SuperWASP

Wide Angle Search for Planets

Search the SuperWASP site:

HOME

NEWS HOW IT WORKS TECHNICAL WASP PLANETS PUBLICATIONS PEOPLE GALLERY

Quicklinks

Exoplanets




Artist's impression of a possible exoplanet.
(Image Courtesy of PPARC)


The search for exoplanets is one of the most exciting fields in astronomy and will perhaps one day answer the question of whether we are alone in the universe. Although searching for alien worlds dates back to ancient times the techniques needed to detect them have only recently been developed with the first exoplanet around a main sequence star being discovered in 1995. We now know of well over 1000 extrasolar planets with a large number of these known to transit their star. These transiting planets are very valuable to scientists as their size and composition can be determined. Space-based missions such as Kepler are able to detect 'Earth' like worlds which reside inside the 'Habitable zone' where liquid water can exist. It is on these worlds that we believe life may exist, however, almost all the Kepler discoveries are around stars that are too faint to follow-up spectroscopically.


Exoplanets are very difficult to detect because they don't emit any light of their own and are completely obscured by their extremely bright parent stars - normal telescope observation techniques cannot be used. This image shows Gliese 229B which is a Brown Dwarf  (a failed star slightly larger than a planet) which illustrates the problem and also demonstrates the power of space based observatories. In order to find exoplanets we use a variety of techniques to detect the effect they have on their stellar system. Below is a brief summary of the most common methods for finding extrasolar-planets:


Pulsar timing
Pulsars are neutron stars for which the magnetic and spin axes are misaligned. As pulsars rotate, flashes of radio waves are emitted like a light-house which reach the Earth at regular intervals. These radio flashes can be detected and timed. The intervals between pulses are so regular they are more accurate than an atomic clock. A planet orbiting this pulsar will cause very slight variations in the timing of these flashes which we can use to detect it. The very first exoplanet orbiting around Pulsar PSR B1257+12 was found using this technique in 1992.

Radial-velocity: (Image)
A planet orbiting a star exerts a small gravitational pull which causes the star to wobble very slightly about the system's centre of mass (barycentre). If the planet is aligned edge-on to the Earth we can observe this wobble as a 'Doppler' shift in the emitted light. As the star is pulled away from us its spectrum is shifted towards the red end and as it is pulled towards us it is shifted to the blue end. The gravitational pull from the planet is minute and so very accurate spectroscopic measurements are required.By measuring the radial velocity of a star it is possible to determine the exoplanet's orbital period but only a minimum mass (as the system's inclination is not known). It is also not possible to determine the size of these planets.

Astrometry: (Image)
This technique uses extremely precise measurements of stars' positions to detect the tiny shifts caused by orbiting planets. It is most effective for planets orbiting face-on where the positional motion is greatest - however, the measurements are very difficult to obtain.

Gravitational lensing:
According to Einstein's theory of relativity, massive foreground objects can bend the light from background objects by their gravitational pull. This bending of light causes a 'lensing' effect which magnifies the distant, background objects allowing the light-curves (and planetary transits) of distant systems to be observed. The OGLE (Optical Gravitational Lensing Experiment) group very successfully make use of this technique and have detected several planetary systems - see their website for more details.

Photometry: (Image)
This is the 'Transit' technique as used by SuperWASP. When a planet passes in front of its parent star edge-on, a decrease in the star's brightness can be detected. Periodic decreases in brightness can indicate the presence of a planet and measurements of the light-curve and spectral type of the star can indicate the size and orbital period of the planet. See the How it works section for more information. When combined with the Radial-velocity technique a large number of parameters can be accurately determined including the mass which can be used to infer the composition of the planet.

An up to date list of discovered exoplanets can be found here (Exoplanets Encyclopedia).

 

Life on other worlds?

A large number of the exoplanets found so far are known as 'Hot Jupiters' - gas giant planets similar in size to Jupiter that orbit extremely close to their parent star. They are easy to detect because of their large size and short orbital period. However, they are unsuitable for hosting life. It is thought the most likely location for life to exist is on small 'Earth-like' rocky planets within a region of the stellar system known as the 'Habitable zone' where temperatures are suitable for liquid water to form.

wasp@warwick
wasp@keele
Public Archive (US)
Public Archive (CZ)
 
 

Members Only:

Hunter Results
Variable Star Investigator
SW-S Status page

 

 

 

 


Home | News | How it works | Exoplanets | Technical | WASP planets | Publications | People | Gallery | History | Map | SW-S Status
University of Cambridge Isaac Newton Group, La Palma  Instituto de Astrofisica de Canarias University of Keele Leicester University The Open University Queens University Belfast St. Andrews University Warwick University