Exoplanets (AQA A Level Physics): Revision Note

Exam code: 7408

Katie M

Written by: Katie M

Reviewed by: Tim

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Exoplanets

  • An exoplanet is:

A planet found outside our Solar System, in orbit around another star

  • Exoplanets are difficult to detect directly because:

    • light from the host star is much brighter than the reflected light from the planet

    • they subtend extremely small angles compared to the resolution of telescopes

  • Astronomers must use indirect detection techniques to observe exoplanets, such as:

    • the transit method

    • the radial velocity method

The transit method

  • When a planet passes in front of a star (as seen from Earth), some of the light from the star is obscured

  • Therefore, the total amount of light reaching the Earth is reduced

  • By measuring the apparent magnitude, or intensity of light received from the star over time, a light curve can be obtained

Light curve using the transit method

Transit light curve showing brightness against time. A planet crosses its star at positions 1, 2 and 3, producing a dip. The diagram states that dip depth indicates planet size and dip length indicates orbital period.
The transit method reveals both the size of the exoplanet and its orbital period
  • The dip in brightness can be used to determine the size of the planet

  • The duration of the dip can be used to determine the orbital period of the planet

  • Some of the limitations of this technique are:

    • the accuracy can be reduced if the Earth, planet and star are not aligned in the same plane

    • only planets with a short orbital period can be detected

The radial velocity method

  • As a planet orbits its host star, they both orbit around a common centre of mass

  • During the orbit, the star will move slightly towards, or away from the Earth as the planet moves to different positions in the orbit

    • The line spectrum of the star will show blueshift when it moves towards the Earth, then redshift when it moves away

Doppler shift of an exoplanet

Diagram and graph showing a star and planet orbiting their common centre of mass, producing blueshift towards Earth and redshift away. Radial velocity varies as a sine wave with peaks between minus 75 to plus 75 metres per second over 0–3 years, repeating every 2 years.
How to determine the orbital period of an exoplanet using the radial velocity method
  • This causes very small, but measurable, periodic shifts in the wavelength of the light received from the star

    • The time period of the planet’s orbit is equal to the time period of the Doppler shift

  • The main limitation of this technique is that:

    • low-mass, or Earth-like, planets do not cause as much 'wobble' as high-mass planets since they have a greater gravitational pull on the star

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Katie M

Author: Katie M

Expertise: Curriculum Expert

Katie has always been passionate about the sciences, and completed a degree in Astrophysics at Sheffield University. She decided that she wanted to inspire other young people, so moved to Bristol to complete a PGCE in Secondary Science. She particularly loves creating fun and absorbing materials to help students achieve their exam potential.

Tim

Reviewer: Tim

Expertise: Content Creator

Timothy graduated with a first class degree in Mathematics and Physics from the University of Warwick. After working as a postgraduate researcher, Timothy has worked as a content creator for various online revision platforms, creating physics resources for a range of levels and exam boards.