Question

Explain Kepler's Law Of Planetary Motion.

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Answer 1

Answer:-

✧ The law which govern's the motion of planets are called Kepler's laws of planetary motion.

The three laws of Kepler's Law Of Panetary motion are :-

❶ Laws Of Orbit : According to this law every planet moves around the sun in an elliptical path with sun at one of the foci.

❷ Laws Of Area : According to this law, the line joining the sun to the planet sweeps out equal areas in equal interval of time. it means aerial velocity of the planet around the sun is constant.

❸ Laws Of Period : This law states that the square of period of revolution of any planet around the sun is directly proportional to the cube of the semi-major axis of the orbit.

Answer 2

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• A 16th century Astronomer "Johannnes Kepler established three laws which govern the motion of planets around the sun.These laws are known as "Law of planetary motion." These laws also describe the motion of satellites around the planet.
• First law of planetary motion : "The planets move in elliptical orbit around the sun ,with the sun at the one of the two foci of the elliptical orbit". This means that path of a planet around the sun is an ellipse or oval - shaped.An elliptical path has two foci or focus and sun is at one of the two foci of the path.
• Second law of planetary motion : "Each planet revolves around the sun in such a way that the line joining the planet to the sun sweeps over equal areas in equal intervals of time." As we know data planet moves around the sun in an elliptical orbit with the sun at one of its focus.Now,the line joining the planet and the sun sweeps over equal areas in equal intervals of time it means that a planet move faster when it is closer to the sun and move slowly when it is farther than the sun.
• Third law of planetary motion : "The cube of the mean distance of a planet from the sun is directly proportional to the square of time it takes to move around the sun" .It can be expressed as :

$\normalsize\:\:\:\qquad\twoheadrightarrow\mathsf{ r^{3} \: \propto \: T^{2} }$

$\normalsize\:\:\:\qquad\twoheadrightarrow\mathsf{ r^{3} \: = constant \: \times \: T^{2} }$