...distance in terms of which, in Kepler's Third Law, nV = k!(l + m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant, k, may be exactly 0.01720209895 when the unit of time is the ephemeris day. . In...

...distance in terms of which, in Kepler's Third Law, nV = k'(l + m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant, k, may be exactly 0.01720209895 when the unit of time is the ephemeris day. In astronomical...

...terms of which, in the Kepler Third Law, л2о3 = ¿2(1 + m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant k may be exactly 0.01720209895 when the unit of time is the ephemeris day. In astronomical...

...in terms of which, in the Kepler Third Law, n2as = &l(l + m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant /; may be exactly 0.01720209895 when the unit of time is the ephemeris day. In astronomical...

...distance in terms of which, in Kepler's Third Law, n'a1 = k'(l + m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant, k, may be exactly 0.01720209895 when the unit of time is the ephemeris day. In astronomical...

...in terms of which, in the Kepler Third Law, n2o3 = A;2(l+m), the semimajor axis a of an elliptical orbit must be expressed in order that the numerical value of the Gaussian constant k may be exactly 0.01720209895 when the unit of time is the ephemeris day. atmosphere....