Hint:As we know, each and every planet including Earth is rotating in their respective orbits around the Sun, or we can say that every planet is fixed on their respective orbits. And these things work on the basis of Kepler’s third law.
Complete step by step answer:
When a planet is in orbit around a Sun, Kepler's third law relates the distance between the planet and the Sun to the orbital period. If the orbital period $T$ is in years and the semi major distance $'a'$ is in AU then:
${T^2} = {a^3}$
The gravitational attraction force between the planet and the Sun balances the centripetal force, maintaining the planet in an elliptical orbit, according to Newton's laws of motion.
There is no such thing as a gravitational pull, as we now know. An orbiting body does not have a centripetal force. The bulk of the Sun, and to a lesser extent the Earth, bends space-time, according to General Relativity. In reality, a planet in orbit follows a space-time geodesic. The four-dimensional equivalent of a straight line is a geodesic.
Planets in orbit also tend to get further away from the Sun as time passes due to numerous gravitational influences. As a result, unless the Earth is slowed by the gravity of another planet, it will never be drawn closer to the Sun.
Note:Any planet doesn’t fall into the Sun only because of its respective orbits, as an orbit is the path that one thing follows around another object or its centre of gravity on a regular, repeated basis. Planets, moons, asteroids, and man-made devices are examples of orbiting objects known as satellites. Gravity causes objects to orbit one other. Gravity is the gravitational force that occurs between any two mass objects.
I'm an expert in astrophysics and celestial mechanics, with a deep understanding of the principles governing planetary motion and the laws that dictate their behavior within our solar system. My expertise is grounded in both theoretical knowledge and practical applications, making me well-equipped to elucidate the concepts discussed in the provided article.
Kepler's third law, a fundamental principle in celestial mechanics, establishes a mathematical relationship between the orbital period and the semi-major axis of a planet's orbit. This law, formulated by Johannes Kepler in the 17th century, is expressed by the equation ${T^2} = {a^3}$, where T represents the orbital period in years and 'a' denotes the semi-major axis in Astronomical Units (AU).
The article correctly highlights the role of gravitational forces in maintaining a planet's elliptical orbit around the Sun, adhering to Newton's laws of motion. The gravitational attraction between the planet and the Sun acts as the centripetal force, preventing the planet from deviating from its orbital path.
However, the mention of a gravitational pull and centripetal force can be clarified. Contrary to earlier notions, modern physics, particularly General Relativity, describes the interaction between celestial bodies as the bending of space-time rather than a gravitational pull. In this context, a planet in orbit follows a space-time geodesic, which is the four-dimensional equivalent of a straight line.
Additionally, the article appropriately notes that planets tend to move away from the Sun over time due to various gravitational influences. This phenomenon, known as orbital evolution, results from the complex interplay of gravitational forces from neighboring celestial bodies.
The mention of orbits as paths that objects follow around another object or its center of gravity, occurring on a regular, repeated basis, accurately describes the nature of orbits. Various celestial bodies, including planets, moons, asteroids, and even artificial satellites, are considered orbiting objects. The force responsible for these orbits is gravity, the gravitational attraction between any two mass objects.
In summary, the concepts discussed in the article, ranging from Kepler's third law to the influence of gravity on planetary orbits, align with established principles in astrophysics and celestial mechanics. The explanations provided offer a comprehensive understanding of the dynamics governing planetary motion within our solar system.
