text:
Exoplanet
From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
For the album by The Contortionist, see Exoplanet (album).
Artist's impression of how commonly planets orbit the stars in the Milky Way[1]
Discovered exoplanets each year as of 26 November 2017[2]
Size comparison of Jupiter and the exoplanet TrES-3b. TrES-3b has an orbital period of only 31 hours[3] and is classified as a Hot Jupiter for being large and close to its star, making it one of the easiest planets to detect by the transit method.
NASA histogram chart of confirmed exoplanets by distance
An exoplanet (UK: /ˈɛk.soʊˌplæn.ɪt/, US: /ˌɛk.soʊˈplæn.ɪt/)[4] or extrasolar planet is a planet outside our solar system. The first evidence of an exoplanet was noted as early as 1917, but was not recognized as such.[5] However, the first scientific detection of an exoplanet was in 1988, although it was not accepted as an exoplanet until later. The first confirmed detection occurred in 1992. As of 1 August 2018, there are 3,815 confirmed planets in 2,853 systems, with 633 systems having more than one planet.[6]
The High Accuracy Radial Velocity Planet Searcher (HARPS), since 2004) has discovered about a hundred exoplanets while the Kepler space telescope (since 2009) has found more than two thousand. Kepler has also detected a few thousand[7][8] candidate planets,[9][10] of which about 11% may be false positives.[11] In several cases, multiple planets have been observed around a star.[12] About 1 in 5 Sun-like stars[a] have an "Earth-sized"[b] planet in the habitable zone.[c] Assuming there are 200 billion stars in the Milky Way,[d] one can hypothesize that there are 11 billion potentially habitable Earth-sized planets in the Milky Way, rising to 40 billion if planets orbiting the numerous red dwarfs are included.[13]
The least massive planet known is Draugr (also known as PSR B1257+12 A or PSR B1257+12 b), which is about twice the mass of the Moon. The most massive planet listed on the NASA Exoplanet Archive is HR 2562 b,[14][15] about 30 times the mass of Jupiter, although according to some definitions of a planet, it is too massive to be a planet and may be a brown dwarf instead. There are planets that are so near to their star that they take only a few hours to orbit and there are others so far away that they take thousands of years to orbit. Some are so far out that it is difficult to tell whether they are gravitationally bound to the star. Almost all of the planets detected so far are within the Milky Way. Nonetheless, evidence suggests that extragalactic planets, exoplanets further away in galaxies beyond the local Milky Way galaxy, may exist.[16][17] The nearest exoplanet is Proxima Centauri b, located 4.2 light-years (1.3 parsecs) from Earth and orbiting Proxima Centauri, the closest star to the Sun.[18]
The discovery of exoplanets has intensified interest in the search for extraterrestrial life. There is special interest in planets that orbit in a star's habitable zone, where it is possible for liquid water, a prerequisite for life on Earth, to exist on the surface. The study of planetary habitability also considers a wide range of other factors in determining the suitability of a planet for hosting life.[19]
Besides exoplanets, there are also rogue planets, which do not orbit any star and which tend to be considered separately, especially if they are gas giants, in which case they are often counted, like WISE 0855−0714, as sub-brown dwarfs.[20] The rogue planets in the Milky Way possibly number in the billions (or more).[21][22]
Contents
1 Nomenclature
2 History of detection
2.1 Early speculations
2.2 Discredited claims
2.3 Confirmed discoveries
2.4 Candidate discoveries
3 Methodology
3.1 Detection techniques
4 Formation and evolution
5 Planet-hosting stars
6 General features
6.1 Color and brightness
6.2 Magnetic field
6.3 Plate tectonics
6.4 Volcanism
6.5 Rings
6.6 Moons
6.7 Atmospheres
6.8 Insolation pattern
7 See also
8 Notes
9 References
10 Further reading
11 External links
Nomenclature[edit]
Exoplanet HIP 65426b is the first discovered planet around star HIP 65426.[23]
Main article: Exoplanet naming convention
The convention for designating exoplanets is an extension of the system used for designating multiple-star systems as adopted by the International Astronomical Union (IAU). For exoplanets orbiting a single star, the designation is normally formed by taking the name or, more commonly, designation of its parent star and adding a lower case letter.[24] The first planet discovered in a system is given the designation "b" (the parent star is considered to be "a") and later planets are given subsequent letters. If several planets in the same system are discovered at the same time, the closest one to the star gets the next letter, followed by the other planets in order of orbital size. A provisional IAU-sanctioned standard exists to accommodate the designation of circumbinary planets. A limited number of exoplanets have IAU-sanctioned proper names. Other naming systems exist.
History of detection[edit]
For centuries scientists, philosophers, and science fiction writers suspected that extrasolar planets existed,[25] but there was no way of detecting them or of knowing their frequency or how similar they might be to the planets of the Solar System. Various detection claims made in the nineteenth century were rejected by astronomers. The first evidence of an exoplanet was noted as early as 1917, but was not recognized as such.[5] The first suspected scientific detection of an exoplanet occurred in 1988. Shortly afterwards, the first confirmed detection came in 1992, with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257+12.[26] The first confirmation of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found in a four-day orbit around the nearby star 51 Pegasi. Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method. As of February 2018, researchers at the Chandra X-ray Observatory, combined with a planet detection technique called microlensing, found evidence that there are potentially one trillion extragalactic exoplanets, stating "Some of these exoplanets are as (relatively) small as the moon, while others are as massive as Jupiter. Unlike Earth, most of the exoplanets are not tightly bound to stars, so they're actually wandering through space or loosely orbiting between stars. We can estimate that the number of planets in this [faraway] galaxy is more than a trillion."[27]
Early speculations[edit]
“ This space we declare to be infinite... In it are an infinity of worlds of the same kind as our own. ”
— Giordano Bruno (1584)[28]
In the sixteenth century the Italian philosopher Giordano Bruno, an early supporter of the Copernican theory that Earth and other planets orbit the Sun (heliocentrism), put forward the view that the fixed stars are similar to the Sun and are likewise accompanied by planets.
In the eighteenth century the same possibility was mentioned by Isaac Newton in the "General Scholium" that concludes his Principia. Making a comparison to the Sun's planets, he wrote "And if the fixed stars are the centres of similar systems, they will all be constructed according to a similar design and subject to the dominion of One."[29]
In 1952, more than 40 years before the first hot Jupiter was discovered, Otto Struve wrote that there is no compelling reason why planets could not be much closer to their parent star than is the case in the Solar System, and proposed that Doppler spectroscopy and the transit method could detect super-Jupiters in short orbits.[30]
Discredited claims[edit]
Claims of exoplanet detections have been made since the nineteenth century. Some of the earliest involve the binary star 70 Ophiuchi. In 1855 William Stephen Jacob at the East India Company's Madras Observatory reported that orbital anomalies made it "highly probable" that there was a "planetary body" in this system.[31] In the 1890s, Thomas J. J. See of the University of Chicago and the United States Naval Observatory stated that the orbital anomalies proved the existence of a dark body in the 70 Ophiuchi system with a 36-year period around one of the stars.[32] However, Forest Ray Moulton published a paper proving that a three-body system with those orbital parameters would be highly unstable.[33] During the 1950s and 1960s, Peter van de Kamp of Swarthmore College made another prominent series of detection claims, this time for planets orbiting Barnard's Star.[34] Astronomers now generally regard all the early reports of detection as erroneous.[35]
In 1991 Andrew Lyne, M. Bailes and S. L. Shemar claimed to have discovered a pulsar planet in orbit around PSR 1829-10, using pulsar timing variations.[36] The claim briefly received intense attention, but Lyne and his team soon retracted it.[37]
Confirmed discoveries[edit]
Main article: Discoveries of exoplanets
See also: List of exoplanet firsts
The three known planets of the star HR8799, as imaged by the Hale Telescope. The light from the central star was blanked out by a vector vortex coronagraph.
2MASS J044144 is a brown dwarf with a companion about 5–10 times the mass of Jupiter. It is not clear whether this companion object is a sub-brown dwarf or a planet.
As of 1 August 2018, a total of 3,815 confirmed exoplanets are listed in the Extrasolar Planets Encyclopaedia, including a few that were confirmations of controversial claims from the late 1980s.[6] The first published discovery to receive subsequent confirmation was made in 1988 by the Canadian astronomers Bruce Campbell, G. A. H. Walker, and Stephenson Yang of the University of Victoria and the University of British Columbia.[38] Although they were cautious about claiming a planetary detection, their radial-velocity observations suggested that a planet orbits the star Gamma Cephei. Partly because the observations were at the very limits of instrumental capabilities at the time, astronomers remained skeptical for several years about this and other similar observations. It was thought some of the apparent planets might instead have been brown dwarfs, objects intermediate in mass between planets and stars. In 1990 additional observations were published that supported the existence of the planet orbiting Gamma Cephei,[39] but subsequent work in 1992 again raised serious doubts.[40] Finally, in 2003, improved techniques allowed the planet's existence to be confirmed.[41]
Coronagraphic image of AB Pictoris showing a companion (bottom left), which is either a brown dwarf or a massive planet. The data was obtained on 16 March 2003 with NACO on the VLT, using a 1.4 arcsec occulting mask on top of AB Pictoris.
On 9 January 1992, radio astronomers Aleksander Wolszczan and Dale Frail announced the discovery of two planets orbiting the pulsar PSR 1257+12.[26] This discovery was confirmed, and is generally considered to be the first definitive detection of exoplanets. Follow-up observations solidified these results, and confirmation of a third planet in 1994 revived the topic in the popular press.[42] These pulsar planets are thought to have formed from the unusual remnants of the supernova that produced the pulsar, in a second round of planet formation, or else to be the remaining rocky cores of gas giants that somehow survived the supernova and then decayed into their current orbits.
On 6 October 1995, Michel Mayor and Didier Queloz of the University of Geneva announced the first definitive detection of an exoplanet orbiting a main-sequence star, namely the nearby G-type star 51 Pegasi.[43][44] This discovery, made at the Observatoire de Haute-Provence, ushered in the modern era of exoplanetary discovery. Technological advances, most notably in high-resolution spectroscopy, led to the rapid detection of many new exoplanets: astronomers could detect exoplanets indirectly by measuring their gravitational influence on the motion of their host stars. More extrasolar planets were later detected by observing the variation in a star's apparent luminosity as an orbiting planet passed in front of it.
Initially, most known exoplanets were massive planets that orbited very close to their parent stars. Astronomers were surprised by these "hot Jupiters", because theories of planetary formation had indicated that giant planets should only form at large distances from stars. But eventually more planets of other sorts were found, and it is now clear that hot Jupiters make up the minority of exoplanets. In 1999, Upsilon Andromedae became the first main-sequence star known to have multiple planets.[45] Kepler-16 contains the first discovered planet that orbits around a binary main-sequence star system.[46]
On 26 February 2014, NASA announced the discovery of 715 newly verified exoplanets around 305 stars by the Kepler Space Telescope. These exoplanets were checked using a statistical technique called "verification by multiplicity".[47][48][49] Prior to these results, most confirmed planets were gas giants comparable in size to Jupiter or larger as they are more easily detected, but the Kepler planets are mostly between the size of Neptune and the size of Earth.[47]
On 23 July 2015, NASA announced Kepler-452b, a near-Earth-size planet orbiting the habitable zone of a G2-type star.[50]
Candidate discoveries[edit]
As of June 2017, NASA's Kepler mission had identified more than 5,000 planetary candidates,[51] several of them being nearly Earth-sized and located in the habitable zone, some around Sun-like stars.[7][8][52]
Exoplanet Populations – June 2017[53][54]
Exoplanet populations
Small planets come in two sizes
Kepler habitable zone planets
Methodology[edit]
The first exoplanet was detected on 6 October 1995, and was named 51 Pegasi b.[55] When an extrasolar planet is observed to transit its parent star, astronomers are able to assess some physical properties of the planet from an interstellar distance, including planetary mass and size, which in turn provide fundamental constraints on models of their physical structure.[56] Furthermore, such events afford the opportunity to study the dynamics and chemistry of its atmosphere.[56]
Statistical surveys and individual characterization are the keys to addressing the fundamental questions in exoplanetology.[57] As of August 2016, varying techniques have been used to discover 3,502 exoplanets.[58] Documenting the properties of a large sample exoplanets at various ages, orbiting their parent stars of various types, will contribute to increased understanding —or better models— of planetary formation (accretion), geological evolution, orbit migration,[57][59] and their potential habitability.[60] Characterizing the atmospheres of extrasolar planets is the new frontier in exoplanetary science.[61]
Detection techniques[edit]
Measuring the flow of gas within a protoplanetary disc allows the detection of exoplanets.[62]
Main article: Methods of detecting exoplanets
About 97% of all the confirmed exoplanets have been discovered by indirect techniques of detection, mainly by radial velocity measurements and transit monitoring techniques.[60] The following methods have proved successful for discovering a new planet or confirming an already discovered planet:[63]
Radial velocity
Gravitational microlensing
Direct imaging
Polarimetry
Astrometry
Transit photometry
Reflection/emission modulations
Light variations due to relativistic beaming
Light variations due to ellipsoidal variations
Timing variations
Pulsar timing
Variable star timing
Transit timing variation method
Transit duration variation method
Eclipsing binary minima timing

Formation and evolution[edit]
See also: Accretion (astrophysics), Nebular hypothesis, and Planetary migration
Planets form within a few tens of millions of years of their star forming.[64][65][66] The planets of the Solar System can only be observed in their current state, but observations of different planetary systems of varying ages allows us to observe planets at different stages of evolution. Available observations range from young proto-planetary disks where planets are still forming [67] to planetary systems of over 10 Gyr old.[68] When terrestrial planets form in a gaseous protoplanetary disk,[69] they have hydrogen envelopes that cool and contract over time and, depending on the mass of the planet, some or all of the hydrogen is eventually lost to space. This means that even terrestrial planets may start off with large radii if they form early enough.[70][71][72] An example is Kepler-51b which has only about twice the mass of Earth but is almost the size of Saturn which is a hundred times the mass of Earth. Kepler-51b is quite young at a few hundred million years old.[73]
Planet-hosting stars[edit]
Main article: Planetary system § Planet-hosting stars
The Morgan-Keenan spectral classification
Artist’s impression of exoplanet orbiting two stars.[74]
There is at least one planet on average per star.[12] About 1 in 5 Sun-like stars[a] have an "Earth-sized"[b] planet in the habitable zone.[75]
Most known exoplanets orbit stars roughly similar to the Sun, i.e. main-sequence stars of spectral categories F, G, or K. Lower-mass stars (red dwarfs, of spectral category M) are less likely to have planets massive enough to be detected by the radial-velocity method.[76][77] Despite this, several tens of planets around red dwarfs have been discovered by the Kepler spacecraft, which uses the transit method to detect smaller planets.
Using data from Kepler, a correlation has been found between the metallicity of a star and the probability that the star host planets. Stars with higher metallicity are more likely to have planets, especially giant planets, than stars with lower metallicity.[78]
Some planets orbit one member of a binary star system,[79] and several circumbinary planets have been discovered which orbit around both members of binary star. A few planets in triple star systems are known[80] and one in the quadruple system Kepler-64.
General features[edit]
Color and brightness[edit]
See also: Sudarsky's gas giant classification
This color–color diagram compares the colors of planets in the Solar System to exoplanet HD 189733b. The exoplanet's deep blue color is produced by silicate droplets, which scatter blue light in its atmosphere.
In 2013 the color of an exoplanet was determined for the first time. The best-fit albedo measurements of HD 189733b suggest that it is deep dark blue.[81][82] Later that same year, the colors of several other exoplanets were determined, including GJ 504 b which visually has a magenta color,[83] and Kappa Andromedae b, which if seen up close would appear reddish in color.[84]
The apparent brightness (apparent magnitude) of a planet depends on how far away the observer is, how reflective the planet is (albedo), and how much light the planet receives from its star, which depends on how far the planet is from the star and how bright the star is. So, a planet with a low albedo that is close to its star can appear brighter than a planet with high albedo that is far from the star.[85]
The darkest known planet in terms of geometric albedo is TrES-2b, a hot Jupiter that reflects less than 1% of the light from its star, making it less reflective than coal or black acrylic paint. Hot Jupiters are expected to be quite dark due to sodium and potassium in their atmospheres but it is not known why TrES-2b is so dark—it could be due to an unknown chemical compound.[86][87][88]
For gas giants, geometric albedo generally decreases with increasing metallicity or atmospheric temperature unless there are clouds to modify this effect. Increased cloud-column depth increases the albedo at optical wavelengths, but decreases it at some infrared wavelengths. Optical albedo increases with age, because older planets have higher cloud-column depths. Optical albedo decreases with increasing mass, because higher-mass giant planets have higher surface gravities, which produces lower cloud-column depths. Also, elliptical orbits can cause major fluctuations in atmospheric composition, which can have a significant effect.[89]
There is more thermal emission than reflection at some near-infrared wavelengths for massive and/or young gas giants. So, although optical brightness is fully phase-dependent, this is not always the case in the near infrared.[89]
Temperatures of gas giants reduce over time and with distance from their star. Lowering the temperature increases optical albedo even without clouds. At a sufficiently low temperature, water clouds form, which further increase optical albedo. At even lower temperatures ammonia clouds form, resulting in the highest albedos at most optical and near-infrared wavelengths.[89]
Magnetic field[edit]
In 2014, a magnetic field around HD 209458 b was inferred from the way hydrogen was evaporating from the planet. It is the first (indirect) detection of a magnetic field on an exoplanet. The magnetic field is estimated to be about one tenth as strong as Jupiter's.[90][91]
Interaction between a close-in planet's magnetic field and a star can produce spots on the star in a similar way to how the Galilean moons produce aurorae on Jupiter.[92] Auroral radio emissions could be detected with radio telescopes such as LOFAR.[93][94] The radio emissions could enable determination of the rotation rate of a planet which is difficult to detect otherwise.[95]
Earth's magnetic field results from its flowing liquid metallic core, but in massive super-Earths with high pressure, different compounds may form which do not match those created under terrestrial conditions. Compounds may form with greater viscosities and high melting temperatures which could prevent the interiors from separating into different layers and so result in undifferentiated coreless mantles. Forms of magnesium oxide such as MgSi3O12 could be a liquid metal at the pressures and temperatures found in super-Earths and could generate a magnetic field in the mantles of super-Earths.[96][97]
Hot Jupiters have been observed to have a larger radius than expected. This could be caused by the interaction between the stellar wind and the planet's magnetosphere creating an electric current through the planet that heats it up causing it to expand. The more magnetically active a star is the greater the stellar wind and the larger the electric current leading to more heating and expansion of the planet. This theory matches the observation that stellar activity is correlated with inflated planetary radii.[98]
Plate tectonics[edit]
In 2007, two independent teams of researchers came to opposing conclusions about the likelihood of plate tectonics on larger super-Earths[99][100] with one team saying that plate tectonics would be episodic or stagnant[101] and the other team saying that plate tectonics is very likely on super-Earths even if the planet is dry.[102]
If super-Earths have more than 80 times as much water as Earth then they become ocean planets with all land completely submerged. However, if there is less water than this limit, then the deep water cycle will move enough water between the oceans and mantle to allow continents to exist.[103][104]
Volcanism[edit]
Large surface temperature variations on 55 Cancri e have been attributed to possible volcanic activity releasing large clouds of dust which blanket the planet and block thermal emissions.[105][106]
Rings[edit]
The star 1SWASP J140747.93-394542.6 is orbited by an object that is circled by a ring system much larger than Saturn's rings. However, the mass of the object is not known; it could be a brown dwarf or low-mass star instead of a planet.[107][108]
The brightness of optical images of Fomalhaut b could be due to starlight reflecting off a circumplanetary ring system with a radius between 20 and 40 times that of Jupiter's radius, about the size of the orbits of the Galilean moons.[109]
The rings of the Solar System's gas giants are aligned with their planet's equator. However, for exoplanets that orbit close to their star, tidal forces from the star would lead to the outermost rings of a planet being aligned with the planet's orbital plane around the star. A planet's innermost rings would still be aligned with the planet's equator so that if the planet has a tilted rotational axis, then the different alignments between the inner and outer rings would create a warped ring system.[110]
Moons[edit]
In December 2013 a candidate exomoon of a rogue planet was announced.[111] No exomoons have been confirmed so far.
Atmospheres[edit]
Main article: Exoplanet atmosphere
Clear versus cloudy atmospheres on two exoplanets.[112]
Atmospheres have been detected around several exoplanets. The first to be observed was HD 209458 b in 2001.[113]
KIC 12557548 b is a small rocky planet, very close to its star, that is evaporating and leaving a trailing tail of cloud and dust like a comet.[114] The dust could be ash erupting from volcanos and escaping due to the small planet's low surface-gravity, or it could be from metals that are vaporized by the high temperatures of being so close to the star with the metal vapor then condensing into dust.[115]
In June 2015, scientists reported that the atmosphere of GJ 436 b was evaporating, resulting in a giant cloud around the planet and, due to radiation from the host star, a long trailing tail 14×10^6 km (9×10^6 mi) long.[116]
In May 2017, glints of light from Earth, seen as twinkling from an orbiting satellite a million miles away, were found to be reflected light from ice crystals in the atmosphere.[117][118] The technology used to determine this may be useful in studying the atmospheres of distant worlds, including those of exoplanets.
Insolation pattern[edit]
Tidally locked planets in a 1:1 spin–orbit resonance would have their star always shining directly overhead on one spot which would be hot with the opposite hemisphere receiving no light and being freezing cold. Such a planet could resemble an eyeball with the hotspot being the pupil.[119] Planets with an eccentric orbit could be locked in other resonances. 3:2 and 5:2 resonances would result in a double-eyeball pattern with hotspots in both eastern and western hemispheres.[120] Planets with both an eccentric orbit and a tilted axis of rotation would have more complicated insolation patterns.[121]
See also: Astrobiology, Circumstellar habitable zone, and Planetary habitability
As more planets are discovered, the field of exoplanetology continues to grow into a deeper study of extrasolar worlds, and will ultimately tackle the prospect of life on planets beyond the Solar System.[60] At cosmic distances, life can only be detected if it is developed at a planetary scale and strongly modified the planetary environment, in such a way that the modifications cannot be explained by classical physico-chemical processes (out of equilibrium processes).[60] For example, molecular oxygen (O
2) in the atmosphere of Earth is a result of photosynthesis by living plants and many kinds of microorganisms, so it can be used as an indication of life on exoplanets, although small amounts of oxygen could also be produced by non-biological means.[122] Furthermore, a potentially habitable planet must orbit a stable star at a distance within which planetary-mass objects with sufficient atmospheric pressure can support liquid water at their surfaces.[123][124]
See also[edit]
Exocomet
Exomoon
Exoplanetology
Extragalactic planet
List of exoplanets
List of exoplanet extremes
List of exoplanet search projects
List of planets
Nexus for Exoplanet System Science
Planetary system
Ultra-short period planet (USP)
Notes[edit]
^ Jump up to: a b For the purpose of this 1 in 5 statistic, "Sun-like" means G-type star. Data for Sun-like stars was not available so this statistic is an extrapolation from data about K-type stars
^ Jump up to: a b For the purpose of this 1 in 5 statistic, Earth-sized means 1–2 Earth radii
Jump up ^ For the purpose of this 1 in 5 statistic, "habitable zone" means the region with 0.25 to 4 times Earth's stellar flux (corresponding to 0.5–2 AU for the Sun).
Jump up ^ About 1/4 of stars are GK Sun-like stars. The number of stars in the galaxy is not accurately known, but assuming 200 billion stars in total, the Milky Way would have about 50 billion Sun-like (GK) stars, of which about 1 in 5 (22%) or 11 billion would be Earth-sized in the habitable zone. Including red dwarfs would increase this to 40 billion.
References[edit]
Jump up ^ "Planet Population is Plentiful". ESO. 11 January 2012. Retrieved 13 January 2012.
Jump up ^ Histogram Plots. Exoplanet.eu
Jump up ^ "Exoplanet Transit Database: TrES-3b". astro.cz. Czech Astronomical Society. Retrieved 7 July 2015.
Jump up ^ "exoplanet Meaning in the Cambridge English Dictionary".
^ Jump up to: a b Landau, Elizabeth (12 November 2017). "Overlooked Treasure: The First Evidence of Exoplanets". NASA. Retrieved 1 November 2017.
^ Jump up to: a b Schneider, J. "Interactive Extra-solar Planets Catalog". The Extrasolar Planets Encyclopedia. Retrieved 1 August 2018.
^ Jump up to: a b Jerry Colen (4 November 2013). "Kepler". nasa.gov. NASA. Archived from the original on 5 November 2013. Retrieved 4 November 2013.
^ Jump up to: a b Harrington, J. D.; Johnson, M. (4 November 2013). "NASA Kepler Results Usher in a New Era of Astronomy".
Jump up ^ Tenenbaum, P.; Jenkins, J. M.; Seader, S.; Burke, C. J.; Christiansen, J. L.; Rowe, J. F.; Caldwell, D. A.; Clarke, B. D.; Li, J.; Quintana, E. V.; Smith, J. C.; Thompson, S. E.; Twicken, J. D.; Borucki, W. J.; Batalha, N. M.; Cote, M. T.; Haas, M. R.; Hunter, R. C.; Sanderfer, D. T.; Girouard, F. R.; Hall, J. R.; Ibrahim, K.; Klaus, T. C.; McCauliff, S. D.; Middour, C. K.; Sabale, A.; Uddin, A. K.; Wohler, B.; Barclay, T.; Still, M. (2013). "Detection of Potential Transit Signals in the First 12 Quarters of Kepler Mission Data". The Astrophysical Journal Supplement Series. 206: 5. arXiv:1212.2915  . Bibcode:2013ApJS..206....5T. doi:10.1088/0067-0049/206/1/5.
Jump up ^ "My God, it's full of planets! They should have sent a poet" (Press release). Planetary Habitability Laboratory, University of Puerto Rico at Arecibo. 3 January 2012.
Jump up ^ Santerne, A.; Díaz, R. F.; Almenara, J.-M.; Lethuillier, A.; Deleuil, M.; Moutou, C. (2013). "Astrophysical false positives in exoplanet transit surveys: Why do we need bright stars?". SF2A-2013: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: L. Cambresy: 555. arXiv:1310.2133  [astro-ph.EP]. Bibcode:2013sf2a.conf..555S.
^ Jump up to: a b Cassan, A.; Kubas, D.; Beaulieu, J. -P.; Dominik, M.; Horne, K.; Greenhill, J.; Wambsganss, J.; Menzies, J.; Williams, A.; Jørgensen, U. G.; Udalski, A.; Bennett, D. P.; Albrow, M. D.; Batista, V.; Brillant, S.; Caldwell, J. A. R.; Cole, A.; Coutures, C.; Cook, K. H.; Dieters, S.; Prester, D. D.; Donatowicz, J.; Fouqué, P.; Hill, K.; Kains, N.; Kane, S.; Marquette, J. -B.; Martin, R.; Pollard, K. R.; Sahu, K. C. (11 January 2012). "One or more bound planets per Milky Way star from microlensing observations". Nature. 481 (7380): 167–169. arXiv:1202.0903  . Bibcode:2012Natur.481..167C. doi:10.1038/nature10684. PMID 22237108.
Jump up ^ Khan, Amina (4 November 2013). "Milky Way may host billions of Earth-size planets". Los Angeles Times. Retrieved 5 November 2013.
Jump up ^ "HR 2562 b". Caltech. Retrieved 15 February 2018.
Jump up ^ Konopacky, Quinn M.; Rameau, Julien; Duchêne, Gaspard; Filippazzo, Joseph C.; Giorla Godfrey, Paige A.; Marois, Christian; Nielsen, Eric L. (20 September 2016). "Discovery of a Substellar Companion to the Nearby Debris Disk Host HR 2562" (Full text). The Astrophysical Journal Letters. 829: 10. arXiv:1608.06660  . Bibcode:2016ApJ...829L...4K. doi:10.3847/2041-8205/829/1/L4.
Jump up ^ Zachos, Elaine (5 February 2018). "More Than a Trillion Planets Could Exist Beyond Our Galaxy – A new study gives the first evidence that exoplanets exist beyond the Milky Way". National Geographic Society. Retrieved 5 February 2018.
Jump up ^ Mandelbaum, Ryan F. (5 February 2018). "Scientists Find Evidence of Thousands of Planets in Distant Galaxy". Gizmodo. Retrieved 5 February 2018.
Jump up ^ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; Berdiñas, Zaira M.; Butler, R. Paul; Coleman, Gavin A. L.; de la Cueva, Ignacio; Dreizler, Stefan; Endl, Michael (2016-08-25). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv:1609.03449  . Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. ISSN 0028-0836. PMID 27558064.
Jump up ^ Overbye, Dennis (6 January 2015). "As Ranks of Goldilocks Planets Grow, Astronomers Consider What's Next". The New York Times.
Jump up ^ Beichman, C.; Gelino, Christopher R.; Kirkpatrick, J. Davy; Cushing, Michael C.; Dodson-Robinson, Sally; Marley, Mark S.; Morley, Caroline V.; Wright, E. L. (2014). "WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection". The Astrophysical Journal. 783 (2): 68. arXiv:1401.1194  . Bibcode:2014ApJ...783...68B. doi:10.1088/0004-637X/783/2/68.
Jump up ^ Neil DeGrasse Tyson in Cosmos: A Spacetime Odyssey as referred to by National Geographic
Jump up ^ Strigari, L. E.; Barnabè, M.; Marshall, P. J.; Blandford, R. D. (2012). "Nomads of the Galaxy". Monthly Notices of the Royal Astronomical Society. 423 (2): 1856–1865. arXiv:1201.2687  . Bibcode:2012MNRAS.423.1856S. doi:10.1111/j.1365-2966.2012.21009.x. estimates 700 objects >10−6 solar masses (roughly the mass of Mars) per main-sequence star between 0.08 and 1 Solar mass, of which there are billions in the Milky Way.
Jump up ^ "ESO's SPHERE Unveils its First Exoplanet". www.eso.org. Retrieved 7 July 2017.
Jump up ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2017-01-29.
Jump up ^ "1992 --"The Year the Milky Way's Planets Came to Life"". Daily Galaxy. 9 January 2017. Retrieved 15 January 2017.
^ Jump up to: a b Wolszczan, A.; Frail, D. A. (1992). "A planetary system around the millisecond pulsar PSR1257 + 12". Nature. 355 (6356): 145–147. Bibcode:1992Natur.355..145W. doi:10.1038/355145a0.
Jump up ^ "These May Be the First Planets Found Outside Our Galaxy". National Geographic. 2018-02-05. Retrieved 2018-02-08.
Jump up ^ Eli Maor (1987). "Chapter 24: The New Cosmology". To Infinity and Beyond: A Cultural History of the Infinite. Originally in De l'infinito universo et mondi [On the Infinite Universe and Worlds] by Giordano Bruno (1584). Boston, MA: Birkhäuser. p. 198. ISBN 978-1-4612-5396-9. Retrieved 9 July 2016.
Jump up ^ Newton, Isaac; I. Bernard Cohen; Anne Whitman (1999) [1713]. The Principia: A New Translation and Guide. University of California Press. p. 940. ISBN 978-0-520-08816-0.
Jump up ^ Struve, Otto (1952). "Proposal for a project of high-precision stellar radial velocity work". The Observatory. 72: 199–200. Bibcode:1952Obs....72..199S.
Jump up ^ Jacob, W. S. (1855). "On Certain Anomalies presented by the Binary Star 70 Ophiuchi". Monthly Notices of the Royal Astronomical Society. 15 (9): 228–230. Bibcode:1855MNRAS..15..228J. doi:10.1093/mnras/15.9.228.
Jump up ^ See, T. J. J. (1896). "Researches on the orbit of 70 Ophiuchi, and on a periodic perturbation in the motion of the system arising from the action of an unseen body". The Astronomical Journal. 16: 17–23. Bibcode:1896AJ.....16...17S. doi:10.1086/102368.
Jump up ^ Sherrill, T. J. (1999). "A Career of Controversy: The Anomaly of T. J. J. See" (PDF). Journal for the History of Astronomy. 30 (98): 25–50. Bibcode:1999JHA....30...25S. doi:10.1177/002182869903000102.
Jump up ^ van de Kamp, P. (1969). "Alternate dynamical analysis of Barnard's star". Astronomical Journal. 74: 757–759. Bibcode:1969AJ.....74..757V. doi:10.1086/110852.
Jump up ^ Boss, Alan (2009). The Crowded Universe: The Search for Living Planets. Basic Books. pp. 31–32. ISBN 978-0-465-00936-7.
Jump up ^ Bailes, M.; Lyne, A. G.; Shemar, S. L. (1991). "A planet orbiting the neutron star PSR1829–10". Nature. 352 (6333): 311–313. Bibcode:1991Natur.352..311B. doi:10.1038/352311a0.
Jump up ^ Lyne, A. G.; Bailes, M. (1992). "No planet orbiting PS R1829–10". Nature. 355 (6357): 213. Bibcode:1992Natur.355..213L. doi:10.1038/355213b0.
Jump up ^ Campbell, B.; Walker, G. A. H.; Yang, S. (1988). "A search for substellar companions to solar-type stars". The Astrophysical Journal. 331: 902. Bibcode:1988ApJ...331..902C. doi:10.1086/166608.
Jump up ^ Lawton, A. T.; Wright, P. (1989). "A planetary system for Gamma Cephei?". Journal of the British Interplanetary Society. 42: 335–336. Bibcode:1989JBIS...42..335L.
Jump up ^ Walker, G. A. H; Bohlender, D. A.; Walker, A. R.; Irwin, A. W.; Yang, S. L. S.; Larson, A. (1992). "Gamma Cephei – Rotation or planetary companion?". Astrophysical Journal Letters. 396 (2): L91–L94. Bibcode:1992ApJ...396L..91W. doi:10.1086/186524.
Jump up ^ Hatzes, A. P.; Cochran, William D.; Endl, Michael; McArthur, Barbara; Paulson, Diane B.; Walker, Gordon A. H.; Campbell, Bruce; Yang, Stephenson (2003). "A Planetary Companion to Gamma Cephei A". Astrophysical Journal. 599 (2): 1383–1394. arXiv:astro-ph/0305110  . Bibcode:2003ApJ...599.1383H. doi:10.1086/379281.
Jump up ^ Holtz, Robert (22 April 1994). "Scientists Uncover Evidence of New Planets Orbiting Star". Los Angeles Times via The Tech Online.
Jump up ^ Mayor, M.; Queloz, D. (1995). "A Jupiter-mass companion to a solar-type star". Nature. 378 (6555): 355–359. Bibcode:1995Natur.378..355M. doi:10.1038/378355a0.
Jump up ^ Gibney, Elizabeth (18 December 2013). "In search of sister earths". Nature. 504 (7480): 361. Bibcode:2013Natur.504..357.. doi:10.1038/504357a.
Jump up ^ Lissauer, J. J. (1999). "Three planets for Upsilon Andromedae". Nature. 398 (6729): 659. Bibcode:1999Natur.398..659L. doi:10.1038/19409.
Jump up ^ Doyle, L. R.; Carter, J. A.; Fabrycky, D. C.; Slawson, R. W.; Howell, S. B.; Winn, J. N.; Orosz, J. A.; Prša, A.; Welsh, W. F.; Quinn, S. N.; Latham, D.; Torres, G.; Buchhave, L. A.; Marcy, G. W.; Fortney, J. J.; Shporer, A.; Ford, E. B.; Lissauer, J. J.; Ragozzine, D.; Rucker, M.; Batalha, N.; Jenkins, J. M.; Borucki, W. J.; Koch, D.; Middour, C. K.; Hall, J. R.; McCauliff, S.; Fanelli, M. N.; Quintana, E. V.; Holman, M. J.; et al. (2011). "Kepler-16: A Transiting Circumbinary Planet". Science. 333 (6049): 1602–6. arXiv:1109.3432  . Bibcode:2011Sci...333.1602D. doi:10.1126/science.1210923. PMID 21921192.
^ Jump up to: a b Johnson, Michele; Harrington, J.D. (26 February 2014). "NASA's Kepler Mission Announces a Planet Bonanza, 715 New Worlds". NASA. Retrieved 26 February 2014.
Jump up ^ Wall, Mike (26 February 2014). "Population of Known Alien Planets Nearly Doubles as NASA Discovers 715 New Worlds". space.com. Retrieved 27 February 2014.
Jump up ^ Jonathan Amos (26 February 2014). "Kepler telescope bags huge haul of planets". BBC News. Retrieved 27 February 2014.
Jump up ^ Johnson, Michelle; Chou, Felicia (23 July 2015). "NASA's Kepler Mission Discovers Bigger, Older Cousin to Earth". NASA.
Jump up ^ Johnson, Michele (9 June 2017). "Media Invited to NASA's Kepler Science Conference". NASA. Retrieved 20 June 2017.
Jump up ^ "NASA's Exoplanet Archive KOI table". NASA. Retrieved 28 February 2014.
Jump up ^ Lewin, Sarah (19 June 2017). "NASA's Kepler Space Telescope Finds Hundreds of New Exoplanets, Boosts Total to 4,034". NASA. Retrieved 19 June 2017.
Jump up ^ Overbye, Dennis (19 June 2017). "Earth-Size Planets Among Final Tally of NASA's Kepler Telescope". The New York Times.
Jump up ^ Exoplanet Anniversary: From Zero to Thousands in 20 Years. NASA News, 6 October 2015.
^ Jump up to: a b Charbonneau, David (May 2008). "The Era of Comparative Exoplanetology." American Astronomical Society. AAS Meeting #212, #54.01; Bulletin of the American Astronomical Society, Vol. 40, p. 250
^ Jump up to: a b Desert, Jean-Michel; Deming, Drake; Knutson, Heather; Bean, Jacob; Fortney, Jonathan; Burrows, Adam; Showman, Adam. "New Frontiers for Comparative Exoplanetology In the Era of Kepler". Spitzer Proposal ID 90092. Bibcode:2012sptz.prop90092D. CS1 maint: Uses authors parameter (link)
Jump up ^ "The Extrasolar Planets Encyclopaedia". Retrieved 2016-08-18.
Jump up ^ Kraus, Adam L.; Ireland, Michael J. (27 December 2012). "LkCa 15: A YOUNG EXOPLANET CAUGHT AT FORMATION?". The Astrophysical Journal. 745 (1): 5. arXiv:1110.3808  . Bibcode:2012ApJ...745....5K. doi:10.1088/0004-637X/745/1/5.
^ Jump up to: a b c d Ollivier, Marc; Maurel, Marie-Christine (2014). "Planetary Environments and Origins of Life: How to reinvent the study of Origins of Life on the Earth and Life in the" (PDF). BIO Web of Conferences 2. 2: 00001. doi:10.1051/bioconf/20140200001. Retrieved 2015-09-11.
Jump up ^ Madhusudhan, Nikku; Agúndez, Marcelino; Moses, Julianne I.; Hu, Yongyun (20 Apr 2016). "Exoplanetary Atmospheres – Chemistry, Formation Conditions, and Habitability". Space Science Reviews. 205 (1): 285–348. arXiv:1604.06092  . Bibcode:2016SSRv..205..285M. doi:10.1007/s11214-016-0254-3. PMC 5207327  . PMID 28057962.
Jump up ^ "ALMA Discovers Trio of Infant Planets around Newborn Star – Novel technique to find youngest planets in our galaxy". www.eso.org. Retrieved 15 June 2018.
Jump up ^ Ollivier M., Encrenaz T., Roques F., Selsis F., Casoli F., Planetary Systems – Detection, Formation and Habitability of Extrasolar Planets, Springer, Berlin (2008)
Jump up ^ Mamajek, Eric E.; Usuda, Tomonori; Tamura, Motohide; Ishii, Miki (2009). "Initial Conditions of Planet Formation: Lifetimes of Primordial Disks". AIP Conference Proceedings. Exoplanets and Disks: Their Formation and Diversity: Proceedings of the International Conference. 1158. p. 3. arXiv:0906.5011  . Bibcode:2009AIPC.1158....3M. doi:10.1063/1.3215910.
Jump up ^ Rice, W. K. M.; Armitage, P. J. (2003). "On the Formation Timescale and Core Masses of Gas Giant Planets". The Astrophysical Journal. 598: L55–L58. arXiv:astro-ph/0310191  . Bibcode:2003ApJ...598L..55R. doi:10.1086/380390.
Jump up ^ Yin, Q.; Jacobsen, S. B.; Yamashita, K.; Blichert-Toft, J.; Télouk, P.; Albarède, F. (2002). "A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites". Nature. 418 (6901): 949–952. Bibcode:2002Natur.418..949Y. doi:10.1038/nature00995. PMID 12198540.
Jump up ^ Calvet, Nuria; D'Alessio, Paola; Hartmann, Lee; Wilner, David; Walsh, Andrew; Sitko, Michael (2001). "Evidence for a developing gap in a 10 Myr old protoplanetary disk". The Astrophysical Journal. 568 (2): 1008–1016. arXiv:astro-ph/0201425  . Bibcode:2002ApJ...568.1008C. doi:10.1086/339061.
Jump up ^ Fridlund, Malcolm; Gaidos, Eric; Barragán, Oscar; Persson, Carina; Gandolfi, Davide; Cabrera, Juan; Hirano, Teruyuki; Kuzuhara, Masayuki; Csizmadia, Sz; Nowak, Grzegorz; Endl, Michael; Grziwa, Sascha; Korth, Judith; Pfaff, Jeremias; Bitsch, Bertram; Johansen, Anders; Mustill, Alexander; Davies, Melvyn; Deeg, Hans; Palle, Enric; Cochran, William; Eigmüller, Philipp; Erikson, Anders; Guenther, Eike; Hatzes, Artie; Kiilerich, Amanda; Kudo, Tomoyuki; MacQueen, Philipp; Narita, Norio; Nespral, David; Pätzold, Martin; Prieto-Arranz, Jorge; Rauer, Heike; van Eylen, Vincent (28 April 2017). "EPIC210894022b −A short period super-Earth transiting a metal poor, evolved old star". Astronomy & Astrophysics. arXiv:1704.08284  .
Jump up ^ D'Angelo, G.; Durisen, R. H.; Lissauer, J. J. (2011). "Giant Planet Formation". In S. Seager. Exoplanets. University of Arizona Press, Tucson, AZ. pp. 319–346. arXiv:1006.5486  . Bibcode:2010exop.book..319D.
Jump up ^ Lammer, H.; Stokl, A.; Erkaev, N. V.; Dorfi, E. A.; Odert, P.; Gudel, M.; Kulikov, Y. N.; Kislyakova, K. G.; Leitzinger, M. (2014). "Origin and loss of nebula-captured hydrogen envelopes from 'sub'- to 'super-Earths' in the habitable zone of Sun-like stars". Monthly Notices of the Royal Astronomical Society. 439 (4): 3225–3238. arXiv:1401.2765  . Bibcode:2014MNRAS.439.3225L. doi:10.1093/mnras/stu085.
Jump up ^ Johnson, R. E. (2010). "Thermally-Diven Atmospheric Escape". The Astrophysical Journal. 716 (2): 1573–1578. arXiv:1001.0917  . Bibcode:2010ApJ...716.1573J. doi:10.1088/0004-637X/716/2/1573.
Jump up ^ Zendejas, J.; Segura, A.; Raga, A.C. (2010). "Atmospheric mass loss by stellar wind from planets around main sequence M stars". Icarus. 210 (2): 539–544. arXiv:1006.0021  . Bibcode:2010Icar..210..539Z. doi:10.1016/j.icarus.2010.07.013.
Jump up ^ Masuda, K. (2014). "Very Low Density Planets Around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event". The Astrophysical Journal. 783: 53. arXiv:1401.2885  . Bibcode:2014ApJ...783...53M. doi:10.1088/0004-637X/783/1/53.
Jump up ^ "Artist's impression of exoplanet orbiting two stars". www.spacetelescope.org. Retrieved 24 September 2016.
Jump up ^ Petigura, E. A.; Howard, A. W.; Marcy, G. W. (2013). "Prevalence of Earth-size planets orbiting Sun-like stars". Proceedings of the National Academy of Sciences. 110 (48): 19273–19278. arXiv:1311.6806  . Bibcode:2013PNAS..11019273P. doi:10.1073/pnas.1319909110. PMC 3845182  . PMID 24191033.
Jump up ^ Cumming, Andrew; Butler, R. Paul; Marcy, Geoffrey W.; Vogt, Steven S.; Wright, Jason T.; Fischer, Debra A. (2008). "The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets". Publications of the Astronomical Society of the Pacific. 120 (867): 531–554. arXiv:0803.3357  . Bibcode:2008PASP..120..531C. doi:10.1086/588487.
Jump up ^ Bonfils, X.; Forveille, T.; Delfosse, X.; Udry, S.; Mayor, M.; Perrier, C.; Bouchy, F.; Pepe, F.; Queloz, D.; Bertaux, J. -L. (2005). "The HARPS search for southern extra-solar planets". Astronomy and Astrophysics. 443 (3): L15–L18. arXiv:astro-ph/0509211  . Bibcode:2005A&A...443L..15B. doi:10.1051/0004-6361:200500193.
Jump up ^ Wang, J.; Fischer, D. A. (2014). "Revealing a Universal Planet–Metallicity Correlation for Planets of Different Solar-Type Stars". The Astronomical Journal. 149: 14. arXiv:1310.7830  . Bibcode:2015AJ....149...14W. doi:10.1088/0004-6256/149/1/14.
Jump up ^ Schwarz, Richard. Binary Catalogue of Exoplanets. Universität Wien
Jump up ^ Schwarz, Richard. STAR-DATA. Universität Wien
Jump up ^ NASA Hubble Finds a True Blue Planet. NASA. 11 July 2013
Jump up ^ Evans, T. M.; Pont, F. D. R.; Sing, D. K.; Aigrain, S.; Barstow, J. K.; Désert, J. M.; Gibson, N.; Heng, K.; Knutson, H. A.; Lecavelier Des Etangs, A. (2013). "The Deep Blue Color of HD189733b: Albedo Measurements with Hubble Space Telescope/Space Telescope Imaging Spectrograph at Visible Wavelengths" (Full text). The Astrophysical Journal. 772 (2): L16. arXiv:1307.3239  . Bibcode:2013ApJ...772L..16E. doi:10.1088/2041-8205/772/2/L16.
Jump up ^ Kuzuhara, M.; Tamura, M.; Kudo, T.; Janson, M.; Kandori, R.; Brandt, T. D.; Thalmann, C.; Spiegel, D.; Biller, B.; Carson, J.; Hori, Y.; Suzuki, R.; Burrows, A.; Henning, T.; Turner, E. L.; McElwain, M. W.; Moro-Martín, A.; Suenaga, T.; Takahashi, Y. H.; Kwon, J.; Lucas, P.; Abe, L.; Brandner, W.; Egner, S.; Feldt, M.; Fujiwara, H.; Goto, M.; Grady, C. A.; Guyon, O.; Hashimoto, J.; et al. (2013). "Direct Imaging of a Cold Jovian Exoplanet in Orbit around the Sun-like Star GJ 504" (Full text). The Astrophysical Journal. 774 (11): 11. arXiv:1307.2886  . Bibcode:2013ApJ...774...11K. doi:10.1088/0004-637X/774/1/11.
Jump up ^ Carson; Thalmann; Janson; Kozakis; Bonnefoy; Biller; Schlieder; Currie; McElwain (15 November 2012). "Direct Imaging Discovery of a 'Super-Jupiter' Around the late B-Type Star Kappa And". The Astrophysical Journal. 763 (2): L32. arXiv:1211.3744  [astro-ph.SR]. Bibcode:2013ApJ...763L..32C. doi:10.1088/2041-8205/763/2/L32.
Jump up ^ The Apparent Brightness and Size of Exoplanets and their Stars, Abel Mendez, updated 30 June 2012, 12:10 PM
Jump up ^ "Coal-Black Alien Planet Is Darkest Ever Seen". Space.com. Retrieved 12 August 2011.
Jump up ^ Kipping, David M.; Spiegel, David S. (2011). "Detection of visible light from the darkest world". Monthly Notices of the Royal Astronomical Society: Letters. 417: L88–L92. arXiv:1108.2297  . Bibcode:2011MNRAS.417L..88K. doi:10.1111/j.1745-3933.2011.01127.x.
Jump up ^ Barclay, T.; Huber, D.; Rowe, J. F.; Fortney, J. J.; Morley, C. V.; Quintana, E. V.; Fabrycky, D. C.; Barentsen, G.; Bloemen, S.; Christiansen, J. L.; Demory, B. O.; Fulton, B. J.; Jenkins, J. M.; Mullally, F.; Ragozzine, D.; Seader, S. E.; Shporer, A.; Tenenbaum, P.; Thompson, S. E. (2012). "Photometrically derived masses and radii of the planet and star in the TrES-2 system". The Astrophysical Journal. 761: 53. arXiv:1210.4592  . Bibcode:2012ApJ...761...53B. doi:10.1088/0004-637X/761/1/53.
^ Jump up to: a b c Burrows, Adam (2014). "Scientific Return of Coronagraphic Exoplanet Imaging and Spectroscopy Using WFIRST". arXiv:1412.6097  [astro-ph.EP].
Jump up ^ Unlocking the Secrets of an Alien World's Magnetic Field, Space.com, by Charles Q. Choi, 20 November 2014
Jump up ^ Kislyakova, K. G.; Holmstrom, M.; Lammer, H.; Odert, P.; Khodachenko, M. L. (2014). "Magnetic moment and plasma environment of HD 209458b as determined from Ly observations". Science. 346 (6212): 981–4. arXiv:1411.6875  . Bibcode:2014Sci...346..981K. doi:10.1126/science.1257829. PMID 25414310.
Jump up ^ Footprint of a Magnetic Exoplanet, www.skyandtelescope.com, 9 January 2004, Robert Naeye
Jump up ^ Nichols, J. D. (2011). "Magnetosphere-ionosphere coupling at Jupiter-like exoplanets with internal plasma sources: Implications for detectability of auroral radio emissions". Monthly Notices of the Royal Astronomical Society. 414 (3): 2125–2138. arXiv:1102.2737  . Bibcode:2011MNRAS.414.2125N. doi:10.1111/j.1365-2966.2011.18528.x.
Jump up ^ Radio Telescopes Could Help Find Exoplanets. RedOrbit. 18 April 2011
Jump up ^ "Radio Detection of Extrasolar Planets: Present and Future Prospects" (PDF). NRL, NASA/GSFC, NRAO, Observatoìre de Paris. Retrieved 15 October 2008.
Jump up ^ Kean, Sam (2016). "Forbidden plants, forbidden chemistry". Distillations. 2 (2): 5. Retrieved 22 March 2018.
Jump up ^ Super-Earths Get Magnetic 'Shield' from Liquid Metal, Charles Q. Choi, SPACE.com, 22 November 2012.
Jump up ^ Buzasi, D. (2013). "Stellar Magnetic Fields As a Heating Source for Extrasolar Giant Planets". The Astrophysical Journal. 765 (2): L25. arXiv:1302.1466  . Bibcode:2013ApJ...765L..25B. doi:10.1088/2041-8205/765/2/L25.
Jump up ^ Valencia, Diana; O'Connell, Richard J. (2009). "Convection scaling and subduction on Earth and super-Earths". Earth and Planetary Science Letters. 286 (3–4): 492–502. Bibcode:2009E&PSL.286..492V. doi:10.1016/j.epsl.2009.07.015.
Jump up ^ Van Heck, H.J.; Tackley, P.J. (2011). "Plate tectonics on super-Earths: Equally or more likely than on Earth". Earth and Planetary Science Letters. 310 (3–4): 252–261. Bibcode:2011E&PSL.310..252V. doi:10.1016/j.epsl.2011.07.029.
Jump up ^ O'Neill, C.; Lenardic, A. (2007). "Geological consequences of super-sized Earths". Geophysical Research Letters. 34 (19): L19204. Bibcode:2007GeoRL..3419204O. doi:10.1029/2007GL030598.
Jump up ^ Valencia, Diana; O'Connell, Richard J.; Sasselov, Dimitar D (November 2007). "Inevitability of Plate Tectonics on Super-Earths". Astrophysical Journal Letters. 670 (1): L45–L48. arXiv:0710.0699  . Bibcode:2007ApJ...670L..45V. doi:10.1086/524012.
Jump up ^ Super Earths Likely To Have Both Oceans and Continents, astrobiology.com. 7 January 2014
Jump up ^ Cowan, N. B.; Abbot, D. S. (2014). "Water Cycling Between Ocean and Mantle: Super-Earths Need Not Be Waterworlds". The Astrophysical Journal. 781: 27. arXiv:1401.0720  . Bibcode:2014ApJ...781...27C. doi:10.1088/0004-637X/781/1/27.
Jump up ^ Michael D. Lemonick (6 May 2015). "Astronomers May Have Found Volcanoes 40 Light-Years From Earth". National Geographic. Retrieved 8 November 2015.
Jump up ^ Demory, Brice-Olivier; Gillon, Michael; Madhusudhan, Nikku; Queloz, Didier (2015). "Variability in the super-Earth 55 Cnc e". Monthly Notices of the Royal Astronomical Society. 455 (2): 2018–2027. arXiv:1505.00269  . Bibcode:2016MNRAS.455.2018D. doi:10.1093/mnras/stv2239.
Jump up ^ Scientists Discover a Saturn-like Ring System Eclipsing a Sun-like Star, Space Daily, 13 January 2012
Jump up ^ Mamajek, E. E.; Quillen, A. C.; Pecaut, M. J.; Moolekamp, F.; Scott, E. L.; Kenworthy, M. A.; Cameron, A. C.; Parley, N. R. (2012). "Planetary Construction Zones in Occultation: Discovery of an Extrasolar Ring System Transiting a Young Sun-Like Star and Future Prospects for Detecting Eclipses by Circumsecondary and Circumplanetary Disks". The Astronomical Journal. 143 (3): 72. arXiv:1108.4070  . Bibcode:2012AJ....143...72M. doi:10.1088/0004-6256/143/3/72.
Jump up ^ Kalas, P.; Graham, J. R.; Chiang, E.; Fitzgerald, M. P.; Clampin, M.; Kite, E. S.; Stapelfeldt, K.; Marois, C.; Krist, J. (2008). "Optical Images of an Exosolar Planet 25 Light-Years from Earth". Science. 322 (5906): 1345–8. arXiv:0811.1994  . Bibcode:2008Sci...322.1345K. doi:10.1126/science.1166609. PMID 19008414.
Jump up ^ Schlichting, Hilke E.; Chang, Philip (2011). "Warm Saturns: On the Nature of Rings around Extrasolar Planets That Reside inside the Ice Line". The Astrophysical Journal. 734 (2): 117. arXiv:1104.3863  . Bibcode:2011ApJ...734..117S. doi:10.1088/0004-637X/734/2/117.
Jump up ^ Bennett, D. P.; Batista, V.; Bond, I. A.; Bennett, C. S.; Suzuki, D.; Beaulieu, J. -P.; Udalski, A.; Donatowicz, J.; Bozza, V.; Abe, F.; Botzler, C. S.; Freeman, M.; Fukunaga, D.; Fukui, A.; Itow, Y.; Koshimoto, N.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Namba, S.; Ohnishi, K.; Rattenbury, N. J.; Saito, T.; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Tristram, P. J.; Tsurumi, N.; Wada, K.; et al. (2014). "MOA-2011-BLG-262Lb: A sub-Earth-mass moon orbiting a gas giant or a high-velocity planetary system in the galactic bulge". The Astrophysical Journal. 785 (2): 155. arXiv:1312.3951  . Bibcode:2014ApJ...785..155B. doi:10.1088/0004-637X/785/2/155.
Jump up ^ "Cloudy versus clear atmospheres on two exoplanets". www.spacetelescope.org. Retrieved 6 June 2017.
Jump up ^ Charbonneau, David; et al. (2002). "Detection of an Extrasolar Planet Atmosphere". The Astrophysical Journal. 568 (1): 377–384. arXiv:astro-ph/0111544  . Bibcode:2002ApJ...568..377C. doi:10.1086/338770.
Jump up ^ Evaporating exoplanet stirs up dust. Phys.org. 28 August 2012
Jump up ^ Woollacott, Emma (18 May 2012) New-found exoplanet is evaporating away. TG Daily
Jump up ^ Bhanoo, Sindya N. (25 June 2015). "A Planet with a Tail Nine Million Miles Long". The New York Times. Retrieved 25 June 2015.
Jump up ^ St. Fleur, Nicholas (19 May 2017). "Spotting Mysterious Twinkles on Earth From a Million Miles Away". The New York Times. Retrieved 20 May 2017.
Jump up ^ Marshak, Alexander; Várnai, Tamás; Kostinski, Alexander (15 May 2017). "Terrestrial glint seen from deep space: oriented ice crystals detected from the Lagrangian point". Geophysical Research Letters. 44 (10): 5197–5202. Bibcode:2017GeoRL..44.5197M. doi:10.1002/2017GL073248.
Jump up ^ Forget "Earth-Like"—We'll First Find Aliens on Eyeball Planets, Nautilus, Posted by Sean Raymond on 20 February 2015
Jump up ^ Dobrovolskis, Anthony R. (2015). "Insolation patterns on eccentric exoplanets". Icarus. 250: 395–399. Bibcode:2015Icar..250..395D. doi:10.1016/j.icarus.2014.12.017.
Jump up ^ Tony Dobrovolskis (18 March 2014). "Patterns of Sunlight on Extra-Solar Planets". SETI Institute. Retrieved 25 March 2014.
Jump up ^ "Oxygen Is Not Definitive Evidence of Life on Extrasolar Planets". NAOJ. Astrobiology Web. 10 September 2015. Retrieved 2015-09-11.
Jump up ^ Kopparapu, Ravi Kumar (2013). "A revised estimate of the occurrence rate of terrestrial planets in the habitable zones around kepler m-dwarfs". The Astrophysical Journal Letters. 767 (1): L8. arXiv:1303.2649  . Bibcode:2013ApJ...767L...8K. doi:10.1088/2041-8205/767/1/L8.
Jump up ^ Cruz, Maria; Coontz, Robert (2013). "Exoplanets - Introduction to Special Issue". Science. 340 (6132): 565. doi:10.1126/science.340.6132.565. Retrieved 18 May 2013.
Further reading[edit]
Boss, Alan (2009). The Crowded Universe: The Search for Living Planets. Basic Books. ISBN 978-0-465-00936-7 (Hardback); ISBN 978-0-465-02039-3 (Paperback).
Dorminey, Bruce (2001). Distant Wanderers. Springer-Verlag. ISBN 978-0-387-95074-7 (Hardback); ISBN 978-1-4419-2872-6 (Paperback).
Jayawardhana, Ray (2011). Strange New Worlds: The Search for Alien Planets and Life beyond Our Solar System. Princeton, NJ: Princeton University Press. ISBN 978-0-691-14254-8 (Hardcover).
Perryman, Michael (2011). The Exoplanet Handbook. Cambridge University Press. ISBN 978-0-521-76559-6.
Seager, Sara, ed. (2011). Exoplanets. University of Arizona Press. ISBN 978-0-8165-2945-2.
Villard, Ray; Cook, Lynette R. (2005). Infinite Worlds: An Illustrated Voyage to Planets Beyond Our Sun. University of California Press. ISBN 978-0-520-23710-0.
Yaqoob, Tahir (2011). Exoplanets and Alien Solar Systems. New Earth Labs (Education and Outreach). ISBN 978-0-9741689-2-0 (Paperback).
van Dishoeck, Ewine F.; Bergin, Edwin A.; Lis, Dariusz C.; Lunine, Jonathan I. (2014). "Water: From Clouds to Planets". Protostars and Planets VI. arXiv:1401.8103  [astro-ph.GA]. Bibcode:2014prpl.conf..835V. doi:10.2458/azu_uapress_9780816531240-ch036. ISBN 978-0-8165-3124-0.
External links[edit]
Wikimedia Commons has media related to Exoplanets.
Wikiversity has learning resources about Observational astronomy/Extrasolar planet
The Extrasolar Planets Encyclopaedia (Paris Observatory)
NASA Exoplanet Archive
Open Exoplanet Catalogue
The Habitable Exoplanets Catalog (PHL/UPR Arecibo)
Extrasolar Planets – D. Montes, UCM
Exoplanets at Paris Observatory
Graphical Comparison of Extrasolar Planets
show
v
t
e
Exoplanetology
Planet
Definition
IAU
Planetary science
Main topics
Exoplanet
Methods of detecting exoplanets
Planetary system
Sizes and types
Terrestrial
Carbon planet
Coreless planet
Desert planet
Dwarf planet
Ice planet
Iron planet
Lava planet
Mega-Earth
Ocean planet
Sub-Earth
Super-Earth
Gaseous
Chthonian planet
Eccentric Jupiter
Gas dwarf
Helium planet
Hot Jupiter
Hot Neptune
Ice giant
Mini-Neptune
Super-Neptune
Super-Jupiter
Other types
Brown dwarf
Circumbinary planet
Double planet
Mesoplanet
Planemo
Planet/Brown dwarf boundary
Planetesimal
Protoplanet
Pulsar planet
Sub-brown dwarf
Ultra-cool dwarf
Ultra-short period planets (USP)
Formation and evolution
Accretion
Merging stars
Nebular hypothesis
Planetary migration
Systems
Exocomet
Exomoon
Interstellar comet
Mean-motion resonances
Retrograde planet
Rogue planet
Titius–Bode laws
Trojan planet
Host stars
A
B
Binary star
Brown dwarfs
Extragalactic planet
F/Yellow-white dwarfs
G/Yellow dwarfs
Herbig Ae/Be
K/Orange dwarfs
M/Red dwarfs
Planets in globular clusters
Pulsar
Red giant
Subdwarf B
Subgiant
T Tauri
White dwarfs
Yellow giant
Detection
Astrometry
Direct imaging
list
Microlensing
list
Polarimetry
Pulsar timing
list
Radial velocity
list
Transit method
list
Transit-timing variation
Habitability
Astrobiology
Circumstellar habitable zone
Earth analog
Extraterrestrial liquid water
Habitability of natural satellites
Superhabitable planet
Catalogues
Catalog of Nearby Habitable Systems
Exoplanet Data Explorer
Extrasolar Planets Encyclopaedia
NASA Exoplanet Archive
NASA Star and Exoplanet Database
Lists
Exoplanetary systems
Host stars
Multiplanetary systems
Stars with proplyds
Exoplanets
List of exoplanets
Discoveries
Extremes
Firsts
Nearest
Largest
Most massive
Terrestrial candidates
Kepler
Potentially habitable
Discovered exoplanets by year
before 2000
2000–2009
2010
2011
2012
2013
2014
2015
2016
2017
2018
Other
Carl Sagan Institute
Exoplanet phase curves
Nexus for Exoplanet System Science
Planets in science fiction
Sudarsky's gas giant classification
Discoveries of exoplanets
Search projects
show
v
t
e
Exoplanet search projects
Exoplanetology
Exoplanet
Ground-based
AAPS
APF
CORALIE
EAPSNet
ELODIE
EPICS
ESPRESSO
FINDS Exo-Earths
Geneva
HARPS
HARPS-N
GPI
HATNet
HEK
HiCIAO
HIRES
KELT
LCES
Magellan
MARVELS
MASCARA
MEarth
MicroFUN
MINERVA
Australis
MOA
N2K
NGTS
NESSI
OGLE
OPSP
PlanetPol
Project 1640
PARAS
SEEDS
SETI
SOPHIE
SPECULOOS
SPHERE
SuperWASP
Systemic
TrES
XO Telescope
ZIMPOL/CHEOPS

Space missions
Past
SWEEPS using HST (2006)
CoRoT (2006–13)
EPOXI using Deep Impact (2008–13)
Current
MOST (2003–present)
Kepler (2009–present)
detected exoplanets
Gaia (2013–present)
ASTERIA (2017–present)
TESS (2018–present)
Planned
CHEOPS (2019)
James Webb Space Telescope (2021)
PLATO (2026)
WFIRST (mid-2020s)
Proposed
ATLAST
EXCEDE
FINESSE
HabEx
HDST
LUVOIR
New Worlds Mission
OST
PEGASE
Cancelled
Darwin
EChO
Eddington
Space Interferometry Mission
Terrestrial Planet Finder
Detection methods
Discoveries of exoplanets
List of exoplanets
full
nearest
Astrobiology portal
Astronomy portal
Space portal
Authority control
BNF: cb13181541m (data)
GND: 4456110-6
SUDOC: 035322225
Retrieved from "https://en.wikipedia.org/w/index.php?title=Exoplanet&oldid=853681430"
Categories:
Exoplanetology
Exoplanets
Search for extraterrestrial intelligence
Types of planet
Hidden categories:
CS1 maint: Uses authors parameter
Use dmy dates from February 2015
Wikipedia articles with BNF identifiers
Wikipedia articles with GND identifiers
Wikipedia articles with SUDOC identifiers
Articles containing video clips
Navigation menu
Personal tools
Not logged in
Talk
Contributions
Create account
Log in
Namespaces
Article
Talk
Variants
Views
Read
Edit
View history
More
Search
Navigation
Main page
Contents
Featured content
Current events
Random article
Donate to Wikipedia
Wikipedia store
Interaction
Help
About Wikipedia
Community portal
Recent changes
Contact page
Tools
What links here
Related changes
Upload file
Special pages
Permanent link
Page information
Wikidata item
Cite this page
Print/export
Create a book
Download as PDF
Printable version
In other projects
Wikimedia Commons
Languages
Afrikaans
العربية
Asturianu
Azərbaycanca
বাংলা
Беларуская
Беларуская (тарашкевіца)
Български
Bosanski
Brezhoneg
Català
Чӑвашла
Čeština
Cymraeg
Dansk
Deutsch
Eesti
Ελληνικά
Español
Esperanto
Estremeñu
Euskara
فارسی
Français
Gaeilge
Galego
한국어
Հայերեն
हिन्दी
Hrvatski
Ido
Bahasa Indonesia
Íslenska
Italiano
עברית
Basa Jawa
ಕನ್ನಡ
ქართული
Қазақша
Kiswahili
Коми
Latina
Latviešu
Lëtzebuergesch
Lietuvių
Limburgs
Magyar
Македонски
മലയാളം
मराठी
Bahasa Melayu
မြန်မာဘာသာ
Nederlands
日本語
Norsk
Norsk nynorsk
Occitan
Oʻzbekcha/ўзбекча
پنجابی
Polski
Português
Română
Русский
Scots
Shqip
Sicilianu
සිංහල
Simple English
Slovenčina
Slovenščina
Српски / srpski
Srpskohrvatski / српскохрватски
Suomi
Svenska
Tagalog
தமிழ்
Татарча/tatarça
ไทย
Türkçe
Українська
اردو
Tiếng Việt
Winaray
粵語
中文
Lingua Franca Nova
77 more
Edit links
This page was last edited on 6 August 2018, at 09:36 (UTC).
Text is available under the Creative Commons Attribution-ShareAlike License; additional terms may apply. By using this site, you agree to the Terms of Use and Privacy Policy. Wikipedia® is a registered trademark of the Wikimedia Foundation, Inc., a non-profit organization.
Privacy policy
About Wikipedia
Disclaimers
Contact Wikipedia
Developers
Cookie statement
Mobile view
Enable previews

values: mw-page-base noprint

values: mw-head-base noprint

values: firstHeading firstHeading en

values: siteSub noprint

attrs: class href

values: mw-jump-link #mw-head

values: mw-jump-link #p-search

values:
note
hatnote navigation-not-searchable

value: p

values: Size-exaggerated artist's conception showing the ratio of planets to stars in our galaxy

value: sup

attrs: class style

values: thumbcaption clear:left

values: Histogram of Discovered Exoplanets each year as of 26 November 2017

values: Size comparison of Jupiter and the exoplanet TrES-3b

values:
/wiki/Transit_method
mw-redirect
Transit method

values: Histogram Chart of Confirmed Exoplanets by distance

values: High Accuracy Radial Velocity Planet Searcher

values:
/wiki/False_positive
mw-redirect
False positive

values:
/wiki/Habitable_zone
mw-redirect
Habitable zone

values: checkbox button toctogglecheckbox toctogglecheckbox display:none

values:
/wiki/Direct_imaging
mw-redirect
Direct imaging

values: color:#b2b7f2; font-size:3.3em; font-family:'Times New Roman',serif; font-weight:bold; padding:4px 2px 2px; width:0.5em; line-height: 1em;

values: color:#b2b7f2; font-size:3.3em; font-family:'Times New Roman',serif; font-weight:bold; padding:4px 2px 2px; text-align:right; vertical-align:bottom; width:0.5em; line-height: 1em;

values: padding-top:10px; font-size:smaller; line-height:1em; text-align:right;

values: border-collapse:collapse; border-style:none; float:right ; margin:0.5em 0.75em; width:33%;

values: Philosophiae Naturalis Principia Mathematica

values:
/wiki/PSR_1829-10
mw-redirect
PSR 1829-10

values:
/wiki/Pulsar_timing
mw-redirect
Pulsar timing

values: False-color, star-subtracted, direct image using a vortex coronagraph of 3 exoplanets around star HR8799

values:
/wiki/Vector_vortex_coronagraph
mw-redirect
Vector vortex coronagraph

values: Hubble image of brown dwarf 2MASS J044144 and its 5–10 Jupiter-mass companion, before and after star-subtraction

values:
/wiki/2MASS_J044144
mw-redirect
2MASS J044144

values: List of instruments at the Very Large Telescope

values:
/wiki/G-type_star
mw-redirect
G-type star

values:
/wiki/Observatoire_de_Haute-Provence
mw-redirect
Observatoire de Haute-Provence

values: The Morgan-Keenan spectral classification system, showing size-and-color comparisons of M, K, G, F, A, B, and O stars

values:
/wiki/Radial-velocity_method
mw-redirect
Radial-velocity method

values:
/wiki/Triple_star
mw-redirect
Triple star

values: Color-color diagram comparing the colors of Solar System planets to exoplanet HD 189733b. HD 189733b reflects as much green as Mars and almost as much blue as Earth.

values:
/wiki/Aurora_(astronomy)
mw-redirect
Aurora (astronomy)

values:
/wiki/Saturn%27s_rings
mw-redirect
Saturn's rings

values:
/wiki/Galilean_moon
mw-redirect
Galilean moon

values:
/wiki/Exoplanet_atmosphere
mw-redirect
Exoplanet atmosphere

values:
/wiki/KIC_12557548_b
mw-redirect
KIC 12557548 b

values:
/wiki/Tidally_locked
mw-redirect
Tidally locked

values:
/wiki/Spin%E2%80%93orbit_resonance
mw-redirect
Spin–orbit resonance

values:
/wiki/Planetary-mass_object
mw-redirect
Planetary-mass object

values:
/wiki/Liquid_water
mw-redirect
Liquid water

values:
/wiki/List_of_planets
mw-redirect
List of planets

values:
/wiki/Ultra-short_period_planet
mw-redirect
Ultra-short period planet

values:
/wiki/K-type_star
mw-redirect
K-type star

values:
reflist mw-references-wrap
list-style-type: lower-alpha;

values:
nofollow
http://www.eso.org/public/news/eso1204/
external text

values:
nofollow
external text
http://exoplanet.eu/diagrams/?t=h

values:
nofollow
external text
http://exoplanet.eu/catalog.php

values:
nofollow
external text
//arxiv.org/abs/1212.2915

values:
nofollow
external text
//arxiv.org/abs/1310.2133

values:
nofollow
external text
//arxiv.org/archive/astro-ph.EP

values:
nofollow
external text
//arxiv.org/abs/1202.0903

values:
nofollow
external text
//doi.org/10.1038/nature10684

values:
/wiki/PubMed_Identifier
mw-redirect
PubMed Identifier

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/22237108

values:
nofollow
external text
http://dro.dur.ac.uk/20763/1/20763.pdf

values:
nofollow
external text
//arxiv.org/abs/1608.06660

values:
nofollow
external text
//arxiv.org/abs/1609.03449

values:
nofollow
external text
//doi.org/10.1038/nature19106

values:
nofollow
external text
//www.worldcat.org/issn/0028-0836

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/27558064

values:
nofollow
external text
//arxiv.org/abs/1401.1194

values:
/wiki/Neil_DeGrasse_Tyson
mw-redirect
Neil DeGrasse Tyson

values: Monthly Notices of the Royal Astronomical Society

values:
nofollow
external text
//arxiv.org/abs/1201.2687

values:
nofollow
external text
//doi.org/10.1038/355145a0

values:
nofollow
external text
//doi.org/10.1093/mnras/15.9.228

values:
nofollow
external text
//doi.org/10.1086/102368

values:
nofollow
external text
http://www.shpltd.co.uk/jha.pdf

values:
/wiki/Astronomical_Journal
mw-redirect
Astronomical Journal

values:
nofollow
external text
//doi.org/10.1086/110852

values:
nofollow
external text
//doi.org/10.1038/352311a0

values:
nofollow
external text
//doi.org/10.1038/355213b0

values:
nofollow
external text
//doi.org/10.1086/166608

values: Journal of the British Interplanetary Society

values:
/wiki/Astrophysical_Journal_Letters
mw-redirect
Astrophysical Journal Letters

values:
nofollow
external text
//doi.org/10.1086/186524

values:
/wiki/Astrophysical_Journal
mw-redirect
Astrophysical Journal

values:
nofollow
external text
//arxiv.org/abs/astro-ph/0305110

values:
nofollow
external text
//doi.org/10.1086/379281

values:
nofollow
external text
//doi.org/10.1038/378355a0

values:
nofollow
external text
//doi.org/10.1038/504357a

values:
nofollow
external text
//doi.org/10.1038/19409

values:
nofollow
external text
//arxiv.org/abs/1109.3432

values:
nofollow
external text
//doi.org/10.1126/science.1210923

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/21921192

values: Category:CS1 maint: Uses authors parameter

values:
nofollow
http://exoplanet.eu/catalog/
external text

values:
nofollow
external text
//arxiv.org/abs/1110.3808

values:
nofollow
external text
//doi.org/10.1051/bioconf/20140200001

values:
nofollow
external text
//arxiv.org/abs/1604.06092

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/28057962

values:
nofollow
external text
//arxiv.org/abs/0906.5011

values:
nofollow
external text
//doi.org/10.1063/1.3215910

values:
nofollow
external text
//arxiv.org/abs/astro-ph/0310191

values:
nofollow
external text
//doi.org/10.1086/380390

values:
nofollow
external text
//doi.org/10.1038/nature00995

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/12198540

values:
nofollow
external text
//arxiv.org/abs/astro-ph/0201425

values:
nofollow
external text
//doi.org/10.1086/339061

values:
nofollow
external text
//arxiv.org/abs/1704.08284

values:
nofollow
external text
//arxiv.org/abs/1006.5486

values:
nofollow
external text
//arxiv.org/abs/1401.2765

values:
nofollow
external text
//doi.org/10.1093/mnras/stu085

values:
nofollow
external text
//arxiv.org/abs/1001.0917

values:
nofollow
external text
//arxiv.org/abs/1006.0021

values:
nofollow
external text
//doi.org/10.1016/j.icarus.2010.07.013

values:
nofollow
external text
//arxiv.org/abs/1401.2885

values: Proceedings of the National Academy of Sciences

values:
nofollow
external text
//arxiv.org/abs/1311.6806

values:
nofollow
external text
//doi.org/10.1073/pnas.1319909110

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/24191033

values:
nofollow
external text
//arxiv.org/abs/0803.3357

values:
nofollow
external text
//doi.org/10.1086/588487

values:
nofollow
external text
//arxiv.org/abs/astro-ph/0509211

values:
nofollow
external text
//arxiv.org/abs/1310.7830

values:
nofollow
external text
//arxiv.org/abs/1307.3239

values:
nofollow
external text
//arxiv.org/abs/1307.2886

values:
nofollow
external text
//arxiv.org/abs/1211.3744

values:
nofollow
external text
//arxiv.org/archive/astro-ph.SR

values:
nofollow
external text
//arxiv.org/abs/1108.2297

values:
nofollow
external text
//arxiv.org/abs/1210.4592

values:
nofollow
external text
//arxiv.org/abs/1412.6097

values:
nofollow
external text
//arxiv.org/abs/1411.6875

values:
nofollow
external text
//doi.org/10.1126/science.1257829

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/25414310

values:
nofollow
external text
//arxiv.org/abs/1102.2737

values:
nofollow
external text
//arxiv.org/abs/1302.1466

values:
nofollow
external text
//doi.org/10.1016/j.epsl.2009.07.015

values:
nofollow
external text
//doi.org/10.1016/j.epsl.2011.07.029

values:
nofollow
external text
//doi.org/10.1029/2007GL030598

values:
nofollow
external text
//arxiv.org/abs/0710.0699

values:
nofollow
external text
//doi.org/10.1086/524012

values:
nofollow
external text
//arxiv.org/abs/1401.0720

values:
nofollow
external text
//arxiv.org/abs/1505.00269

values:
nofollow
external text
//doi.org/10.1093/mnras/stv2239

values:
nofollow
external text
//arxiv.org/abs/1108.4070

values:
nofollow
external text
//arxiv.org/abs/0811.1994

values:
nofollow
external text
//doi.org/10.1126/science.1166609

values:
nofollow
external text
//www.ncbi.nlm.nih.gov/pubmed/19008414

values:
nofollow
external text
//arxiv.org/abs/1104.3863

values:
nofollow
external text
//arxiv.org/abs/1312.3951

values:
nofollow
external text
//arxiv.org/abs/astro-ph/0111544

values:
nofollow
external text
//doi.org/10.1086/338770

values:
nofollow
external text
//doi.org/10.1002/2017GL073248

values:
nofollow
external text
//doi.org/10.1016/j.icarus.2014.12.017

values:
nofollow
external text
//arxiv.org/abs/1303.2649

values:
nofollow
external text
//doi.org/10.1126/science.340.6132.565

values: -moz-column-width: 30em; -webkit-column-width: 30em; column-width: 30em; list-style-type: decimal;

values:
/wiki/Distant_Wanderers_(book)
mw-redirect
Distant Wanderers (book)

values:
nofollow
external text
//arxiv.org/abs/1401.8103

values:
nofollow
external text
//arxiv.org/archive/astro-ph.GA

values:
nofollow
http://www.exoplanet.eu/
external text

values:
nofollow
http://www.openexoplanetcatalogue.com/
external text

values:
nofollow
http://media4.obspm.fr/exoplanets/
external text

values:
nofollow
http://exographs.net/
external text

values:
*_Planet
**_Definition
***_IAU
*_Planetary_science

values:
/wiki/Ultra-short_period_planets
mw-redirect
Ultra-short period planets

values:
/wiki/Interstellar_comet
mw-redirect
Interstellar comet

values: List of exoplanets detected by microlensing

values: List of exoplanets detected by radial velocity

values: List of nearest terrestrial exoplanet candidates

values: List of exoplanets discovered using the Kepler spacecraft

values: List of potentially habitable exoplanets

values: List of exoplanets discovered before 2000

values: List of exoplanets discovered between 2000–2009

values: nowraplinks hlist collapsible autocollapse navbox-inner mw-collapsible mw-made-collapsible mw-collapsed

values: navigation navbox Exoplanetology padding:3px

values: Swiss 1.2-metre Leonhard Euler Telescope

values: Fiber-optic Improved Next-generation Doppler Search for Exo-Earths

values: Miniature Exoplanet Radial Velocity Array

values: Microlensing Observations in Astrophysics

values: New Mexico Exoplanet Spectroscopic Survey Instrument

values: Optical Gravitational Lensing Experiment

values: PRL Advanced Radial-velocity All-sky Search

values: Strategic Explorations of Exoplanets and Disks with Subaru

values: Search for extraterrestrial intelligence

values: Spectro-Polarimetric High-Contrast Exoplanet Research

values: Systemic (amateur extrasolar planet search project)

values:
navbox-image
2
width:1px;padding:0px 0px 0px 2px

values: Sagittarius Window Eclipsing Extrasolar Planet Search

values: Advanced Technology Large-Aperture Space Telescope

values: Exoplanetary Circumstellar Environments and Disk Explorer

values: Fast Infrared Exoplanet Spectroscopy Survey Explorer

values:
noprint metadata navbox
navigation
Portals
font-weight:bold;padding:0.4em 2em

attrs: alt src width height style srcset data-file-width data-file-height

values:
nofollow
external text
https://d-nb.info/gnd/4456110-6

values:
nofollow
external text
https://www.idref.fr/035322225

values: Category:Search for extraterrestrial intelligence

values: Category:Use dmy dates from February 2015

values: Category:Wikipedia articles with BNF identifiers

values: Category:Wikipedia articles with GND identifiers

values: Category:Wikipedia articles with SUDOC identifiers

values: Category:Articles containing video clips

values: Discussion about edits from this IP address [ctrl-alt-n]

values: A list of edits made from this IP address [ctrl-alt-y]

values: You are encouraged to create an account and log in; however, it is not mandatory

values: You're encouraged to log in; however, it's not mandatory. [ctrl-alt-o]

values:
/wiki/Exoplanet
View the content page [ctrl-alt-c]
c

values: Discussion about the content page [ctrl-alt-t]

values: p-namespaces navigation vectorTabs p-namespaces-label

values:
p-variants
navigation
vectorMenu emptyPortlet
p-variants-label

values: Past revisions of this page [ctrl-alt-h]

values: p-views navigation vectorTabs p-views-label

values:
p-cactions
navigation
vectorMenu emptyPortlet
p-cactions-label

values:
mw-wiki-logo
/wiki/Main_Page
Visit the main page

values:
/wiki/Main_Page
Visit the main page [ctrl-alt-z]
z

values: Featured content – the best of Wikipedia

values: Find background information on current events

values:
/wiki/Special:Random
Load a random article [ctrl-alt-x]
x

values: portal navigation p-navigation p-navigation-label

values: Guidance on how to use and edit Wikipedia

values: About the project, what you can do, where to find things

values: A list of recent changes in the wiki [ctrl-alt-r]

values: portal navigation p-interaction p-interaction-label

values: List of all English Wikipedia pages containing links to this page [ctrl-alt-j]

values: Recent changes in pages linked from this page [ctrl-alt-k]

values:
/wiki/Wikipedia:File_Upload_Wizard
Upload files [ctrl-alt-u]
u

values: A list of all special pages [ctrl-alt-q]

values: Permanent link to this revision of the page

values: Link to connected data repository item [ctrl-alt-g]

values: Printable version of this page [ctrl-alt-p]

values: portal navigation p-wikibase-otherprojects p-wikibase-otherprojects-label

values:
interlanguage-link interwiki-af
display: none;

values: كوكب خارج المجموعة الشمسية – Arabic

values:
interlanguage-link interwiki-ar
display: none;

values:
interlanguage-link interwiki-ast
display: none;

values:
interlanguage-link interwiki-az
display: none;

values: বহির্গ্রহ – Bangla

values:
interlanguage-link interwiki-bn
display: none;

values: Экзапланета – Belarusian

values:
interlanguage-link interwiki-be
display: none;

values: Экзаплянэта – Belarusian (Taraškievica orthography)

values:
interlanguage-link interwiki-be-x-old
display: none;

values: Екзопланета – Bulgarian

values:
interlanguage-link interwiki-bg
display: none;

values:
interlanguage-link interwiki-bs
display: none;

values:
interlanguage-link interwiki-br
display: none;

values:
interlanguage-link interwiki-ca
display: none;

values: Экзопланета – Chuvash

values:
interlanguage-link interwiki-cv
display: none;

values:
interlanguage-link interwiki-cs
display: none;

values:
interlanguage-link interwiki-cy
display: none;

values:
https://da.wikipedia.org/wiki/Exoplanet
Exoplanet – Danish
da
da
interlanguage-link-target

values:
interlanguage-link interwiki-da
display: none;

values:
https://de.wikipedia.org/wiki/Exoplanet
Exoplanet – German
de
de
interlanguage-link-target

values:
interlanguage-link interwiki-de
display: none;

values:
interlanguage-link interwiki-et
display: none;

values: Εξωηλιακός πλανήτης – Greek

values:
interlanguage-link interwiki-el
display: none;

values: interlanguage-link interwiki-es badge-Q17437798 badge-goodarticle

values:
interlanguage-link interwiki-eo
display: none;

values:
interlanguage-link interwiki-ext
display: none;

values:
interlanguage-link interwiki-eu
display: none;

values: سیاره فراخورشیدی – Persian

values:
interlanguage-link interwiki-fa
display: none;

values:
interlanguage-link interwiki-fr
display: none;

values:
interlanguage-link interwiki-ga
display: none;

values:
interlanguage-link interwiki-gl
display: none;

values: interlanguage-link interwiki-ko badge-Q17437798 badge-goodarticle

values: Էկզոմոլորակ – Armenian

values:
interlanguage-link interwiki-hy
display: none;

values: बहिर्ग्रह – Hindi

values:
interlanguage-link interwiki-hi
display: none;

values:
interlanguage-link interwiki-hr
display: none;

values:
interlanguage-link interwiki-io
display: none;

values:
interlanguage-link interwiki-id
display: none;

values:
interlanguage-link interwiki-is
display: none;

values:
interlanguage-link interwiki-it
display: none;

values: כוכב לכת חוץ-שמשי – Hebrew

values:
interlanguage-link interwiki-jv
display: none;

values: ಸೌರಾತೀತ ಗ್ರಹ – Kannada

values:
interlanguage-link interwiki-kn
display: none;

values: ეგზოპლანეტა – Georgian

values: interlanguage-link interwiki-ka badge-Q17437796 badge-featuredarticle

values: Экзопланета – Kazakh

values:
interlanguage-link interwiki-kk
display: none;

values:
interlanguage-link interwiki-sw
display: none;

values: Экзопланет – Komi

values:
interlanguage-link interwiki-kv
display: none;

values: interlanguage-link interwiki-la badge-Q17437796 badge-featuredarticle

values:
interlanguage-link interwiki-lv
display: none;

values:
interlanguage-link interwiki-lt
display: none;

values:
interlanguage-link interwiki-li
display: none;

values: interlanguage-link interwiki-hu badge-Q17437796 badge-featuredarticle

values: Вонсончева планета – Macedonian

values:
interlanguage-link interwiki-mk
display: none;

values: സൗരയൂഥേതരഗ്രഹം – Malayalam

values:
interlanguage-link interwiki-ml
display: none;

values: परग्रह – Marathi

values:
interlanguage-link interwiki-mr
display: none;

values:
interlanguage-link interwiki-ms
display: none;

values: နေစကြာဝဠာပြင်ပဂြိုဟ် – Burmese

values:
interlanguage-link interwiki-my
display: none;

values:
interlanguage-link interwiki-ja
display: none;

values:
interlanguage-link interwiki-no
display: none;

values:
interlanguage-link interwiki-nn
display: none;

values:
interlanguage-link interwiki-oc
display: none;

values:
interlanguage-link interwiki-uz
display: none;

values: سورجوں پرے پاندھی – Western Punjabi

values:
interlanguage-link interwiki-pnb
display: none;

values:
interlanguage-link interwiki-pt
display: none;

values: Экзопланета – Russian

values:
interlanguage-link interwiki-ru
display: none;

values:
interlanguage-link interwiki-sco
display: none;

values:
interlanguage-link interwiki-sq
display: none;

values: interlanguage-link interwiki-scn badge-Q17437796 badge-featuredarticle

values: බහිෂ්-සෞර ග්‍රහ ලෝකය – Sinhala

values:
interlanguage-link interwiki-si
display: none;

values:
interlanguage-link interwiki-sl
display: none;

values: Екстрасоларне планете – Serbian

values:
interlanguage-link interwiki-sr
display: none;

values:
interlanguage-link interwiki-sh
display: none;

values: interlanguage-link interwiki-fi badge-Q17559452 badge-recommendedarticle

values:
https://sv.wikipedia.org/wiki/Exoplanet
Exoplanet – Swedish
sv
sv
interlanguage-link-target

values: interlanguage-link interwiki-sv badge-Q17559452 badge-recommendedarticle

values:
interlanguage-link interwiki-tl
display: none;

values: புறக்கோள் – Tamil

values:
interlanguage-link interwiki-ta
display: none;

values: Экзопланета – Tatar

values:
interlanguage-link interwiki-tt
display: none;

values: ดาวเคราะห์นอกระบบ – Thai

values: interlanguage-link interwiki-th badge-Q17437796 badge-featuredarticle

values: Екзопланета – Ukrainian

values:
interlanguage-link interwiki-uk
display: none;

values: بیرونی سیارہ – Urdu

values:
interlanguage-link interwiki-ur
display: none;

values: Hành tinh ngoài hệ Mặt Trời – Vietnamese

values:
interlanguage-link interwiki-war
display: none;

values:
interlanguage-link interwiki-zh-yue
display: none;

values: 太陽系外行星 – Chinese

values:
interlanguage-link interwiki-zh
display: none;

values: Planetas estrasolal – Lingua Franca Nova

values:
interlanguage-link interwiki-lfn
display: none;

values: mediawiki ltr sitedir-ltr mw-hide-empty-elt ns-0 ns-subject page-Exoplanet rootpage-Exoplanet skin-vector action-view