Physics In Flux. (Physics Blog)

  In previous blogs, I discussed Kepler's first  and second laws of planetary motion. In this blog, I will be discussing Kepler's third law of planetary motion. Statement:  "The ratio of the square of the orbital period of objects to the cube of the semi-major axis is the same for all objects orbiting the same prime celestial body. Kepler's 3rd Law of Planatery Motion T 1 2 /R 1 3 = T 2 2 /R 2 3 = T 3 2 /R 3 3    or vice versa R 1 3 /T 1 2 = R 2 3 /T 2 2 = R 3 3 /T 3 2  Different Elements of Ellipse For example, if you take the sun as being a prime celestial body orbited by objects that are planets like Mercury, Venus, Earth, and Mars. Planets Average distance from the Sun during a complete revolution (In Astronomical Unit ) Time Taken for a complete revolution (In Earth days) Mercury 0.387 87.969 Venus 0.723 244.700 Earth 1 365.256

Kepler's Second Law, The Law of Equal Areas: Kepler's second law of planetary motion states that "a line joining a planet and the Sun sweeps out equal areas in equal time intervals". This means that the planet moves faster when it is closer to the Sun and slower when it is farther away. To understand Kepler's second law, it is helpful to think about the concept of angular momentum. Angular momentum is the product of an object's mass, its velocity, and the distance from the object to the center of rotation. In the case of a planet orbiting the Sun, the angular momentum of the planet is constant. Kepler's second law of planetary motion. Angular momentum = Mass*Velocity*Distance from Sun to celestial body. L = MVR Now, angular momentum is constant (as angular momentum is conserved). Therefore, L and M are constant. R is a variable as the orbit is elliptical in shape (from the first law of Kepler). So, to compensate for the variable R, the velocity V of the pl

In the vast expanse of the cosmos, celestial bodies dance through the void in intricate and mesmerizing patterns. For centuries, humanity gazed upon the heavens, seeking to decipher the celestial choreography. Among those who dedicated their lives to unraveling these celestial mysteries, Johannes Kepler stands as a luminary figure. His first law of planetary motion, unveiled in the early 17th century, revolutionized our understanding of how planets move through space. At the heart of Kepler's first law lies a simple yet profound revelation, planets do not follow perfectly circular paths in their orbits around the Sun, as had been previously believed. Instead, they trace elliptical orbits. This departure from circularity opened Pandora's box of questions and insights, forever altering our understanding of the cosmos. An ellipse is a geometric shape resembling a flattened circle, characterized by two focal points rather than a single center. In the context of planetary motion, th