Lines point towards the center of mass, density indicates field strength.

Planet (M), Satellite (m), Orbital Radius (r), Gravitational Force (F).

1. $F = G \frac{m_1 m_2}{r^2}$ (Gravitational Force), 2. $F = m_1 a$ (Newton's Second Law), 3. $m_1 a = G \frac{m_1 m_2}{r^2}$ (Equate forces), 4. $a = G \frac{m_2}{r^2}$ (Solve for acceleration), 5. $g = G \frac{M}{r^2}$ (Replace $a$ with $g$, $m_2$ with $M$).

1. Identify the masses $m_1$ and $m_2$. 2. Measure the distance $r$ between their centers. 3. Use the formula $F = G \frac{m_1 m_2}{r^2}$ with $G = 6.67 \times 10^{-11} Nm^2/kg^2$.

1. Identify the planet's mass $M$ and radius $r$. 2. Use the formula $g = G \frac{M}{r^2}$ with $G = 6.67 \times 10^{-11} Nm^2/kg^2$.

1. Equate gravitational force to centripetal force: $G \frac{Mm}{r^2} = m\frac{v^2}{r}$. 2. Solve for $v$: $v = \sqrt{\frac{GM}{r}}$ where $r$ is the orbital radius.

1. Identify initial conditions (velocity, height). 2. Use kinematic equations with $a = g = 9.8 m/s^2$. 3. Solve for unknowns (time, final velocity, distance).

The direction of the gravitational force; field lines point towards the center of the mass creating the field.

The strength of the gravitational field; closer lines indicate a stronger field.

The gravitational force between the planet and the satellite.

The planet with greater mass would have more dense and closely spaced gravitational field lines.

Radially inward, converging towards the center of the sphere.