Solves Kepler's equation M = E − e·sin E for the eccentric anomaly E (radians), for 0 ≤ e < 1. Newton iteration from Danby's starting value, safeguarded by bisection so it converges for any M, including eccentricities up to 0.99 and beyond.
M = E − e·sin E
Solves Kepler's equation
M = E − e·sin Efor the eccentric anomaly E (radians), for 0 ≤ e < 1. Newton iteration from Danby's starting value, safeguarded by bisection so it converges for any M, including eccentricities up to 0.99 and beyond.