Everything including planets, moons, asteroids, and comets revolve around the sun in their orbits. Our solar system consists of eight planets. The Sun is the only star in our solar system. There are millions of stars in this universe and planets revolving around these stars. The planets revolving outside the solar system revolving around a star other than the sun is called an exoplanet. Scientists have discovered many exoplanets using various methods. These methods used to detect the planets outside the solar system are discussed in detail here.
What is an Exoplanet or Extrasolar Planet?
The term exoplanet comes from combining the words exo meaning external and the planet. The word exo and planet are combined to produce the word exoplanet meaning planets outside the solar system. Any planet outside the solar system which is revolving around stars other than the sun is called an exoplanet. The exoplanets are also called extrasolar planets. These exoplanets orbit their own stars with some being part of entire planetary systems. The exoplanets are made up of the same elements by which the planets in our solar system are made up of. Based on the composition and the structure, each exoplanet differs from the others.
The exoplanets are classified into four types. The different categories of exoplanets are as follows:
The giant or Neptune-like planets are large gaseous exoplanets like the gaseous planets in our solar system. Hot Jupiters are other gaseous exoplanets that closely orbit their stars. Since hot Jupiters are closely orbiting their respective sun, the surface temperature of these hot Jupiters is high. Super earth is another category of exoplanets. Super earth is larger than our earth but smaller than the gas giants. Super earth is terrestrial and is made up of primarily rocky or icy materials. The fourth category of exoplanets is earth analogs. As the name suggests, earth analogs are similar to earth in various ways. The similarities of the earth analogs with our earth include size, composition, and distance from the star.
Methods of Detection of Exoplanets
It is very difficult to detect the exoplanets directly. The main reason that makes the exoplanet unable to detect or identify directly is that exoplanets are very faint to detect. This is because of the brightness of the stars that exoplanets are orbiting around. There are various methods used to detect the exoplanets. Scientists use radial velocity methods to detect and study the exoplanet. Let us learn some methods used by astronomers to detect the exoplanet in detail. We will also discuss the principle behind each method.
Radial Velocity Method
Through radial velocity, an exoplanet can be identified outside the solar system. The radial velocity method measures the motion of the host star in response to the gravitational tug by their planets. The first planet discovered outside the solar system is 51 Pegasi b in 1995. The great discovery was made by Swiss astronomers Michel Mayor and Didier Queloz. They were given the Nobel prize in Physics for their discovery.
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The exoplanet and the star exert equal amounts of gravitational force according to Newton’s law of gravitation. Even though the exoplanets are small compared to the stars, the gravitational pull of the exoplanet on the star causes the star to wobble. Suppose we are observing the exoplanet orbiting the star. When the position of the exoplanet is between the star and the observer at a particular instant of its orbital motion, the exoplanet pulls the star slightly towards us. When the exoplanet is behind the star, then the exoplanet pulls the star away from us. This causes the wobbling of the star back and forth due to the gravitational tug of the exoplanet on the star. The astronomers look for the wobbling of the stars to identify the exoplanet.
The astronomers use a spectrograph and powerful telescope to identify the wobbling of the stars. The lights coming from distant stars are examined in a spectrograph. The spectrograph contains dark lines or small dark gaps due to the absorption of light by the atmosphere of the star when the light passes through it. When the star moves toward us due to the gravitational tug, these dark lines shift towards the blue region of the spectrum. When the star moves away from us due to the gravitational pull of the exoplanet, the dark lines shift towards the red end of the spectrum. Therefore, this is how astronomers check if any exoplanet is orbiting a distant star by examining the light spectrum of the star. Through the radial velocity method, astronomers can find the size and shape of the orbits of the extrasolar planet orbiting the star.
Transit Method
The transit method uses the concept of shadows to identify the exoplanet. If we are observing a star from the earth which is orbited by an exoplanet, then the exoplanet will regularly pass through the position between the observer and the star. When the position of the exoplanet is between the star and the earth or the observer from the earth, the exoplanet will block a tiny amount of light coming from the star and reaching the observer. Hence the intensity of light from the star is slightly reduced for a period of time due to the current transit of planets.
The current transit of planets and their effects is similar to the case of the solar eclipse. A solar eclipse happens when the position of the moon is in between the sun and the earth. The moon will block a certain amount of light coming from the sun from reaching the earth. Similarly, for a brief period of time, the star looks dimmer. This will help the astronomers to identify that an exoplanet is orbiting the star. If the brightness of the distant star is decreased regularly and repeatedly for a brief period of time, it could be due to the reason that the exoplanet is transiting the star. THis is the principle behind the transit method to identify the exoplanet.
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The transit method is also called transit photometry. Through this method, astronomers can measure the size of the exoplanets as well as the time period of the exoplanet orbiting around the star. Astronomers combine the radial velocity method and transit photometry to obtain accurate measurements of the mass of the exoplanets. The density of the exoplanet can also be measured which helps to identify the composition of the exoplanets. The spectroscopy studies of the transit exoplanets help to identify the gases such as hydrogen, sodium, and methane in the upper atmosphere of giants. In 1999, the exoplanet HD 209458b was identified using transit photometry. The exoplanets orbiting close to the stars are identified easily using the transit photometry method.
Gravitational Microlensing Method
Through gravitational microlensing, exoplanets are identified by astronomers. When one celestial body passes in front of another celestial body from our point of view, The close objects’ gravity can bend and magnify the light of a more distant object. This causes the distant object to appear brighter than normal for a short period of time. This is called gravitational microlensing. This gravitational microlensing is a form of gravitational lensing. Gravitational lensing is a physical phenomenon that occurs when a massive body bends the light coming from the source with respect to the observer. A gravitational lens bends the light by the gravity of the massive body. If the bending of light due to bodies like stars, planets or blackholes, then it is called microlensing.
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If one star passes in fron
t of another distant star, the distant star will temporarily appear brighter for a short period of time. The brightness of the distant star returns to normal once the closer star passes it. But if the star that is passing by is accompanied by an exoplanet, then the brightness of the distant star increases temporarily for the second time as the planet passes in front of it. Therefore astronomers can identify the presence of an exoplanet by observing the distant star’s brightness to intensify twice.
Astrometry Method
Astrometry is the science of precisely measuring the position of an object in the sky. As we have discussed earlier, when an exoplanet is orbiting the star, the exoplanet will exert a gravitational pull on the star which causes the star to slightly move toward the observer on the earth as well as away from the observer depending on the position of the exoplanet. This causes the star to wobble due to the gravitational pull of the exoplanet. So, there is a small relative movement of the star with respect to other stars. This movement with a periodic rhythm can be observed using a powerful telescope. Thereby, astronomers can identify the presence of exoplanets orbiting the star.
Direct Imaging Method
Taking a picture of an exoplanet is the most difficult way because of the reason that exoplanets are outshined by the bright stars. The presence of the exoplanet’s faint glow is very very difficult to detect in the bright lights from the stars. In spite of this, astronomers use this technique to discover any exoplanets out there. Astronomers use a black mask called a coronagraph to cover up the star and most of the light coming from the star. If the planet is nearby to the star and is not covered by the coronagraph, then a powerful telescope might be able to detect the reflected light from the exoplanet. This is how the direct imaging technique works.
Exoplanets or extrasolar planets are planets outside the solar system which are orbiting a star other than the sun. Due to the faint glow of these exoplanets in the presence of bright stars, exoplanets are very difficult to identify. Therefore astronomers use different methods to identify the presence of exoplanets. There are five different methods astronomers use to detect and study exoplanets.
The radial velocity method is the most successful method so far to detect the exoplanet. Astronomers can measure the mass of the exoplanets accurately by combining the radial velocity method and the transit photometry method. There are many exoplanets similar to our earth. The study about exoplanets helps us to find out if there is any possibility of planets having extraterrestrial life outside the solar system.