Physics - A Course on Gravitation from Beginner to Advanced.

The lecture shows gravitational potential energy is negative, with zero at infinity and Earth's surface as the reference, and that energy increases as distance grows.

Examine gravitational interactions and weight through the universal law, gravitational constant, and Newton's second law, illustrated with sugar bags, people, and Earth.

Derive the first cosmic velocity by equating gravity to centripetal force for a circular orbit around Earth. This speed is about 7.9 km/s at the surface and decreases with altitude.

Derive geostationary orbit radius using Kepler's third law, linking a 24-hour orbital period to altitude, gravity, centripetal force, and angular velocity for communication satellites.

Compute the second cosmic velocity required to escape Earth, using conservation of energy to relate kinetic and potential energy, and note Sun's influence on the escape path.

Explore earth orbits—LEO, MEO, and GEO—defined by altitude, and learn how orbital velocity and period depend on distance, with higher orbits offering fewer satellites but greater signal delay.

Explore how acceleration creates non-inertial frames in a lift, producing fictitious forces opposite to acceleration. The lecture explains overload, under load, and weightlessness as gravity and inertia interact.

Examine how Earth's rotation drives radial acceleration and centrifugal force, shaping the apparent weight of objects. Relate angular velocity and latitude to gravity and the distance from the rotation axis.

Discover how centrifugal force from Earth's rotation lowers gravity toward the equator, making objects weigh less, with gravity strongest at the poles and a 0.3 percent latitude difference.

Explore how gravity and centrifugal force from Earth's rotation shape weight on the surface. Learn why the Earth bulges at the equator and why gravity varies from pole to pole.

Explore how Earth's rotation creates a non inertial frame where gravity is opposed by centrifugal force, yielding gravity at the poles (9.83 m/s^2) and at the equator (9.78 m/s^2).

Explore how gravity shapes planetary atmospheres and drives tides, explaining moon and sun gravity, centrifugal effects, and tides during new moon and full moon alignments.

Explore gravity inside and outside planets via universal gravitation and dynamics, noting Earth's surface value around 9.8 m/s^2. Outside, gravity follows inverse square; inside, it scales linearly with radius.

Explore how gravitational and electrostatic field intensities are illustrated by sun-like field lines, showing how field strength varies with distance and source mass or charge.

Explore gravitational and electrostatic fields through inverse-square laws, mass and charge sources, and constants G and k, noting electric forces far exceed gravitational forces.

Compare the gravitational and electrostatic forces between two electrons using Coulomb's law and Newton's law of gravitation, showing the electrostatic force is about 10^42 times stronger and independent of distance.

Explore near-surface motion under gravity, neglecting air resistance, including freefall and vertical, horizontal, and diagonal projections, with energy conservation yielding maximum height, range, and a parabolic trajectory.