Kepler's three laws of planetary motion were a stunning development in human intellectual history. This new approach facilitated predictions of celestial phenomena to unprecedented levels of accuracy, and the realization that these orbits reflected an underlying universal physical law whose validity extended from the firmament of the Earth to the remotest cosmos marked the birth of modern science.
This second edition is a concise, self-contained treatment of Kepler/Newton planetary orbits at the level of an advanced undergraduate physics student. New to this edition are elements such as a detailed derivation of Newton's shell-point equivalency theorem, a revised derivation of the polar equation for an ellipse, Kepler's Third Law for non-inverse-square central potentials, a chapter on transfer and rendezvous orbits, and an expanded treatment of methods of calculating the average distance between the Sun and a planet.
This course text starts with fundamental concepts such as position, velocity and acceleration and pairs them with Newton's gravitational law to show how elliptical orbits and Kepler's law result, while also setting up general expressions for exploring relationships between distances, angles and times for such orbits. The approach is student-friendly, featuring brief sections, clear notation and diagrams, and mathematics that undergraduates will be comfortable with, accompanied by numerous exercises.
This second edition is a concise, self-contained treatment of Kepler/Newton planetary orbits at the level of an advanced undergraduate physics student. New to this edition are elements such as a detailed derivation of Newton's shell-point equivalency theorem, a revised derivation of the polar equation for an ellipse, Kepler's Third Law for non-inverse-square central potentials, a chapter on transfer and rendezvous orbits, and an expanded treatment of methods of calculating the average distance between the Sun and a planet.
This course text starts with fundamental concepts such as position, velocity and acceleration and pairs them with Newton's gravitational law to show how elliptical orbits and Kepler's law result, while also setting up general expressions for exploring relationships between distances, angles and times for such orbits. The approach is student-friendly, featuring brief sections, clear notation and diagrams, and mathematics that undergraduates will be comfortable with, accompanied by numerous exercises.
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