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3.02 Gravity Practice Quiz
Master gravity concepts with engaging practice tests
Study Outcomes
- Analyze gravitational forces and their effects on objects.
- Apply Newton's law of universal gravitation to solve quantitative problems.
- Interpret concepts of gravitational fields and potential energy.
- Compute gravitational interactions using relevant formulas.
- Evaluate the impact of mass and distance on gravitational force.
3.02 Gravity Quiz: Exam Review Cheat Sheet
- Newton's Law of Universal Gravitation - Imagine every object in the universe whispering "pull me closer"! This law tells us that the force between two masses is F = G · (m · m₂)/r², meaning larger masses or shorter distances crank up the attraction. It's your go‑to for calculating everything from apple drops to planet orbits. Read more
- Gravitational Constant (G) - This tiny number (~6.674×10❻¹¹ N·m²/kg²) sets the "strength dial" for gravity in all your equations. Nail down G and you'll unlock the power to compute forces between any two masses in the cosmos. Read more
- Acceleration Due to Gravity (g) - Here on Earth, everything falls at about 9.8 m/s² - no matter your shoe size! Whether you're tracking a tumbling apple or plotting a cannonball's path, g is the constant that keeps free‑fall fun. Study the equations
- Gravitational Potential Energy (U) - Think of this as a "cosmic savings account" of energy an object has due to its position, calculated as U = - G · (m · m₂)/r. The deeper the negative value, the more work you'd need to pull an object away, making energy‑conservation puzzles a total blast. Explore more
- Kepler's Laws of Planetary Motion - Meet the trio that choreographs planetary dances: ellipses for orbits, equal areas in equal times, and a precise period‑distance relationship. These laws let you predict planetary positions like a cosmic choreographer. Learn more
- Gravitational Field Strength (g) - This measures the force per unit mass, g = G · M/r², showing how gravity weakens as you move away from a planet. It's essential for understanding why you weigh less atop a mountain or on a space station. Dive deeper
- Escape Velocity - The minimum speed (vₑ = √(2 · G · M/r)) needed to break free from a planet's gravitational grip without extra thrust. Master this speed and you're officially prepped for an interplanetary road trip! Discover more
- Orbital Velocity - Keep the perfect pace (vₒ = √(G · M/r)) to circle a planet in a stable orbit. Satellites and astronauts rely on this magic number to stay aloft without firing rockets constantly. Find details
- Weightlessness - Ever wonder why astronauts float? In free‑fall or orbit, there's no net force acting on you, creating that glorious zero‑gravity sensation. It's the ultimate space party trick and a cornerstone of astronaut training. Learn why
- Gravitational Potential (V) - This gives the energy per unit mass at a point, V = - G · M/r, mapping out "gravitational hills and valleys" an object must climb or dive into. Use it to chart the energy landscape of any celestial field. Check it out