سیارهٔ فراخورشیدی یا سیارهٔ غیرخورشیدی (به انگلیسی: Exoplanet یا Extrasolar planet) سیاره‌ای است که بیرون از منظومهٔ خورشیدی قرار دارد و به دور یک ستاره (غیر از خورشید) در حال گردش است. نخستین شناسایی علمی وجود یک سیارهٔ فراخورشیدی در سال ۱۹۸۸ انجام شد، با این حال، نخستین تأیید در سال ۱۹۹۲ صورت گرفت. از آن به بعد، و تا اول مهٔ ۲۰۱۷، شمار سیارگان فراخورشیدی شناسایی‌شده ۳٬۶۰۸ سیاره بوده که ۲٬۷۰۲ سیاره در ۶۱۰ سامانهٔ سیاره‌ای مختلف، تأیید شده‌اند[۱] و این تعداد روز به روز در حال افزایش است.[۲][۳]
مطالعهٔ سیاره‌های فراخورشیدی جزو موضوعات نوین در دانش اخترشناسی است و شامل دو شاخهٔ کلی کشف و شخصیت‌پردازی این‌گونه سیاره‌ها می‌شود. نخستین سیارهٔ فراخورشیدی در اوایل دههٔ ۹۰ میلادی کشف شد و از سال ۲۰۰۲ افزون‌بر کشف، بررسی ویژگی‌های این سیاره‌ها نیز آغاز شد.
رصدهای زمینی و فضایی سیارات فراخورشیدی به دو دلیل عمده کار چندان آسانی نیست. نخست اینکه سیارات به‌طور کلی نسبت به ستارگان اندازه‌های بسیار کوچکی دارند و سیارات فراخورشیدی در فاصله‌های بسیار دوری از زمین واقع‌اند. دیگر اینکه سیارات با ستارهٔ میزبان‌شان اختلاف درخشندگی فوق‌العاده زیادی دارند. وابسته به‌نوع ستاره، اندازه و دمای سیاره، ستاره می‌تواند از حدود ۱٬۰۰۰ تا یک میلیون برابر پرفروغ‌تر از سیاره‌های پیرامون خود باشد؛ بنابراین تفکیک نور بازتاب‌شده از سیاره از نور ستاره بسیار مشکل است. به عنوان یک تشبیه، رصد یک سیارهٔ غول‌پیکر مانند مشتری در مدار نزدیکترین ستاره‌ها به خورشید، مانند این‌ست که در تهران بایستیم و بخواهیم سر یک مورچه، که در جزیرهٔ کیش در حال راه رفتن در کنار یک نورافکن به شدت پرنور است را مشاهده کنیم!
با وجود تمام این سختی‌ها، اخترشناسان توانسته‌اند روش‌ها و ابزارهایی برای آشکارسازی و مطالعهٔ خصوصیات سیارات فراخورشیدی ابداع کنند. تاکنون حدود شش روش آشکارسازی یافت شده که به‌استثنای یکی، در بقیه سیاره به‌روش غیرمستقیم بررسی می‌شود.
روش تصویربرداری مستقیم:
روش تصویربرداری مستقیم، تنها روشی است که در آن سیاره به‌طور مستقیم رصد می‌شود.
این روش برای سیاره‌های جوان و داغی مناسب است که به‌اندازهٔ کافی از ستارهٔ میزبان خود دور هستند. تعداد سیاره‌هایی که با این روش کشف شده‌اند زیاد نیست. در حال حاضر با پیشرفت روش‌های کرونوگرافی استفاده از این روش در حال افزایش است.
در باقی روش‌ها سیارهٔ فراخورشیدی به‌طور مستقیم دیده نمی‌شود و تنها می‌توان با رصد ستارهٔ میزبان و مشاهدهٔ تأثیرات گرانشی یا تغییرات نوری‌ای که سیاره بر روی آن می‌گذارد، به‌طور غیرمستقیم، به‌وجود سیاره پی برد.
روش سرعت شعاعی:
تاکنون سرعت شعاعی موفق‌ترین روش در کشف سیاره‌های فراخورشیدی بوده‌است. حدود نیمی از آن‌ها با این روش کشف شده‌اند. در یک سیستم ستاره‌ای، این تنها سیاره نیست که در حال حرکت در مدارش است، بلکه ستاره و سیاره، هر دو به دور مرکز جرم مشترکشان در حال گردش هستند. چون مرکز جرم این سیستم به مرکز ستاره بسیار نزدیک‌است، مدار ستاره بسیار کوچک است که موجب حرکت نوسانی ریزی در ستاره می‌شود. این حرکت نوسانی باعث ایجاد پدیدهٔ داپلر می‌شود و با اندازه‌گیری انتقال به سرخ در طیف ستاره قابل اندازه‌گیری‌است.
این روش برای سیاره‌های سنگین و بزرگی مناسب‌است که به ستارهٔ میزبان خود بسیار نزدیک هستند.
روش گذر:
اساس این روش مانند مطالعهٔ ستاره‌های دوتایی گرفتی است. در برخی موارد، هنگامی که زاویهٔ اینکلینشن مدار نزدیک به ۹۰ درجه است، پدیدهٔ گذر روی می‌دهد که در آن سیاره از دید ما از روی دیسک ستارهٔ میزبان عبور می‌کند. در نتیجهٔ این گذر، مقداری از نور ستاره مسدود می‌شود و روشنایی ظاهری ستاره اندکی تغییر می‌کند. اگر در اندازه‌گیری‌های فتومتری، تغییر نوری در ستاره ایجاد شود، می‌تواند مدرکی از وجود یک سیاره در اطراف آن باشد. هرچند برای تأیید قطعی کشف سیاره، به رصدهای پشتیبان نیاز است. روش گذر دومین روش موفق در کشف سیارات فراخورشیدی و نیز نخستین متد موفق در بررسی ویژگی‌های سیارات است.
بسیاری از آن‌ها بزرگ‌تر از سیارهٔ مشتری هستند. در سال‌های اخیر با بهبود فناوری رصدی، ۱۳ سیارهٔ فراخورشیدی هم‌اندازه با کرهٔ زمین نیز کشف شده‌است.[۲]
در میان سیاره‌های فراخورشیدی نمونه‌های شگرفی دیده می‌شوند، برای نمونه سیاره‌ای مشابه به سیاره کوروت- ۷بی (COROT-7b) در ۲۶۰ سال نوری از زمین وجود دارد که سرعت گردش آن به دور ستارهٔ مادر چنان بالاست که هر سال در این سیاره تنها سه روز به درازا می‌کشد.[۴]
دانشمندان بر این باورند که سیاره‌های بیشماری بوده یا هستند که توسط ستارهٔ خود فرو بلعیده شده یا از مدار و منظومه خود به بیرون پرت شده و در فضای خالی سرگردان گشته‌اند.[۴]
ستاره‌شناسان مأموریت کپلر می‌گویند سیاره‌ای فراخورشیدی همانند زمین موجود است که در منطقه قابل سکونت ستارهٔ خود قراردارد. دانشمندان می‌گویند این سیاره که به اسم کپلر ۶۹سی نامیده شده همانند سیاره‌های سامانه خورشیدی در مداری ویژه پیرامون ستاره‌ای می‌چرخد. این سیارهٔ فراخورشیدی احتمالاً نخستین سیاره‌ای‌است که در آن زندگی خارج از زمین وجود دارد.[۷]
در سال ۱۹۹۲ یک ستارهشناسلهستانی به نام الکساندر وُلستکان، نخستین سیارهٔ فراخورشیدی را در پیرامون تپ اختر PSR 1257+12 کشف کرد. این کشف سریعاً مورد تأیید قرار گرفت و به عنوان نخستین کشف سیارهٔ فراخورشیدی تأیید شده، شناخته شد. سیارهٔ بعدی در ۶ اکتبر ۱۹۹۵ توسط تیمی به سرپرستی میشل مایور از دانشگاه ژنو، به دور ستارهٔ رشته اصلی، ۵۱ پگاسوس صورت گرفت.
حروف کوچک b بعد از نام ستاره، برای نامگذاری اولین سیارهٔ آن سیستم است مانند (۵۱ Pegasi b). برای نامگذاری دومین سیارهٔ کشف شده در یک سیستم، از حرف کوچک (c) استفاده می‌شود، مانند، (۵۱pegasi c)و سومین سیارهٔ کشف شده آن سیستم (۵۱pegasi d) و به همین ترتیب. از حرف a استفاده نمی‌شود زیرا به خود ستاره بر می‌گردد.
ترتیب حروف کوچک … ,a,b,c به ترتیب زمان کشف، بر روی سیارات یک سیستم گذاشته می‌شود نه به ترتیب نزدیکی به ستاره. به‌طور مثال در سیستم Gliese 876 نزدیکترین سیاره به آن Gliese 876 d می‌باشد. قبل از کشف ۵۱pegasi b سیارگان فراخورشیدی به ترتیب نزدیکی به ستارهٔ مادر نامگذاری می‌شدند: برای مثال PSR1257+12 c و PSR1257+12 b :کشف شدند PSR۱۲۵۷+۱۲ اولین سیاره‌هایی که اطراف تپ اختر بودند. سیارهٔ نزدیکتری که بعداً کشف شد، PSR1257+12 a نام گرفت نه PSR1257+12 d. بعضی از سیاره‌های فراخورشیدی نیز اسم‌های مستعار دارند. به‌طور مثال HD 209458 b، اوزیریس و 51 Pegasi b، بلروفون نام دارند.
↑ ۲٫۰۲٫۱Ferris, Timothy. 2009. "Searching for New Earths - Distant worlds are being discovered. Is one of them like ours?" National Geographic. 216 (6): 78.
Four exoplanets orbiting counterclockwise with their host star (HR 8799).
An exoplanet or extrasolar planet is a planet outside the Solar System. The first possible evidence of an exoplanet was noted in 1917 but was not recognized as such.[1] The first confirmation of detection occurred in 1992. A different planet, initially detected in 1988, was confirmed in 2003. As of 1 December 2022, there are 5,284 confirmed exoplanets in 3,899 planetary systems, with 847 systems having more than one planet.[2][3]
There are many methods of detecting exoplanets. Transit photometry and Doppler spectroscopy have found the most, but these methods suffer from a clear observational bias favoring the detection of planets near the star; thus, 85% of the exoplanets detected are inside the tidal locking zone.[4] In several cases, multiple planets have been observed around a star.[5] About 1 in 5 Sun-like stars[a] have an "Earth-sized"[b] planet in the habitable zone.[c][6][7] Assuming there are 200 billion stars in the Milky Way,[d] it can be hypothesized 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.[8]
The least massive exoplanet 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 exoplanet listed on the NASA Exoplanet Archive is HR 2562 b,[9][10][11] about 30 times the mass of Jupiter. However, according to some definitions of a planet (based on the nuclear fusion of deuterium[12]), it is too massive to be a planet and might be a brown dwarf instead. Known orbital times for exoplanets vary from less than an hour (for those closest to their star) to thousands of years. Some exoplanets are so far away from the star that it is difficult to tell whether they are gravitationally bound to it.
Almost all of the planets detected so far are within the Milky Way. However, there is evidence that extragalactic planets, exoplanets farther away in galaxies beyond the local Milky Way galaxy, may exist.[13][14] The nearest exoplanets are located 4.2 light-years (1.3 parsecs) from Earth and orbit Proxima Centauri, the closest star to the Sun.[15]
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 (or sometimes called "goldilocks zone"), where it is possible for liquid water, a prerequisite for life as we know it, to exist on the surface. However, the study of planetary habitability also considers a wide range of other factors in determining the suitability of a planet for hosting life.[16]
Rogue planets are those that do not orbit any star. Such objects are considered a separate category of planets, especially if they are gas giants, often counted as sub-brown dwarfs.[17] The rogue planets in the Milky Way possibly number in the billions or more.[18][19]
The official definition of the term planet used by the International Astronomical Union (IAU) only covers the Solar System and thus does not apply to exoplanets.[20][21] The IAU Working Group on Extrasolar Planets issued a position statement containing a working definition of "planet" in 2001 and which was modified in 2003.[22] An exoplanet was defined by the following criteria:
Objects with true masses below the limiting mass for thermonuclear fusion of deuterium (currently calculated to be 13 Jupiter masses for objects of solar metallicity) that orbit stars or stellar remnants are "planets" (no matter how they formed). The minimum mass/size required for an extrasolar object to be considered a planet should be the same as that used in the Solar System.
Substellar objects with true masses above the limiting mass for thermonuclear fusion of deuterium are "brown dwarfs", no matter how they formed or where they are located.
Free-floating objects in young star clusters with masses below the limiting mass for thermonuclear fusion of deuterium are not "planets", but are "sub-brown dwarfs" (or whatever name is most appropriate).
This working definition was amended by the IAU's Commission F2: Exoplanets and the Solar System in August 2018.[23][24] The official working definition of an exoplanet is now as follows:
Objects with true masses below the limiting mass for thermonuclear fusion of deuterium (currently calculated to be 13 Jupiter masses for objects of solar metallicity) that orbit stars, brown dwarfs or stellar remnants and that have a mass ratio with the central object below the L4/L5 instability (M/Mcentral < 2/(25+√621)) are "planets" (no matter how they formed).
The minimum mass/size required for an extrasolar object to be considered a planet should be the same as that used in our Solar System.
The IAU noted that this definition could be expected to evolve as knowledge improves.
Alternatives
The IAU's working definition is not always used. One alternate suggestion is that planets should be distinguished from brown dwarfs on the basis of formation. It is widely thought that giant planets form through core accretion, which may sometimes produce planets with masses above the deuterium fusion threshold;[25][26][12] massive planets of that sort may have already been observed.[27] Brown dwarfs form like stars from the direct gravitational collapse of clouds of gas and this formation mechanism also produces objects that are below the 13MJup limit and can be as low as 1MJup.[28] Objects in this mass range that orbit their stars with wide separations of hundreds or thousands of AU and have large star/object mass ratios likely formed as brown dwarfs; their atmospheres would likely have a composition more similar to their host star than accretion-formed planets which would contain increased abundances of heavier elements. Most directly imaged planets as of April 2014 are massive and have wide orbits so probably represent the low-mass end of brown dwarf formation.[29]
One study suggests that objects above 10MJup formed through gravitational instability and should not be thought of as planets.[30]
Also, the 13-Jupiter-mass cutoff does not have precise physical significance. Deuterium fusion can occur in some objects with a mass below that cutoff.[12] The amount of deuterium fused depends to some extent on the composition of the object.[31] As of 2011 the Extrasolar Planets Encyclopaedia included objects up to 25 Jupiter masses, saying, "The fact that there is no special feature around 13MJup in the observed mass spectrum reinforces the choice to forget this mass limit".[32]
As of 2016 this limit was increased to 60 Jupiter masses[33] based on a study of mass–density relationships.[34]
The Exoplanet Data Explorer includes objects up to 24 Jupiter masses with the advisory: "The 13 Jupiter-mass distinction by the IAU Working Group is physically unmotivated for planets with rocky cores, and observationally problematic due to the sin i ambiguity."[35]
The NASA Exoplanet Archive includes objects with a mass (or minimum mass) equal to or less than 30 Jupiter masses.[36]
Another criterion for separating planets and brown dwarfs, rather than deuterium fusion, formation process or location, is whether the core pressure is dominated by coulomb pressure or electron degeneracy pressure with the dividing line at around 5 Jupiter masses.[37][38]
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 IAU designation is formed by taking the designated or proper name of its parent star, and adding a lower case letter.[40] Letters are given in order of each planet's discovery around the parent star, so that the first planet discovered in a system is designated "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
For centuries scientists, philosophers, and science fiction writers suspected that extrasolar planets existed, but there was no way of knowing whether they were real in fact, how common they were, 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 a possible exoplanet, orbiting Van Maanen 2, was noted in 1917, but was not recognized as such. The astronomer Walter Sydney Adams, who later became director of the Mount Wilson Observatory, produced a spectrum of the star using Mount Wilson's 60-inch telescope. He interpreted the spectrum to be of an F-type main-sequence star, but it is now thought that such a spectrum could be caused by the residue of a nearby exoplanet that had been pulverized into dust by the gravity of the star, the resulting dust then falling onto the star.[1]
The first suspected scientific detection of an exoplanet occurred in 1988. Shortly afterwards, the first confirmation of detection came in 1992, with the discovery of several terrestrial-mass planets orbiting the pulsarPSR B1257+12.[41] 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. In February 2018, researchers using the Chandra X-ray Observatory, combined with a planet detection technique called microlensing, found evidence of planets in a distant galaxy, 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."[42]
On 21st March 2022, the 5000th exoplanet beyond our solar system was confirmed.[43]
Early speculations
This space we declare to be infinite... In it are an infinity of worlds of the same kind as our own.
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."[45]
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.[46]
Discredited claims
Claims of exoplanet detections have been made since the nineteenth century. Some of the earliest involve the binary star70 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.[47] 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.[48] However, Forest Ray Moulton published a paper proving that a three-body system with those orbital parameters would be highly unstable.[49] 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.[50] Astronomers now generally regard all the early reports of detection as erroneous.[51]
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 December 2022, a total of 5,284 confirmed exoplanets are listed in the Extrasolar Planets Encyclopaedia, including a few that were confirmations of controversial claims from the late 1980s.[2] 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.[54] 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,[55] but subsequent work in 1992 again raised serious doubts.[56] Finally, in 2003, improved techniques allowed the planet's existence to be confirmed.[57]
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 pulsarPSR 1257+12.[41] 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.[58] 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. As pulsars are aggressive stars, it was considered unlikely at the time that a planet may be able to be formed in their orbit.[59]
In the early 1990s, a group of astronomers led by Donald Backer, who were studying what they thought was a binary pulsar (PSR B1620−26 b), determined that a third object was needed to explain the observed Doppler shifts. Within a few years, the gravitational effects of the planet on the orbit of the pulsar and white dwarf had been measured, giving an estimate of the mass of the third object that was too small for it to be a star. The conclusion that the third object was a planet was announced by Stephen Thorsett and his collaborators in 1993.[60]
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, nearby G-type star51 Pegasi.[61][62][63] This discovery, made at the Observatoire de Haute-Provence, ushered in the modern era of exoplanetary discovery, and was recognized by a share of the 2019 Nobel Prize in Physics. 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 transited in front of it.[61]
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.[61] In 1999, Upsilon Andromedae became the first main-sequence star known to have multiple planets.[64]Kepler-16 contains the first discovered planet that orbits around a binary main-sequence star system.[65]
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".[66][67][68] Before these results, most confirmed planets were gas giants comparable in size to Jupiter or larger because they are more easily detected, but the Kepler planets are mostly between the size of Neptune and the size of Earth.[66]
On 23 July 2015, NASA announced Kepler-452b, a near-Earth-size planet orbiting the habitable zone of a G2-type star.[69]
On 6 September 2018, NASA discovered an exoplanet about 145 light years away from Earth in the constellation Virgo.[70] This exoplanet, Wolf 503b, is twice the size of Earth and was discovered orbiting a type of star known as an "Orange Dwarf". Wolf 503b completes one orbit in as few as six days because it is very close to the star. Wolf 503b is the only exoplanet that large that can be found near the so-called Fulton gap. The Fulton gap, first noticed in 2017, is the observation that it is unusual to find planets within a certain mass range.[70] Under the Fulton gap studies, this opens up a new field for astronomers, who are still studying whether planets found in the Fulton gap are gaseous or rocky.[70]
In January 2020, scientists announced the discovery of TOI 700 d, the first Earth-sized planet in the habitable zone detected by TESS.[71]
Candidate discoveries
As of January 2020, NASA's Kepler and TESS missions had identified 4374 planetary candidates yet to be confirmed,[72] several of them being nearly Earth-sized and located in the habitable zone, some around Sun-like stars.[73][74][75]
Planets are extremely faint compared with their parent stars. For example, a Sun-like star is about a billion times brighter than the reflected light from any exoplanet orbiting it. It is difficult to detect such a faint light source, and furthermore the parent star causes a glare that tends to wash it out. It is necessary to block the light from the parent star in order to reduce the glare while leaving the light from the planet detectable; doing so is a major technical challenge which requires extreme optothermal stability.[82] All exoplanets that have been directly imaged are both large (more massive than Jupiter) and widely separated from their parent star.
Specially designed direct-imaging instruments such as Gemini Planet Imager, VLT-SPHERE, and SCExAO will image dozens of gas giants, but the vast majority of known extrasolar planets have only been detected through indirect methods.
When the star is behind a planet, its brightness will seem to dim
If a planet crosses (or transits) in front of its parent star's disk, then the observed brightness of the star drops by a small amount. The amount by which the star dims depends on its size and on the size of the planet, among other factors. Because the transit method requires that the planet's orbit intersect a line-of-sight between the host star and Earth, the probability that an exoplanet in a randomly oriented orbit will be observed to transit the star is somewhat small. The Kepler telescope used this method.
Exoplanet detections per year as of June 2022.[83]
As a planet orbits a star, the star also moves in its own small orbit around the system's center of mass. Variations in the star's radial velocity—that is, the speed with which it moves towards or away from Earth—can be detected from displacements in the star's spectral lines due to the Doppler effect. Extremely small radial-velocity variations can be observed, of 1 m/s or even somewhat less.[84]
When multiple planets are present, each one slightly perturbs the others' orbits. Small variations in the times of transit for one planet can thus indicate the presence of another planet, which itself may or may not transit. For example, variations in the transits of the planet Kepler-19b suggest the existence of a second planet in the system, the non-transiting Kepler-19c.[85][86]
Animation showing difference between planet transit timing of one-planet and two-planet systems
When a planet orbits multiple stars or if the planet has moons, its transit time can significantly vary per transit. Although no new planets or moons have been discovered with this method, it is used to successfully confirm many transiting circumbinary planets.[87]
Microlensing occurs when the gravitational field of a star acts like a lens, magnifying the light of a distant background star. Planets orbiting the lensing star can cause detectable anomalies in the magnification as it varies over time. Unlike most other methods which have detection bias towards planets with small (or for resolved imaging, large) orbits, microlensing method is most sensitive to detecting planets around 1–10 AU away from Sun-like stars.
Astrometry consists of precisely measuring a star's position in the sky and observing the changes in that position over time. The motion of a star due to the gravitational influence of a planet may be observable. Because the motion is so small, however, this method has not yet been very productive. It has produced only a few disputed detections, though it has been successfully used to investigate the properties of planets found in other ways.
A pulsar (the small, ultradense remnant of a star that has exploded as a supernova) emits radio waves extremely regularly as it rotates. If planets orbit the pulsar, they will cause slight anomalies in the timing of its observed radio pulses. The first confirmed discovery of an extrasolar planet was made using this method. But as of 2011, it has not been very productive; five planets have been detected in this way, around three different pulsars.
Like pulsars, there are some other types of stars which exhibit periodic activity. Deviations from the periodicity can sometimes be caused by a planet orbiting it. As of 2013, a few planets have been discovered with this method.[88]
When a planet orbits very close to the star, it catches a considerable amount of starlight. As the planet orbits around the star, the amount of light changes due to planets having phases from Earth's viewpoint or planet glowing more from one side than the other due to temperature differences.[89]
Relativistic beaming measures the observed flux from the star due to its motion. The brightness of the star changes as the planet moves closer or further away from its host star.[90]
Massive planets close to their host stars can slightly deform the shape of the star. This causes the brightness of the star to slightly deviate depending how it is rotated relative to Earth.[91]
With polarimetry method, a polarized light reflected off the planet is separated from unpolarized light emitted from the star. No new planets have been discovered with this method although a few already discovered planets have been detected with this method.[92][93]
Disks of space dust surround many stars, thought to originate from collisions among asteroids and comets. The dust can be detected because it absorbs starlight and re-emits it as infrared radiation. Features in the disks may suggest the presence of planets, though this is not considered a definitive detection method.
Planets may form within a few to tens (or more) of millions of years of their star forming.[94][95][96][97][98]
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[99] to planetary systems of over 10 Gyr old.[100] When planets form in a gaseous protoplanetary disk,[101] they accrete hydrogen/helium envelopes.[102][103] These envelopes cool and contract over time and, depending on the mass of the planet, some or all of the hydrogen/helium is eventually lost to space.[101] This means that even terrestrial planets may start off with large radii if they form early enough.[104][105][106] 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.[107]
Using data from Kepler, a correlation has been found between the metallicity of a star and the probability that the star hosts a giant planet, similar to the size of Jupiter. Stars with higher metallicity are more likely to have planets, especially giant planets, than stars with lower metallicity.[112]
Some planets orbit one member of a binary star system,[113] and several circumbinary planets have been discovered which orbit around both members of binary star. A few planets in triple star systems are known[114] and one in the quadruple system Kepler-64.
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.[115][116] Later that same year, the colors of several other exoplanets were determined, including GJ 504 b which visually has a magenta color,[117] and Kappa Andromedae b, which if seen up close would appear reddish in color.[118]Helium planets are expected to be white or grey in appearance.[119]
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.[120]
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.[121][122][123]
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.[124]
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.[124]
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.[124]
Magnetic field
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.[125][126]
The magnetic fields of exoplanets may be detectable by their auroralradio emissions with sensitive enough radio telescopes such as LOFAR.[127][128] The radio emissions could enable determination of the rotation rate of the interior of an exoplanet, and may yield a more accurate way to measure exoplanet rotation than by examining the motion of clouds.[129]
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.[130][131]
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 (Joule heating) 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.[132]
In August 2018, scientists announced the transformation of gaseous deuterium into a liquid metallic hydrogen form. This may help researchers better understand giant gas planets, such as Jupiter, Saturn and related exoplanets, since such planets are thought to contain a lot of liquid metallic hydrogen, which may be responsible for their observed powerful magnetic fields.[133][134]
Although scientists previously announced that the magnetic fields of close-in exoplanets may cause increased stellar flares and starspots on their host stars, in 2019 this claim was demonstrated to be false in the HD 189733 system. The failure to detect "star-planet interactions" in the well-studied HD 189733 system calls other related claims of the effect into question.[135]
In 2019 the strength of the surface magnetic fields of 4 hot Jupiters were estimated and ranged between 20 and 120 gauss compared to Jupiter's surface magnetic field of 4.3 gauss.[136][137]
Plate tectonics
In 2007, two independent teams of researchers came to opposing conclusions about the likelihood of plate tectonics on larger super-Earths[138][139] with one team saying that plate tectonics would be episodic or stagnant[140] and the other team saying that plate tectonics is very likely on super-Earths even if the planet is dry.[141]
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.[142][143]
Volcanism
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.[144][145]
Rings
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.[146][147]
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.[148]
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.[149]
Moons
In December 2013 a candidate exomoon of a rogue planet was announced.[150] On 3 October 2018, evidence suggesting a large exomoon orbiting Kepler-1625b was reported.[151]
Clear versus cloudy atmospheres on two exoplanets.[152]
Atmospheres have been detected around several exoplanets. The first to be observed was HD 209458 b in 2001.[153]
Sunset studies on Titan by Cassini help understand exoplanet atmospheres (artist's concept).
As of February 2014, more than fifty transiting and five directly imaged exoplanet atmospheres have been observed,[154] resulting in detection of molecular spectral features; observation of day–night temperature gradients; and constraints on vertical atmospheric structure.[155] Also, an atmosphere has been detected on the non-transiting hot Jupiter Tau Boötis b.[156][157]
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.[158][159] The technology used to determine this may be useful in studying the atmospheres of distant worlds, including those of exoplanets.
Comet-like tails
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.[160] 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.[161]
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 million km (9 million mi) long.[162]
Insolation pattern
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.[163] 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.[164] Planets with both an eccentric orbit and a tilted axis of rotation would have more complicated insolation patterns.[165]
Surface
Surface composition
Surface features can be distinguished from atmospheric features by comparing emission and reflection spectroscopy with transmission spectroscopy. Mid-infrared spectroscopy of exoplanets may detect rocky surfaces, and near-infrared may identify magma oceans or high-temperature lavas, hydrated silicate surfaces and water ice, giving an unambiguous method to distinguish between rocky and gaseous exoplanets.[166]
Surface temperature
Artist's illustration of temperature inversion in exoplanet's atmosphere.[167]
The temperature of an exoplanet can be estimated by measuring the intensity of the light it receives from its parent star. For example, the planet OGLE-2005-BLG-390Lb is estimated to have a surface temperature of roughly −220 °C (50 K). However, such estimates may be substantially in error because they depend on the planet's usually unknown albedo, and because factors such as the greenhouse effect may introduce unknown complications. A few planets have had their temperature measured by observing the variation in infrared radiation as the planet moves around in its orbit and is eclipsed by its parent star. For example, the planet HD 189733b has been estimated to have an average temperature of 1,205 K (932 °C) on its dayside and 973 K (700 °C) on its nightside.[168]
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.[169] 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).[169] 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.[170] 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.[171][172]
The habitable zone around a star is the region where the temperature is just right to allow liquid water to exist on the surface of planet; that is, not too close to the star for the water to evaporate and not too far away from the star for the water to freeze. The heat produced by stars varies depending on the size and age of the star, so that the habitable zone can be at different distances for different stars. Also, the atmospheric conditions on the planet influence the planet's ability to retain heat so that the location of the habitable zone is also specific to each type of planet: desert planets (also known as dry planets), with very little water, will have less water vapor in the atmosphere than Earth and so have a reduced greenhouse effect, meaning that a desert planet could maintain oases of water closer to its star than Earth is to the Sun. The lack of water also means there is less ice to reflect heat into space, so the outer edge of desert-planet habitable zones is further out.[173][174] Rocky planets with a thick hydrogen atmosphere could maintain surface water much further out than the Earth–Sun distance.[175] Planets with larger mass have wider habitable zones because the gravity reduces the water cloud column depth which reduces the greenhouse effect of water vapor, thus moving the inner edge of the habitable zone closer to the star.[176]
Planetary rotation rate is one of the major factors determining the circulation of the atmosphere and hence the pattern of clouds: slowly rotating planets create thick clouds that reflect more and so can be habitable much closer to their star. Earth with its current atmosphere would be habitable in Venus's orbit, if it had Venus's slow rotation. If Venus lost its water ocean due to a runaway greenhouse effect, it is likely to have had a higher rotation rate in the past. Alternatively, Venus never had an ocean because water vapor was lost to space during its formation [177] and could have had its slow rotation throughout its history.[178]
Tidally locked planets (a.k.a. "eyeball" planets[179]) can be habitable closer to their star than previously thought due to the effect of clouds: at high stellar flux, strong convection produces thick water clouds near the substellar point that greatly increase the planetary albedo and reduce surface temperatures.[180]
Habitable zones have usually been defined in terms of surface temperature, however over half of Earth's biomass is from subsurface microbes,[181] and the temperature increases with depth, so the subsurface can be conducive for microbial life when the surface is frozen and if this is considered, the habitable zone extends much further from the star,[182] even rogue planets could have liquid water at sufficient depths underground.[183] In an earlier era of the universe the temperature of the cosmic microwave background would have allowed any rocky planets that existed to have liquid water on their surface regardless of their distance from a star.[184] Jupiter-like planets might not be habitable, but they could have habitable moons.[185]
The outer edge of the habitable zone is where planets are completely frozen, but planets well inside the habitable zone can periodically become frozen. If orbital fluctuations or other causes produce cooling then this creates more ice, but ice reflects sunlight causing even more cooling, creating a feedback loop until the planet is completely or nearly completely frozen. When the surface is frozen, this stops carbon dioxide weathering, resulting in a build-up of carbon dioxide in the atmosphere from volcanic emissions. This creates a greenhouse effect which thaws the planet again. Planets with a large axial tilt[186] are less likely to enter snowball states and can retain liquid water further from their star. Large fluctuations of axial tilt can have even more of a warming effect than a fixed large tilt.[187][188] Paradoxically, planets orbiting cooler stars, such as red dwarfs, are less likely to enter snowball states because the infrared radiation emitted by cooler stars is mostly at wavelengths that are absorbed by ice which heats it up.[189][190]
Tidal heating
If a planet has an eccentric orbit, then tidal heating can provide another source of energy besides stellar radiation. This means that eccentric planets in the radiative habitable zone can be too hot for liquid water. Tides also circularize orbits over time so there could be planets in the habitable zone with circular orbits that have no water because they used to have eccentric orbits.[191] Eccentric planets further out than the habitable zone would still have frozen surfaces but the tidal heating could create a subsurface ocean similar to Europa's.[192] In some planetary systems, such as in the Upsilon Andromedae system, the eccentricity of orbits is maintained or even periodically varied by perturbations from other planets in the system. Tidal heating can cause outgassing from the mantle, contributing to the formation and replenishment of an atmosphere.[193]
A review in 2015 identified exoplanets Kepler-62f, Kepler-186f and Kepler-442b as the best candidates for being potentially habitable.[194] These are at a distance of 1200, 490 and 1,120 light-years away, respectively. Of these, Kepler-186f is in similar size to Earth with its 1.2-Earth-radius measure, and it is located towards the outer edge of the habitable zone around its red dwarf star.
When looking at the nearest terrestrial exoplanet candidates, Proxima Centauri b is about 4.2 light-years away. Its equilibrium temperature is estimated to be −39 °C (234 K).[195]
In November 2013 it was estimated that 22±8% of Sun-like[a] stars in the Milky Way galaxy may have an Earth-sized[b] planet in the habitable[c] zone.[6][109] Assuming 200 billion stars in the Milky Way,[d] that would be 11 billion potentially habitable Earths, rising to 40 billion if red dwarfs are included.[8]
Kepler-186f, a 1.2-Earth-radius planet in the habitable zone of a red dwarf, reported in April 2014.
Proxima Centauri b, a planet in the habitable zone of Proxima Centauri, the nearest known star to the solar system with an estimated minimum mass of 1.27 times the mass of the Earth.
In February 2013, researchers speculated that up to 6% of small red dwarfs may have Earth-size planets. This suggests that the closest one to the Solar System could be 13 light-years away. The estimated distance increases to 21 light-years when a 95% confidence interval is used.[196] In March 2013 a revised estimate gave an occurrence rate of 50% for Earth-size planets in the habitable zone of red dwarfs.[197]
CoRoT - Mission to look for exoplanets using the transit method.
Kepler - Mission to look for large numbers of exoplanets using the transit method.
TESS - To search for new exoplanets; rotating so by the end of its two-year mission it will have observed stars from all over the sky. It is expected to find at least 3,000 new exoplanets.
ESPRESSO - A rocky planet-finding, and stable spectroscopic observing, spectrograph mounted on ESO's 4 by 8.2m VLT telescope, sited on the levelled summit of Cerro Paranal in the Atacama Desert of northern Chile.
ANDES - The ArmazoNes high Dispersion Echelle Spectrograph, a planet finding and planet characterisation spectrograph, is expected to be fitted onto ESO's ELT 39.3m telescope. ANDES was formally known as HIRES, which itself was created after a merger of the consortia behind the earlier CODEX (optical high-resolution) and SIMPLE (near-infrared high-resolution) spectrograph concepts.
Notes
^ abcFor 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.
^ abcFor the purpose of this 1 in 5 statistic, Earth-sized means 1–2 Earth radii.
^ abFor 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).
^ abAbout 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 have Earth-sized planets in the habitable zone. Including red dwarfs would increase this to 40 billion.
^ abCassan, 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. PMID22237108. S2CID2614136.
^Maire, A.; Rodet, L.; Lazzoni, C.; Boccaletti, A.; Brandner, W.; Galicher, R.; Cantalloube, F.; Mesa, D.; Klahr, H.; Beust, H.; Chauvin, G.; Desidera, S.; Janson, M.; Keppler, M.; Olofsson, J.; Augereau, J.; Daemgen, S.; Henning, T.; Thébault, P.; Bonnefoy, M.; Feldt, M.; Gratton, R.; Lagrange, A.; Langlois, M.; Meyer, M. R.; Vigan, A.; D’Orazi, V.; Hagelberg, J.; Le Coroller, H.; Ligi, R.; Rouan, D.; Samland, M.; Schmidt, T.; Udry, S.; Zurlo, A.; Abe, L.; Carle, M.; Delboulbé, A.; Feautrier, P.; Magnard, Y.; Maurel, D.; Moulin, T.; Pavlov, A.; Perret, D.; Petit, C.; Ramos, J. R.; Rigal, F.; Roux, A.; Weber, L. (2018). "VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B". Astronomy & Astrophysics. 615: A177. arXiv:1804.04584. Bibcode:2018A&A...615A.177M. doi:10.1051/0004-6361/201732476.
^ abcBodenheimer, Peter; D'Angelo, Gennaro; Lissauer, Jack J.; Fortney, Jonathan J.; Saumon, Didier (2013). "Deuterium Burning in Massive Giant Planets and Low-mass Brown Dwarfs Formed by Core-nucleated Accretion". The Astrophysical Journal. 770 (2): 120. arXiv:1305.0980. Bibcode:2013ApJ...770..120B. doi:10.1088/0004-637X/770/2/120. S2CID118553341.
^Kumar, Shiv S. (2003). "Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?". Brown Dwarfs. 211: 532. Bibcode:2003IAUS..211..529B.
^Brandt, T. D.; McElwain, M. W.; Turner, E. L.; Mede, K.; Spiegel, D. S.; Kuzuhara, M.; Schlieder, J. E.; Wisniewski, J. P.; Abe, L.; Biller, B.; Brandner, W.; Carson, J.; Currie, T.; Egner, S.; Feldt, M.; Golota, T.; Goto, M.; Grady, C. A.; Guyon, O.; Hashimoto, J.; Hayano, Y.; Hayashi, M.; Hayashi, S.; Henning, T.; Hodapp, K. W.; Inutsuka, S.; Ishii, M.; Iye, M.; Janson, M.; Kandori, R.; et al. (2014). "A Statistical Analysis of Seeds and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?". The Astrophysical Journal. 794 (2): 159. arXiv:1404.5335. Bibcode:2014ApJ...794..159B. doi:10.1088/0004-637X/794/2/159. S2CID119304898.
^Wright, J. T.; Fakhouri, O.; Marcy, G. W.; Han, E.; Feng, Y.; Johnson, John Asher; Howard, A. W.; Fischer, D. A.; Valenti, J. A.; Anderson, J.; Piskunov, N. (2010). "The Exoplanet Orbit Database". Publications of the Astronomical Society of the Pacific. 123 (902): 412–422. arXiv:1012.5676. Bibcode:2011PASP..123..412W. doi:10.1086/659427. S2CID51769219.
^Newton, Isaac; I. Bernard Cohen; Anne Whitman (1999) [1713]. The Principia: A New Translation and Guide. University of California Press. p. 940. ISBN978-0-520-08816-0.
^Struve, Otto (1952). "Proposal for a project of high-precision stellar radial velocity work". The Observatory. 72: 199–200. Bibcode:1952Obs....72..199S.
^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.
^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.
^Rodriguez Baquero, Oscar Augusto (2017). La presencia humana más allá del sistema solar [Human presence beyond the solar system] (in Spanish). RBA. p. 29. ISBN978-84-473-9090-8.
^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. PMID21921192. S2CID206536332.
^Ballard, S.; Fabrycky, D.; Fressin, F.; Charbonneau, D.; Desert, J. M.; Torres, G.; Marcy, G.; Burke, C. J.; Isaacson, H.; Henze, C.; Steffen, J. H.; Ciardi, D. R.; Howell, S. B.; Cochran, W. D.; Endl, M.; Bryson, S. T.; Rowe, J. F.; Holman, M. J.; Lissauer, J. J.; Jenkins, J. M.; Still, M.; Ford, E. B.; Christiansen, J. L.; Middour, C. K.; Haas, M. R.; Li, J.; Hall, J. R.; McCauliff, S.; Batalha, N. M.; Koch, D. G.; et al. (2011). "The Kepler-19 System: A Transiting 2.2 R⊕ Planet and a Second Planet Detected Via Transit Timing Variations". The Astrophysical Journal. 743 (2): 200. arXiv:1109.1561. Bibcode:2011ApJ...743..200B. doi:10.1088/0004-637X/743/2/200. S2CID42698813.
^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. Vol. 1158. p. 3. arXiv:0906.5011. Bibcode:2009AIPC.1158....3M. doi:10.1063/1.3215910. S2CID16660243. Exoplanets and Disks: Their Formation and Diversity: Proceedings of the International Conference
^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. PMID12198540. S2CID4391342.
^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". The Astrophysical Journal. 772 (2): L16. arXiv:1307.3239. Bibcode:2013ApJ...772L..16E. doi:10.1088/2041-8205/772/2/L16. S2CID38344760.
^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 (1): 53. arXiv:1210.4592. Bibcode:2012ApJ...761...53B. doi:10.1088/0004-637X/761/1/53. S2CID18216065.
^ abcBurrows, Adam (2014). "Scientific Return of Coronagraphic Exoplanet Imaging and Spectroscopy Using WFIRST". arXiv:1412.6097 [astro-ph.EP].
^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.
^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.
^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. S2CID55818711.
^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. S2CID118327512.
^Kopparapu, Ravi Kumar; Ramirez, Ramses M.; Schottelkotte, James; Kasting, James F.; Domagal-Goldman, Shawn; Eymet, Vincent (2014). "Habitable Zones around Main-sequence Stars: Dependence on Planetary Mass". The Astrophysical Journal. 787 (2): L29. arXiv:1404.5292. Bibcode:2014ApJ...787L..29K. doi:10.1088/2041-8205/787/2/L29. S2CID118588898.
Jayawardhana, Ray (2011). Strange New Worlds: The Search for Alien Planets and Life beyond Our Solar System. Princeton, NJ: Princeton University Press. ISBN978-0-691-14254-8 (Hardcover).
Perryman, Michael (2011). The Exoplanet Handbook. Cambridge University Press. ISBN978-0-521-76559-6.
Seager, Sara, ed. (2011). Exoplanets. University of Arizona Press. ISBN978-0-8165-2945-2.
