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Over 1000 planets have been found orbiting other stars---exoplanets (sometimes also called extrasolar planets)---in over 760 exoplanet systems as of mid-January 2014. This section will first look at how we find exoplanets and then I will draw some preliminary conclusions based on the statistics of the orbits and masses of the exoplanets.
Detecting exoplanets around other stars is a difficult project requiring very careful observations. At first finding exoplanets might seem a simple thing to do---take pictures of stars and look for small faint things orbiting them. An exoplanet would indeed be a faint: a billion or more times fainter than a star in the visible band---the glare of the starlight would wash out the feeble light of an exoplanet. The direct imaging technique of finding exoplanets would be better accomplished in the infrared band because the exoplanet's thermal spectrum would have maximum emission in the infrared band. Also, stars produce less infrared energy than visible band energy---an exoplanet would only be ten thousand to a hundred thousand times fainter than the star. The exoplanet would still be very faint, but at least the contrast ratio is improved by many thousands of times. The direct imaging technique is able to find jovian exoplanets far from their parent stars. Thirty-two exoplanets (as of early January 2013) have been found this way.
Some of the exoplanets imaged are very young and still quite warm from their formation. Therefore, the young exoplanets are quite bright in the infrared and easier to detect. Some exoplanets have been imaged by blocking the light from the much brighter star with a device called a coronograph so that the feeble light from the exoplanet can be detected. Use of a coronograph was essential to create the first visible light (optical) image of an exoplanet: that orbiting the very bright star, Fomalhaut, shown below. The black area in the center is the coronograph, the white dot shows the location of the star, the ring is a dusty debris disk analogous to our solar system's Kuiper Belt (but much further out), the small white box shows the location of the exoplanet some 115 AU from its star, and the inset shows its motion over two years of its entire 872-year orbit. Its motion proved it was an object orbiting the star.
Astronomers have detected disks of dust and gas around young stars using sensitive infrared detectors on the largest telescopes in the world. An equivalent amount of material locked up into a single object will have a smaller total surface area than if it was broken up into many tiny particles. The disks have a lot of surface area and, therefore, can emit a lot of infrared energy. Some bright stars in our sky have dust around them: Vega, Beta Pictoris, and Fomalhaut. These are systems possibly in the beginning stages of forming planets. One disk around the star HR 4796A appears to be in between the dust disk stage and a fully-fledged planet system. The inner part of the disk has been cleared away. Presumably, the dust material has now coalesced into larger things like planets. The exoplanets would have a smaller surface area than if the material was still in tiny particles form, so the exoplanets will be much fainter. The Hubble Space Telescope has also detected disks of gas and dust around 50% of the stars still forming in the Orion Nebula. It appears that the formation of planet systems is a common process in the universe.
Another way to look for exoplanets is to notice their gravitational effect on the stars they orbit. One signature of an exoplanet would be that the star would appear to wobble about as the star and the exoplanet orbit a point situated between them, proportionally closer to the more massive star, called the center of mass. This technique is called the astrometric technique. Recall from the gravity chapter that the gravity force acting on the star and the exoplanet must be the same but the much smaller mass exoplanet will have much greater acceleration and the massive star will have a much smaller acceleration—just a "wobble".
Our Sun wobbles because of the gravity of the planets orbiting it. Most of the wobble is due to Jupiter which contains more mass than all of the other planets combined. However, the wobble is tiny! Because the Sun is over a thousand times more massive than Jupiter, the center of mass is over a thousand times closer to the Sun, or about 47,000 kilometers above the surface of the Sun (this distance is less than 7% the radius of the Sun). Despite the tiny wobble, astronomers on planets orbiting nearby stars could detect this wobble using the same technology we have here on Earth if they observed the Sun's motion very carefully over a couple of decades. The stronger the gravity between the star and exoplanet, the larger will be the wobble of the star and the easier to detect. Therefore, the astrometric technique is well-suited to finding massive jovian exoplanets close to their parent stars. Because of the distorting effect of the Earth's atmosphere, no exoplanets have been found using this technique using ground-based telescopes (at the time of writing). The now-canceled SIM Lite mission was to use this technique and the Gaia mission, scheduled to launch in October 2013, will use this technique.
Another signature of an exoplanet would be doppler shifts in the star's spectral lines as they orbit their common center of mass. The doppler shift technique (also sometimes called the radial velocity technique) has been the easiest and most prolific way to find exoplanets so far. At of the time of writing almost 500 exoplanets have been found using the doppler shift technique. Like the astrometric technique, the doppler shift technique is well-suited to finding massive jovian exoplanets close to their parent stars. However, in late 2012 astronomers were able to refine the technique enough to detect an exoplanet around Alpha Centauri B (the slightly smaller of the two stars at the center of the closest star system to us) that is just 1.13 times the mass of the Earth. It produces the smallest doppler star wobble detected so far, just 0.51 meter per second or about the speed of a baby crawling.
In another milestone of the technique, astronomers announced in late June 2013 after several years of radial velocity measurements of a nearby star Gliese 667C (just 22 light years away), the discovery of three exoplanets orbiting in the habitable zone of the star. The habitable zone is the region around a star in which an exoplanet's surface would be not too hot nor too cold for liquid water to exist on the surface. While other exoplanets have been found in the habitable zones of stars, especially by the Kepler mission discussed below, this was the largest number of exoplanets in a habitable zone so far, and for Gliese 667C, very likely the largest number of exoplanets possible in its habitable zone (so the habitable zone is said to be "dynamically packed"). In our solar system there is just one habitable planet, Earth. Mars might have been habitable if it was bigger to retain a thicker atmosphere and have plate tectonics working on it for long-term habitability. Gliese 667C is a low-mass star, smaller than our Sun and those cooler, lower mass stars are more common in the Galaxy than stars like the Sun.
The period of the star wobble is measured and then the distance (semi-major axis of the orbit) is derived from Kepler's third law. The star's velocity change is measured and then the total mass of the system is derived from Newton's Laws of Motion. We can estimate the mass of the star from its spectral type, estimate the exoplanet velocity from the star wobble period and then derive the exoplanet's mass. However, the doppler effect tells you about the motion along the line of sight only. The exoplanet orbits are undoubtedly inclined, or tipped, to our line of sight and the amount of inclination is uncertain. This introduces an uncertainty in the derived masses of the exoplanets. Usually, astronomers will quote the masses as "mass×sin(orbit inclination angle)", so the actual exoplanet masses could be higher. The star-wobble techniques can also give us the orbit eccentricity if we have observations from the entire orbit. The three exoplanets in the habitable zone of Gliese 667C have minimum masses ("M sin(i)") of 2.7 to 3.8 times the mass of the Earth, so they are called "super-Earths". Because of the uncertainty in inclination of their orbits, their masses may be up to two times larger based on computer models of what gravitationally stable planet orbits would be possible.
Astronomers cannot yet determine the diameters of most of the exoplanets so their densities, and, therefore, their composition is still unknown. A fraction of the exoplanets have been observed to move in front of their stars and cause an eclipse or dimming of the starlight. This is called a transit so this means of detecting exoplanets is called the transit technique. A transit means that the exoplanet's orbit is aligned with our line of sight (and the inclination angle is nearly 90 degrees). From the exoplanet transit, astronomers have been able to accurately measure the diameter of the exoplanet. Using the exoplanet mass from the star wobble methods, you can then determine the density. Careful observations of the spectrum of the star while the exoplanet is transiting across will enable astronomers to determine the chemical composition of the exoplanet's atmosphere using spectroscopy. In other cases, the exoplanet's spectrum is found from taking the spectrum of the star plus exoplanet, then taking the spectrum of just the star when the exoplanet is behind the star and subtracting it from the star plus exoplanet spectrum. One exoplanet, HD 189733b, has water, methane and carbon dioxide in its atmosphere but the exoplanet is much too hot and massive to support life. It was not until January 2010 that astronomers had been able to take the spectrum of an exoplanet directly---an important step in eventually being able to analyze the spectrum of a terrestrial exoplanet to see if it is supporting life on it.
Most of the transiting exoplanets discovered in the early years were first detected via the doppler shift technique, but the transit technique can be another way of searching for exoplanets around other stars. However, most planetary systems do not have their orbits so exquisitely aligned with our line of sight so a lot of stars would need to be looked at to improve the chances of finding even a few transits. One advantage of the transit technique over the star-wobble methods for exoplanet detection is that you would be able to detect terrestrial-diameter exoplanets (i.e., small exoplanets). Small exoplanets like the Earth produce too small a wobble in their parent star because of their small mass to be detected by the star-wobble methods. The COROT mission (ESA) found an exoplanet less than twice the diameter of the Earth. However, this exoplanet is so close to its star that the exoplanet's surface temperature is 1000 to 1500 deg C!
The NASA/JPL spacecraft mission called Kepler looked at about 156,000 stars simultaneously to search for Earth-sized exoplanets during a four-year period of time. The spacecraft focussed on exoplanets that could be in the stars' habitable zones. Only 0.5% of the stars are expected to have their planets orbits in the habitable zones properly aligned for detection by Kepler. A terrestrial exoplanet with mass between 0.5 to 10 Earth masses will cause its star to dim by a fractional amount of between 0.00005 to 0.0004, respectively, and the transits will last just a few hours. Each exoplanet transit must be repeatable at least two more times after the first detected transit with the same time interval between transits and depth of transit. Such repeatability of the transits would mean that something was orbiting the star and not just some chance occurrence of an unrelated object passing in front of the star. For a solar-type star with an exoplanet in the habitable zone, the exoplanet would transit the star once a year. However, this assumes that the stars are calm and steady like our Sun. The Kepler team has found that a number of the stars are a bit more active, more variable, than our Sun, so they got an extension on the mission to get more observations in order to tease out the dimmings due to transiting exoplanets from those due to the intrinsic variability of the stars themselves. The mission extension was carry the mission to the year 2016 but hardware failure of a couple of its stabilizer reaction wheels brought the observing to an end in early 2013. Although the observing is finished, the Kepler team still has many thousands of transits to sift through, so there are plenty of discoveries still to be made. The Kepler team has created some nice interactives showing how the exoplanet detection works as well as how the various planet parameters are derived.
As of late 2013, Kepler had found over 3600 planetary candidates with over 20% of the planetary systems having multiple planets. Candidate exoplanets are those that have not been verified yet through follow-up observations to make sure the star dimming is not due to another star as in an eclipsing binary system or a dead star called a white dwarf. Over a 170 exoplanets have been confirmed as of November 2013. Using the number of confirmed exoplanets from the candidate list along with the numbers of candidates that were later rejected, we now have a very good idea of how well the Kepler team's transit vetting process works in finding possible planets. Just ten percent of the exoplanet candidates turn out to be something else. That leaves 90% of the exoplanet candidates as actual exoplanets.
At least eight of the confirmed exoplanets found by Kepler are definitely rocky exoplanets with densities greater than 3 times that of water. The first rocky exoplanet discovered, called Kepler-10b, has a density of 8.8 times that of water. However, Kepler-10b orbits less than 0.017 AU from its star (Mercury orbits our Sun at 0.39 AU), so its surface temperature is over 1800 K! The oceans there would be liquid iron. Another confirmed exoplanet, Kepler-22b, is the first one from the Kepler mission known to be in its star's habitable zone. At 2.4 times the diameter of Earth, Kepler-22b is considered to be a "mini-Neptune", instead of a "super-Earth". A comparison of Kepler-22b and its star's habitable zone with our solar system is shown in the image below. The picture of Kepler-22b is an artist's imagination of what Kepler-22b might look like. Since the star Kepler-22 is slightly cooler than the Sun, its habitable zone is slightly smaller than the Sun's.
The smallest confirmed exoplanet in a star's habitable zone seen by Kepler (so far) is Kepler 62f at just 1.4 times the size of the Earth. If Kepler 62f has the same density as the Earth, it would be a little over 2.7 times the mass of the Earth. The statistics of the known densities of exoplanets plus sophisticated modeling tells us that about 75% of the exoplanets smaller than 1.5 Earth-radii are rocky worlds. Therefore, it is very likely that Kepler 62f is a rocky world composed mostly of silicates, iron, nickel, and magnesium like the Earth. One of its companions, Kepler 62e is 1.6 times the size of the Earth and it orbits at the inner edge of the habitable zone. A comparison of the Kepler 62 system's five planets with the inner four planets of our solar system is shown below. Note that the star Kepler 62 is cooler and only 20% the luminosity of the Sun so its habitable zone is significantly smaller than the Sun's habitable zone.
Another confirmed exoplanet system, Kepler 20, has five exoplanets including two exoplanets that are the size of Earth. Kepler-20e is smaller than Venus and Kepler-20f is just 3% larger than the Earth. Unfortunately, both of them orbit well inside Kepler-20's habitable zone but this discovery clearly shows that the Kepler spacecraft can detect Earth-sized exoplanets and that such exoplanets definitely exist. Yet another confirmed exoplanet system, Kepler 37, has one exoplanet just slightly larger than the Moon, a second slightly smaller than Venus, and a third that is twice the size of the Earth. Of the candidates (as of late 2013), over 600 have diameters less than 1.25 Earth's and over 100 candidates reside in their star's habitable zone and have diameters ranging from Earth-size to larger than Jupiter with one having the sought for combination of Earth size in the star's habitable zone (24 in the habitable zone have sizes from 0.9 to 2 times the diameter of the Earth).
Other statistical results from the Kepler mission as of November 2013 include: nature makes planets of a variety of sizes up to 3 Earth diameters with equal ease and has more difficulty with larger planets like Saturn or Jupiter; 22% of sun-like stars (that's 1 in 5) have a planet of 1 to 2 Earth diameters in size orbiting in the star's habitable zone; at least 70% of ordinary stars including those hotter than the Sun and the great majority cooler than the Sun have a planet of some size orbiting them; and about 50% or so of the very common cool stars have a planet between 0.5 to 1.4 Earth diameters orbiting within their habitable zone. That last statistic means that the closest Earth-size exoplanet having its orbit aligned just right with our line of sight so the exoplanet transits its star is just 29 light years away---within very easy reach of the proposed TESS mission that will look for transiting exoplanets around stars in all directions but at closer distances than the Kepler mission.
Although the Kepler team has not found the exact Earth analog of an exoplanet of identical size to the Earth orbiting a star with the same temperature as the Sun at the exact same distance as the Earth is from the Sun, it has become quite clear that there are PLENTY of small rocky-world exoplanets orbiting within the habitable zone of their star in just this one small section of the Milky Way we have searched.
The transit method can usually find just the exoplanet's diameter and the doppler shift technique must be used to determine the exoplanet's mass. In a few systems with multiple exoplanets it may be possible to find the exoplanet masses. The precision of the Kepler measurements are high enough that the Kepler team has been able to detect changes in the exoplanet periods caused by the exoplanets pulling on each other. The exoplanet mass follows from observing the amount of acceleration changes in the exoplanets' motions. This also requires the exoplanets to have closely spaced orbits. One last thing to note is that in order to even see a system with multiple transiting exoplanets at all requires the exoplanets to have very closely aligned orbits, even more closely aligned than the planets in our own solar system—there are some very flat systems out there!
Another method of exoplanet detection uses the gravitational lensing effect discussed in the Einstein's Relativity chapter. When a star passes almost in front of another more distant star as seen from the Earth (the stars are not orbiting each other), the light from the distant star can be warped and focussed toward us by the gravity of the nearer star to produce multiple images of the distant star or even a ring of light if they are aligned exactly right. This lensing effect is too small and the resolving powers of telescopes are too small to see the multiple images. The multiple images will blend together into a single blurry blob that is brighter than when the multiple images are not present (a microlens event). As the nearer star moves in front of the distant star, the nearer star's blurry blob will appear to brighten and then dim as the nearer star moves out of alignment. The microlens event for typical stars in our galaxy moving at typical speeds will last a few weeks to a few months and the amount of the brightness magnification will depend on how closely the near and distant stars are aligned with our line of sight.
The animation above shows an extemely-magnified view of two possible microlens events (what you would see if you had an optical telescope several hundred meters across in space). The brightness of the ring and the combined brightness of the two distorted images exceed the distant star's brightness when it is not lensed. This animation is adapted from a figure by Penny Sackett in a talk about the search for planetary systems using microlenses.
If the nearer star has a planetary system with an exoplanet at the right position, a smaller and briefer microlens event will happen superimposed on top of the star's microlens. By looking for brief deviations in the otherwise smooth increase, then smooth decrease of a stellar microlens event, you could detect the presence of an exoplanet. This method is called the microlens technique and is summarized in the figure below—select the image to view the full-size version in another window. The exoplanet's mass and orbit size could be determined from careful measurements of the brief deviations. The microlens event method can be used to detect jovian-mass and terrestrial-mass exoplanets near their parent stars and the parent stars are distant from the Earth. Like the transit method, a lot of stars must be monitored to pick up even a single stellar microlens event. The microlens events are due to chance alignments that are not repeatable. Sixteen exoplanets orbiting stars have been found using the microlens technique as of early January 2013.
In May 2011, two teams using the microlens technique announced the discovery of several other exoplanets that are not orbiting a star—"free floaters". The teams had observed about 50 million stars in the direction of the Milky Way's bulge every 10 to 50 minutes in 2006 and 2007 looking for those chance alignments. They found a surprisingly large number of brightenings caused by planet mass objects alone. A statistical extrapolation of the results says that the free floater planets could be almost twice as numerous as normal main sequence stars in the Galaxy!
The searches have so far focussed on stars similar to the Sun, but exoplanets have also been found around other types of stars, from those much larger and hotter than the Sun to stars much smaller and cooler than the Sun, and even two systems have exoplanets orbiting a pulsar (a type of ultra-compact, dead star discussed in the stellar evolution chapter—exoplanets found using a variation of the doppler shift technique called the timing technique). The number of systems discovered and the details about them changes so rapidly that the best place to find up-to-date information on exoplanets is on the internet. Some websites are given at the end of this chapter.
The transit and microlens techniques are not good for looking exoplanets around a particular star of interest. The star-wobble and direct imaging methods are better. However, the transit and microlens methods are useful for determining the statistics of planetary systems in our galaxy, particularly the number of star systems with terrestrial exoplanets in the habitable zones. Another possible exoplanet detection method uses the amount of lithium in a star. A comparison of stars with planets and those stars without planets shows that the stars with planets have about 1% of the lithium in the star than in stars without planets. Such a detection method could offer a much more cost-effective to search for planetary systems than the other techniques being used now.
The left figure below summarizes the orbit sizes of the 801 exoplanets with known orbit sizes as of January 2013 from the Extrasolar Planets Encyclopedia. The right figure is for the 680 other planetary systems with known eccentricities. Most of these exoplanets are Saturn-Jupiter mass or larger and most of those that transit their star have densities like Saturn-Jupiter or less. The Kepler mission has found a few smaller exoplanets so far, including those with terrestrial planet-like densities, and within several years, their number is expected to be well over a hundred. In the orbit size plot, the large exoplanets (those with mass greater than or equal to half of Jupiter's mass, "Mjup") are the blue bars and the smaller exoplanets are the red bars plotted on top so that the total number of exoplanets for a given orbit size is simply the total height of the blue plus red.
Two things to notice are how close the large exoplanets (50% Jupiter's mass or larger = blue bar) are to their stars and the large eccentricities of some of the exoplanet orbits. The large exoplanets very close to their stars (within 0.5 AU) are called "hot Jupiters" because their temperatures can get up to 1000 deg C in their cloudtops (the clouds would probably be made out of rock-dust minerals instead of the ammonia, ammonium hydrosulfide, and water clouds of the much colder Jupiter and Saturn). The hot Jupiters with low densities have atmospheres puffed out by the extreme solar heating---that inflates their diameter.
The Condensation Model outlined in the previous section predicts that large planets will only form far from the young star. Giant planets start from a core of rock and ices that were able to solidify far from the intense heat of the young star. The rock-ice cores then pull in surrounding gas by their gravity. Near the star, the temperature is too high to form the rock-ice cores.
Over a decade before the discovery of the first exoplanets, astronomers predicted as part of the Condensation Model that large gas/rock clumps would form far from a young star and spiral inward toward the star because of friction with the gas remaining in the disk around the forming star. The gas/rock clumps can also interact with each other sending one into a small orbit while the other is ejected out of the system. Such interactions may also explain the elliptical orbits we see. Some astronomers working on planet formation models are looking for ways to halt the inward spiral of the gas giant planets near the star through tidal interactions between the planet and star. Perhaps the gas giant planets we see are simply the ones that did not have time to spiral completely into the stars before the gas disk was cleared away by the strong T-Tauri winds that accompany the start of nuclear fusion. Perhaps in our solar system other giant planets had formed but did not survive or were ejected. Evidence for the ejection possibility comes from the potentially large number of free floater planets that the microlens surveys are saying must exist in the Galaxy. Recent computer simulations of the dynamical history of our solar system show that the gravity of Saturn helped prevent Jupiter from spiraling into the Sun and that their orbits may have started further out than they are now, then moved closer in than they are now, and then finally moved further out to their present distances. The simulations also show that Uranus' initial orbit might have been larger than Neptune's initial orbit and that both planets' orbits were smaller than they are now. This shuffling of the gas giant planets would also have affected the material forming the terrestrial planets and changed the distributions of various types of asteroids and comets. Observations of other star/planet formation places and other planetary systems along with more sophisticated computer simulations have confirmed various features of the Condensation Model and they have also led to modifications and extensions of the theory in the continual interaction of the observation-theory-testing error correction process of science.
The Kepler mission has provided strong evidence in favor of the inward migration idea for how the hot Jupiter systems formed. A recent study looked at over 60 hot Jupiter systems in the Kepler catalog and none of them had multiple planets while other systems with large planets further out can have multiple planets. Another study investigated Kepler-30, a non-hot Jupiter system, and were able to determine that the star's rotation is aligned with the orbits of the three planets, just like our Sun's equator is aligned with the planets in our solar system. The hot Jupiter systems usually have orbits mis-aligned with the star's rotation because of the gravity tugs from other former planets flung out by the hot Jupiter as it spiraled in. Kepler-30 is just one system so future work will need to be done on other systems to confirm or negate this conclusion.
One puzzling statistic from the Kepler mission has to do with the sizes (diameters) of the exoplanets. More than three-fourths of the planet candidates in the Kepler catalog have sizes ranging between that of the Earth and Neptune. Why does not our solar system have a planet in that size range? In that respect, our solar system's architecture seems to be an unusual one in the Galaxy. Further refinement of the Condensation Model will need to be made to explain why super-Earths/mini-Neptunes are so common and what happened in our solar system to prevent such a planet from forming or continue to exist in our solar system.
In the next few years, ground-based interferometers will be completed that can image large exoplanets. What about Earth-like planets? It is unlikely that life could arise on a gas giant planet. NASA's proposed Terrestrial Planet Finder (TPF), a space-based mission, should be able to obtain infrared or optical pictures of life-bearing planets. With TPF astronomers will also be able to analyze the spectrum of the planets to determine the composition of their atmospheres. Spectral lines from water would say that a planet has a vital ingredient for life. If oxygen, particularly ozone (a molecule of three oxygen atoms), is found in the atmosphere, then it would be very likely that life is indeed on the planet. Recall from the previous chapter that molecular oxygen quickly disappears if it is not continually replenished by the photosynthesis process of plants and algae. However, it is conceivably possible for a few non-biological processes (e.g., the runaway greenhouse effect with the photodissociation of carbon dioxide and water) to create an atmosphere rich in molecular oxygen and molecular oxygen does not produce absorption lines in the preferred infrared band that would be used in the TPF mission. Ozone does. Ozone existing along with nitrous oxide and methane in particular ratios with carbon dioxide and water, all of which produce absorption lines in the infrared, would be very strong evidence for an inhabited world.
The setup and technologies TPF will employ will be based on the experience gained from previous projects such as the Keck Interferometer, the Large Binocular Telescope Interferometer, Kepler, CoRot, and the Gaia Mission. Unfortunately, there are now no plans to develop TPF for at least the next decade.
|astrometric technique||center of mass||direct imaging technique|
|doppler shift technique||exoplanet||microlens technique|
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last updated: January 24, 2014