If we are referring to the centre of mass of the two-body system as origin, then h and l are the angular momentum per unit mass of the orbiting body and the semi latus rectum relative to the c...If we are referring to the centre of mass of the two-body system as origin, then h and l are the angular momentum per unit mass of the orbiting body and the semi latus rectum relative to the centre of mass of the system, and M is the mass function M3/(M+m)2 of the system, M and m being the masses of Sun and planet respectively.
there is a classical set of three laws, called Kepler’s laws of planetary motion, that describe the orbits of all bodies satisfying the two previous conditions (not just planets in our solar system). ...there is a classical set of three laws, called Kepler’s laws of planetary motion, that describe the orbits of all bodies satisfying the two previous conditions (not just planets in our solar system). These descriptive laws are named for the German astronomer Johannes Kepler, who devised them after careful study (over some 20 years) of a large amount of meticulously recorded observations of planetary motion done by Tycho Brahe.
there is a classical set of three laws, called Kepler’s laws of planetary motion, that describe the orbits of all bodies satisfying the two previous conditions (not just planets in our solar system). ...there is a classical set of three laws, called Kepler’s laws of planetary motion, that describe the orbits of all bodies satisfying the two previous conditions (not just planets in our solar system). These descriptive laws are named for the German astronomer Johannes Kepler, who devised them after careful study (over some 20 years) of a large amount of meticulously recorded observations of planetary motion done by Tycho Brahe.
Kepler's second law. that argued a line joining a planet and the Sun sweeps out equal areas during equal intervals of time, can be derived from conservation of angular momentum.