1. Identify the masses of the two objects ($m_1$ and $m_2$). 2. Determine the distance ($r$) between the centers of the two objects. 3. Use the formula: F = G rac{m_1 m_2}{r^2}, where G is the gravitational constant ($6.674 × 10^{-11} Nm^2/kg^2$).

1. Identify the mass ($M$) of the object being orbited. 2. Determine the radius ($r$) of the orbit. 3. Use the formula: $v = \sqrt{\frac{GM}{r}}$, where G is the gravitational constant ($6.674 × 10^{-11} Nm^2/kg^2$).

1. Identify the mass ($M$) of the celestial body. 2. Determine the radius ($r$) of the celestial body. 3. Use the formula: $v_e = \sqrt{\frac{2GM}{r}}$, where G is the gravitational constant ($6.674 × 10^{-11} Nm^2/kg^2$).

1. Determine the radius ($r$) of the orbit. 2. Identify the mass ($M$) of the object being orbited. 3. Use the formula: $T = 2\pi \sqrt{\frac{r^3}{GM}}$, where G is the gravitational constant ($6.674 × 10^{-11} Nm^2/kg^2$).

1: $m_1$, 2: $m_2$, 3: r, 4: F

1: Central Body, 2: Orbiting Object, 3: Orbital Path

The attractive force between objects with mass.

The path an object takes around another object in space.

An oval-shaped orbit, not a perfect circle.

The speed needed to maintain a stable orbit.

The minimum speed to break free from a celestial body's gravity.

The time for one complete orbit.