Classical Mechanics
Gravitational Fields: g = GM/r², Field Lines & Orbital Speed
Understanding gravitational fields means understanding why objects fall the way they do, why satellites stay in orbit, and why the…
Classical Mechanics
Classical Mechanics
Gravitational Potential Energy: GPE = mgh Formula, Derivation & Examples
Lift a book off a table, stretch a spring, or carry water up to a rooftop tank, and in each…
Classical Mechanics
Impulse & Momentum: J = FΔt = Δp Formula & Worked Examples
Impulse & momentum are two of the most important concepts in classical mechanics, and they explain everything from why airbags…
Classical Mechanics
Escape Velocity: v = √(2GM/r) Formula, Derivation & Worked Examples
Escape velocity is one of the most fascinating ideas in classical mechanics and astrophysics. It explains why a rocket needs…
Classical Mechanics
Mechanical Energy: KE + PE, Conservation & Energy Transformations
Mechanical energy is one of the first ideas that ties motion and position together into a single, usable number. Every…
Classical Mechanics
Momentum and Impulse Collisions: Conservation Laws & Examples
Momentum and impulse collisions form one of the most important topics in classical mechanics. Every time two objects crash into…
Classical Mechanics
Potential Energy: Gravitational, Elastic & Electric Forms Explained
Potential energy is one of the first ideas every physics student meets, and it stays useful all the way from…
Classical Mechanics
Net Force: Definition, Formula & Newton’s Second Law Applied
Net force is one of the most important concepts in classical mechanics. Every object you see moving, stopping, or staying…
Classical Mechanics
Pressure in Fluids: P = ρgh, Pascal’s Law & Hydraulics Explained
Pressure in fluids is one of the most practical ideas in all of physics. It explains why a dam is…
Kinematics
Terminal Velocity: Why Objects Stop Accelerating & Calculations
Terminal velocity is the constant speed an object reaches when the pulling force of gravity is fully balanced by the…