Formula: P2=ka3 where: P = period of the orbit, measured in units of time. a = average distance of the object, measured in units of distance….Formula: F = G M1M2/R2 where:

Kepler’s Third law can be used to determine the orbital radius of the planet if the mass of the orbiting star is known (R3=T2−Mstar/Msun, the radius is in AU and the period is in earth years).

Radius of the moon: 1.7 x 106 m. Orbital radius of the Moon around the Earth: 3.48 x 108 m.

1. F = force of gravity.
2. M1,M2 = masses of the objects involved.
3. R = distance between their centers of mass (usually just their centers)
4. G = a constant.

There are actually three, Kepler’s laws that is, of planetary motion: 1) every planet’s orbit is an ellipse with the Sun at a focus; 2) a line joining the Sun and a planet sweeps out equal areas in equal times; and 3) the square of a planet’s orbital period is proportional to the cube of the semi-major axis of its …

In physics, you can use orbital distance to determine how long it takes for an object to revolve around another one. For example, you can calculate how long it takes Mars to travel around the Sun, given its distance from the Sun, in astronomical units.

365 days

Caprica is in the third orbit around the Helios Alpha star and shares its orbit with the planet Gemenon. They revolve around their common barycenter, or center-of-gravity, with an orbital period of 28.2 days.

225 days

Venus has an albedo of 0.7, which means that it reflects about 70 per cent of the sunlight that falls on it. So, that’s why Venus is shining so brightly at the moment, and it makes for wonderful viewing in the evening sky.

From top to bottom: Mercury (Mariner 10), Venus (Magellan), Earth (Galileo) (and moon), Mars (Viking), and Jupiter, Saturn, Uranus and Neptune (Voyager).