fields - Gravitational fields add up vectorially, so for multiple masses you just sum each field to find the total pull at a point. This principle is your go-to tool for analyzing systems from binary stars to Saturn's rings. Once you practice it, complex gravitational landscapes become puzzle pieces instead of brick walls. Read more on Fiveable
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