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Orbits and the Wider Universe

Newton's law of gravitation applied to orbits

  • 3 things to know
  • A2 Unit 4 Section A

Overview

Recall questions on Newton's law of gravitation applied to orbits.

What you need to know

Answer each one before you reveal it.

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Key term

What provides the centripetal force that holds a planet in orbit around the Sun?

Key term

Write the equation obtained by setting the gravitational force equal to the centripetal force for a circular orbit.

Key term

Give the equation relating the orbital period to the speed and the radius.

Questions from this subtopic

Each one with the model answer underneath.

  1. 1

    What provides the centripetal force that holds a planet in orbit around the Sun?

    Model answer

    The gravitational attraction between the planet and the Sun.

  2. 2

    Write the equation obtained by setting the gravitational force equal to the centripetal force for a circular orbit.

    Model answer

    GMm/r² = mv²/r, where M is the central mass, m the orbiting mass, v the orbital speed and r the orbital radius.

  3. 3

    Rearrange that to give the orbital speed, and define every symbol.

    Model answer

    Cancelling m and one factor of r gives v = √(GM/r), where v is in m s⁻¹, G the gravitational constant, M the central mass in kilograms and r the orbital radius in metres.

  4. 4

    Why does the mass of the orbiting body not affect its orbital speed?

    Model answer

    It appears on both sides of the equation and cancels, so every object at the same radius must travel at the same speed.

  5. 5

    How does orbital speed change as the orbital radius increases?

    Model answer

    It falls in proportion to one over the square root of the radius, so a more distant planet moves more slowly.

  6. 6

    Calculate the orbital speed of a satellite 7.2 × 10⁶ m from the Earth's centre, taking M as 6.0 × 10²⁴ kg.

    Model answer

    v = √(GM/r) = √(6.67 × 10⁻¹¹ × 6.0 × 10²⁴ ÷ 7.2 × 10⁶) = √(5.56 × 10⁷), which is 7.5 × 10³ m s⁻¹.

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