Kepler's Physical AstronomyPrinceton University Press, 25. júl. 1994 - 216 síður From Hipparchus and Ptolemy in the ancient world, through Copernicus and Brahe in the sixteenth century, astronomers had used geometrical models to give a kinematic account of the movements of the sun, moon, and planets. Johannes Kepler revolutionized this most ancient of sciences by being the first to understand astronomy as a part of physics. By closely and clearly analyzing the texts of Kepler's great astronomical works, in particular the Astronomia nova of 1609, Bruce Stephenson demonstrates the importance of Kepler's physical principles--principles now known to be "incorrect"--in the creation of his first two laws of planetary motion. |
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angle aphelion approximation apsidal line area law argument Astronomia nova axis body calculations Chapter circular orbit circular sectors circumsolar coequated anomaly component computed conchoid construction Copernican Copernicus deflection delay direction distance law distance theory earth earth's orbit eccentric anomaly eccentric circle ecliptic ellipse epicycle epicyclic model Epitome equal equant center equant model equation of center equivalent error evection explain Figure geometrical heliocentric hence increments inequality Kepler Kepler's physics latitude theory libration theory libratory force longitude lunar theory Mars mathematical mean anomaly mean distances mean sun measured moon moon's moved the planet nodes optical equation oval path perihelion perpendicular physical equation physical theory planet moved planet's distance planetary mind planetary motion planetary theory position precisely problem Ptolemy quadrant radius ratio reason rotation second anomaly simple solar radius solar theory speed sphere sun's sunlight syzygies triangle true anomaly true sun variation velocity versed sine