Circumstellar habitable zone

From Wikipedia, the free encyclopedia
  (Redirected from Habitable zone)
Jump to: navigation, search
"Goldilocks zone" and "Comfort zone (astronomy)" redirect here. For the planet originally nicknamed "Goldilocks", see 70 Virginis b. For the more general Goldilocks principle, see Goldilocks principle. For other uses, see Comfort zone (disambiguation).
An example of a system based on stellar luminosity for predicting the location of the habitable zone around various types of stars. Planet sizes, star sizes, orbit lengths, and habitable zone sizes are not to scale.

In astronomy and astrobiology, the circumstellar habitable zone (CHZ), or simply the habitable zone, colloquially known as the Goldilocks zone, is the region around a star within which planetary-mass objects with sufficient atmospheric pressure can support liquid water at their surfaces.[1][2] The bounds of the CHZ are calculated using the known requirements of Earth's biosphere, its position in the Solar System and the amount of radiant energy it receives from the Sun. Due to the importance of liquid water to life as it exists on Earth, the nature of the CHZ and the objects within is believed to be instrumental in determining the scope and distribution of earth-like extraterrestrial life and intelligence.

Since the concept of the CHZ was first presented in 1953,[3] numerous planets have now been discovered in the CHZ. Most such planets, being super-Earths or gas giants, are more massive than Earth, because such planets are easier to detect. On November 4, 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of sun-like stars and red dwarf stars within the Milky Way Galaxy.[4][5] 11 billion of these estimated planets may be orbiting sun-like stars.[6] The nearest such planet may be 12 light-years away, according to the scientists.[4][5] The CHZ is also of particular interest to the emerging field of natural satellite habitability, because planetary-mass moons in the CHZ might outnumber planets.[7]

In subsequent decades, the CHZ concept began to be challenged as a primary criterion for life. Since the discovery of evidence for extraterrestrial liquid water, substantial quantities of it are now believed to occur outside the circumstellar habitable zone. Sustained by other energy sources, such as tidal heating[8][9] or radioactive decay[10] or pressurized by other non-atmospheric means, the basic conditions for water-dependent life may be found even in interstellar space, on rogue planets or their moons.[11] In addition, other circumstellar zones, where non-water solvents favorable to hypothetical life based on alternative biochemistries could exist in liquid form at the surface, have been proposed.[12]

History[edit]

The concept of a Circumstellar Habitable Zone was first introduced in 1953 by Hubertus Strughold, who in his treatise The Green and the Red Planet: A Physiological Study of the Possibility of Life on Mars coined the term "ecosphere" and referred to various "zones" in which life could emerge.[3][13] In the same year, Harlow Shapley wrote "Liquid Water Belt", which described the same theory in further scientific detail. Both works stressed the importance of liquid water to life.[14] Su-Shu Huang, an American astrophysicist, first introduced the term "habitable zone" in 1959 to refer to the area around a star where liquid water could exist on a sufficiently large body, and was the first to introduce it in the context of planetary habitability and extraterrestrial life.[15][16] A major early contributor to habitable zone theory, Huang argued in 1960 that circumstellar habitable zones, and by extension extraterrestrial life, would be uncommon in multiple star systems, given the gravitational instabilities of those systems.[17]

The theory of habitable zones was further developed in 1964 by Stephen H. Dole in his book Habitable Planets for Man, in which he covered the circumstellar habitable zone itself as well as various other determinants of planetary habitability, eventually estimating the number of habitable planets in the Milky Way to be about 600 million.[18] At the same time, science-fiction author Isaac Asimov introduced the concept of a circumstellar habitable zone to the general public through his various explorations of space colonization.[19] The term "Goldilocks zone" emerged in the 1970s, referencing specifically a region around a star whose temperature is "just right" for water to be present in the liquid phase.[20] In 1993, astronomer James Kasting introduced the term "circumstellar habitable zone" to refer more precisely to the region then (and still) known as the habitable zone.[15]

An update to habitable-zone theory came in 2000, when astronomers Peter Ward and Donald Brownlee introduced the idea of the "galactic habitable zone", which they later developed with Guillermo Gonzalez.[21][22] The galactic habitable zone, defined as the region where life is most likely to emerge in a galaxy, encompasses those regions close enough to a galactic center that stars there are enriched with heavier elements, but not so close that star systems, planetary orbits, and the emergence of life would be frequently disrupted by the intense radiation and enormous gravitational forces commonly found at galactic centers.[21]

Subsequently, several planetary scientists have criticized the circumstellar habitable zone theory for its "carbon chauvinism", proposing that the concept be extended to other solvents, such as ammonia or methane, which could be the basis of life based on an alternative biochemistry.[12] In 2013, further developments in habitable zone theory were made with the proposal of a circumplanetary habitable zone, also known as the "habitable edge", to encompass the region around a planet where the orbits of natural satellites would not be disrupted, and at the same time tidal heating from the planet would not cause liquid water to boil away.[23]

Determination of the circumstellar habitable zone[edit]

The range of published estimates for the extent of the Sun's CHZ. The conservative CHZ[18] is indicated by a dark-green band crossing the inner edge of the aphelion of Venus, whereas an extended CHZ,[24] extending to the orbit of the dwarf planet Ceres, is indicated by a light-green band.

Whether a body is in the circumstellar habitable zone of its host star is dependent on the radius of the planet's orbit (for natural satellites, the host planet's orbit), the mass of the body itself, and the radiative flux of the host star. Given the large spread in the masses of planets within a circumstellar habitable zone, coupled with the discovery of super-Earth planets which can sustain thicker atmospheres and stronger magnetic fields than Earth, circumstellar habitable zones are now split into two separate regions—a "conservative habitable zone" in which lower-mass planets like Earth or Venus can remain habitable, complemented by a larger "extended habitable zone" in which super-Earth planets, with stronger greenhouse effects, can have the right temperature for liquid water to exist at the surface.[25]

Solar System estimates[edit]

Estimates for the habitable zone within the Solar System range from 0.725 to 3.0 astronomical units, though arriving at these estimates has been challenging for a variety of reasons. Venus, for example, has an orbit whose aphelion touches the inner reaches of the Solar System's habitable zone, but has an extremely thick carbon dioxide atmosphere which causes the surface temperature to reach 462 °C (864 °F).[26] Although the entire orbits of the Moon,[27] Mars,[28] and the dwarf planet Ceres[29] lie within various estimates of the habitable zone, and seasonal flows on warm Martian slopes have not yet been ruled out, these three bodies have atmospheric pressures that are far too low to create a strong greenhouse effect and sustain liquid water on their surfaces.

Most estimates, therefore, are inferred from the effect that a repositioned orbit would have on the habitability of Earth or Venus. According to extended habitable zone theory, however, a planet with a denser atmosphere than Earth orbiting in the extended habitable zone might theoretically possess liquid water. Gliese 667 Cd[30] and Gliese 581 d are examples of sufficiently massive planets considered to have the potential for possessing terrestrial surfaces and global warming inducing atmospheres sufficient for habitability.[31][32]

Estimates of the circumstellar-habitable-zone boundaries of the Solar System
Inner Edge (AU) Outer Edge (AU) Year Notes
0.725 1.24 Dole 1964[18] Used optically thin atmospheres and fixed albedos. Places the aphelion of Venus just inside the zone.
1.385–1.398 Budyko 1969[33] Based on studies of ice albedo feedback models to determine the point at which Earth would experience global glaciation. This estimate was supported in studies by Sellers 1969[34] and North 1975.[35]
0.88–0.912 Rasool and DeBurgh 1970[36] Based on studies of Venus's atmosphere, Rasool and DeBurgh concluded that this is the minimum distance at which Earth would have formed stable oceans.
0.95 1.01 Hart et al. 1979[37] Based on computer modelling and simulations of the evolution of Earth's atmospheric composition and surface temperature. This estimate has often been cited by subsequent publications.
3.0 Fogg 1992[24] Used the carbon cycle to estimate the outer edge of the circumstellar habitable zone.
1.37 Kasting et al. 1993[15] Noted the cooling effect of cloud albedo.
2.0 Spiegel et al. 2010[38] Proposed that seasonal liquid water is possible to this limit when combining high obliquity and orbital eccentricity.
0.75 Abe et al. 2011[39] Found that land-dominated "desert planets" with water at the poles could exist closer to the Sun than watery planets like Earth.
0.77—0.87 1.02—1.18 Vladilo et al. 2013[40] Inner edge of circumstellar habitable zone is closer and outer edge is farther for higher atmospheric pressures; determined minimum atmospheric pressure required to be 15 millibar.
0.99 1.688 Kopparapu et al. 2013[1] Revised estimates using updated runaway greenhouse and water loss algorithms. According to this measure Earth is at the inner edge of the HZ and close to, but just outside, the runaway greenhouse limit. This applies to a planet with Earth-like atmospheric composition and pressure.
0.5 Zsom et al. 2013
[41]
Estimate based on various possible combinations of atmospheric composition, pressure and relative humidity of the planet's atmosphere.

Extrasolar extrapolation[edit]

Astronomers use stellar flux and the inverse-square law to extrapolate cirumstellar-habitable-zone models created for the Solar System to other stars. For example, although the Solar System has a circumstellar habitable zone centered at 1.34 AU from the Sun,[1] a star with 0.25 times the luminosity of the Sun would have a habitable zone centered at \sqrt{0.25}, or 0.5, the distance from the star, corresponding to a distance of 0.67 AU. Various complicating factors, though, including the individual characteristics of stars themselves, mean that extrasolar extrapolation of the CHZ concept is more complex.

Spectral types and star-system characteristics[edit]

A video explaining the significance of the 2011 discovery of a planet in the circumbinary habitable zone of Kepler-47.

Some scientists argue that the concept of a circumstellar habitable zone is actually limited to stars in certain types of systems or of certain spectral types. Binary systems, for example, have circumstellar habitable zones that differ from those of single-star planetary systems, in addition to the orbital-stability concerns inherent with a three-body configuration.[42] If the Solar System were such a binary system, the outer limits of the resulting circumstellar habitable zone could extend as far as 2.4 AU.[43][44]

With regard to spectral types, Zoltán Balog proposes that O-type stars cannot form planets due to the photoevaporation caused by their strong ultraviolet emissions.[45] Studying ultraviolet emissions, Andrea Buccino found that only 40 percent of stars studied (including the Sun) had overlapping liquid water and ultraviolet habitable zones.[46] Stars smaller than the Sun, on the other hand, have distinct impediments to habitability. Michael Hart, for example, proposed that only main-sequence stars of spectral class K0 or brighter could possess habitable zones, an idea which has evolved in modern times into the concept of a tidal locking radius for red dwarfs. Within this radius, which is coincidental with the red-dwarf habitable zone, it has been suggested that the volcanism caused by tidal heating could cause a "tidal Venus" planet with high temperatures and no ability to support life.[47]

Others maintain that circumstellar habitable zones are more common and that it is indeed possible for water to exist on planets orbiting cooler stars. Climate modelling from 2013 supports the idea that red dwarf stars can support planets with relatively constant temperatures over their surfaces in spite of tidal locking.[48] Astronomy professor Eric Agol argues that even white dwarfs may support a relatively brief habitable zone through planetary migration.[49] At the same time, others have written in similar support of semi-stable, temporary habitable zones around brown dwarfs.[47]

Stellar evolution[edit]

Natural defenses against space weather, such as the magnetosphere depicted in this artistic rendition, may be required for planets to sustain surface water for prolonged periods.

Circumstellar habitable zones change over time with stellar evolution. For example, hot O-type stars, which may remain on the main sequence for fewer than 10 million years,[50] would have rapidly changing habitable zones not conducive to the development of life. Red dwarf stars, on the other hand, which can live for hundreds of billions of years on the main sequence, would have planets with ample time for life to develop and evolve.[51][52] Even while stars are on the main sequence, though, their energy output steadily increases, pushing their habitable zones farther and farther out; our Sun, for example, was only 75 percent as bright in the Archaean as it is now,[53] and in the future continued increases in energy output will put Earth outside the Sun's habitable zone, even before it reaches the red giant phase.[54] In order to deal with this increase in luminosity, the concept of a continuously habitable zone has been introduced. As the name suggests, the continuously habitable zone is a region around a star in which planetary-mass bodies can sustain liquid water for a given period of time. Like the general circumstellar habitable zone, the continuously habitable zone of a star is divided into a conservative and extended region.[54]

In red dwarf systems, gigantic stellar flares which could double a star's brightness in minutes[55] and huge starspots which can cover 20 percent of the star's surface area,[56] have the potential to strip an otherwise habitable planet of its atmosphere and water.[57] As with more massive stars, though, stellar evolution changes their nature,[58] so by about 1.2 billion years of age, red dwarfs generally become sufficiently constant to allow for the development of life.[57][59]

Once a star has evolved sufficiently to become a red giant, its circumstellar habitable zone will change dramatically from its main-sequence size. For example, the Sun is expected to engulf the previously-habitable Earth as a red giant.[60] However, once a red giant star reaches the horizontal branch, it achieves a new equilibrium and can sustain a circumstellar habitable zone, which in the case of the Sun would range from 7 to 22 AU.[61] At such stage, Saturn's moon Titan would likely be habitable in Earth's sense.[62] Given that this new equilibrium lasts for about 1 Gyr, and because life on Earth emerged by 0.7 Gyr from the formation of the Solar System at latest, life could conceivably develop on planetary mass objects in the habitable zone of red giants.[61] However, around such a helium-burning star, important life processes like photosynthesis could only happen around planets where the atmosphere has been artificially seeded with carbon dioxide, as by the time a solar-mass star becomes a red giant, planetary-mass bodies would have already absorbed much of their free carbon dioxide.[63]

Desert planets[edit]

A planet's atmospheric conditions influence its 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.[64][65]

Other considerations[edit]

Earth's hydrosphere. Water covers 71% of Earth's surface, with the global ocean accounting for 97.3% of the water distribution on Earth.

A planet cannot have a hydrosphere—a key ingredient for the formation of carbon-based life—unless there is a source for water within its stellar system. The origin of water on Earth is still unknown; possible sources include the result of impacts with icy bodies, outgassing, mineralization, leakage from hydrous minerals from the lithosphere, and photolysis.[66][67] For an extrasolar system, an icy body from beyond the frost line could migrate into the habitable zone of its star, creating an ocean planet with seas hundreds of kilometers deep[68] such as GJ 1214 b[69][70] or Kepler-22b may be.[71]

Maintenance of liquid surface water also requires a sufficiently thick atmosphere. Possible origins of terrestrial atmospheres are currently theorised to outgassing, impact degassing and ingassing.[72] Atmospheres are thought to be maintained through similar processes along with biogeochemical cycles and the mitigation of atmospheric escape.[73] In a 2013 study led by Italian astronomer Giovanni Vladilo, it was shown that the size of the circumstellar habitable zone increased with greater atmospheric pressure.[40] Below an atmospheric pressure of about 15 millibars, it was found that habitability could not be maintained[40] because even a small shift in pressure or temperature could render water unable to form a liquid.[74]

In the case of planets orbiting in the CHZs of red dwarf stars, the extremely close distances to the stars cause tidal locking, an important factor in habitability. For a tidally locked planet, the sidereal day is as long as the orbital period, causing one side to permanently face the host star and the other side to face away. In the past, such tidal locking was believed to cause extreme heat on the star-facing side and bitter cold on the opposite side, making many red dwarf planets uninhabitable; however, a 2013 paper written by geophysicist Jun Yang of the University of Chicago and collaborators, using three-dimensional climate models, showed that the side of a red dwarf planet facing the host star would have extensive cloud cover, increasing its Bond albedo and reducing significantly temperature differences between the two sides.[48]

Planetary-mass natural satellites have the potential to be habitable as well. However, these bodies need to fulfill additional parameters, in particular being located within the circumplanetary habitable zones of their host planets.[23] More specifically, planets need to be far enough from their host giant planets that they are not transformed by tidal heating into volcanic worlds like Io,[23] but must still remain within the Hill radius of the planet so that they are not pulled out of orbit of their host planet.[75] Red dwarfs that have masses less than 20 percent of that of the Sun cannot have habitable moons around giant planets, as the small size of the circumstellar habitable zone would put a habitable moon so close to a star that it would be stripped from its host planet. In such a system, a moon close enough to its host planet to maintain its orbit would have tidal heating so intense as to eliminate any prospects of habitability.[23]

Artists concept of a planet on an eccentric orbit that passes through the CHZ for only part of its year

A planetary object that orbits a star with high orbital eccentricity may spend only some of its year in the CHZ and experience a large variation in temperature and atmospheric pressure. This would result in dramatic seasonal phase shifts where liquid water may exist only intermittently. It is possible that subsurface habitats could be insulated from such changes and that extremophiles on or near the surface might survive through adaptions such as hibernation (cryptobiosis) and/or hyperthermostability. Tardigrades, for example, can survive in a dehydrated state temperatures between 0.150 K (−273 °C)[76] and 424 K (151 °C).[77] Life on a planetary object orbiting outside CHZ might hibernate on the cold side as the planet approaches the apastron where the planet is coolest and become active on approach to the periastron when the planet is sufficiently warm.[78]

Extrasolar discoveries[edit]

Studies that have attempted to estimate the number of terrestrial planets within the circumstellar habitable zone tend to reflect the availability of scientific data. A 2013 study by Ravi Kumar Kopparapu put ηe, the fraction of stars with planets in the CHZ, at 0.48,[1] meaning that there may be roughly 95–180 billion habitable planets in the Milky Way.[79] However, this is merely a statistical prediction; only a small fraction of these possible planets have yet been discovered.[80]

Previous studies have been more conservative. In 2011, Seth Borenstein concluded that there are roughly 500 million habitable planets in the Milky Way.[81] NASA's Jet Propulsion Laboratory 2011 study, based on observations from the Kepler mission, raised the number somewhat, concluding that about "1.4 to 2.7 percent" of all stars of spectral class F, G, and K are expected to have planets in their CHZs.[82][83]

Early findings[edit]

The first discoveries of extrasolar planets in the CHZ occurred just a few years after the first extrasolar planets were discovered. One of the first discoveries was 70 Virginis b, a gas giant initially nicknamed "Goldilocks" due to it being neither "too hot" nor "too cold." Later study revealed temperatures analogous to Venus ruling out any potential for liquid water.[84] 16 Cygni Bb, also discovered in 1996, has an extremely eccentric orbit that causes extreme seasonal effects on the planet's surface. In spite of this, simulations have suggested that it is possible for a terrestrial natural satellite to support water at its surface year-round.[85]

Gliese 876 b, discovered in 1998, and Gliese 876 c, discovered in 2001, are both gas giants discovered in the habitable zone around Gliese 876. Although they are not thought to themselves possess significant water at their surfaces, both may have habitable moons.[86] Upsilon Andromedae d, discovered in 1999, is a gas giant in its star's circumstellar habitable zone considered to be large enough to favor the formation of large, Earth-like moons.[87]

Announced on April 4, 2001, HD 28185 b is a gas giant found to orbit entirely within its star's circumstellar habitable zone[88] and has a low orbital eccentricity, comparable to that of Mars in the Solar System.[89] Tidal interactions suggest that HD 28185 b could harbor habitable Earth-mass satellites in orbit around it for many billions of years,[90] though it is unclear whether such satellites could form in the first place.[91]

HD 69830 d, a gas giant with 17 times the mass of Earth, was in 2006 found orbiting within the circumstellar habitable zone of HD 69830, 41 light years away from Earth.[92] The following year, 55 Cancri f was discovered within the CHZ of its host star 55 Cancri A.[93][94] Although conditions on this massive and dense planet are not conducive to the formation of water or life as we know it, a hypothetical moon of this planet with the proper mass and composition could be able to support liquid water at its surface.[95]

Habitable super-Earths[edit]

The habitable zone of Gliese 581 compared with our Solar System's habitable zone.

The 2007 discovery of Gliese 581 c, the first super-Earth in the circumstellar habitable zone, created significant interest in the system by the scientific community, although the planet was later found to have surface conditions that likely resemble Venus more than Earth.[96] Gliese 581 d, another planet in the same system and thought to be a better candidate for habitability, was also announced in 2007. Its existence was later disconfirmed in 2014. Gliese 581 g, yet another planet thought to have been discovered in the circumstellar habitable zone of the system, was considered to be more habitable than both Gliese 581 c and d. However, its existence was also disconfirmed in 2014.[97]

Discovered in August 2011, HD 85512 b was initially believed to be habitable,[98] but the new circumstellar-habitable-zone criteria devised by Kopparapu et al. in 2013 place the planet outside the circumstellar habitable zone.[80] With an increase in the intensity of exoplanet discovery, the Earth Similarity Index was devised in October 2011 as a way of comparing planetary properties, such as surface temperature and density, to those of Earth in order to better gauge the habitability of extrasolar bodies.[99]

A diagram comparing size (artist's impression) and orbital position of planet Kepler-22b within Sun-like star Kepler 22's habitable zone and that of Earth in the Solar System

Kepler-22 b, discovered in December 2011 by the Kepler space probe,[100] is the first transiting exoplanet discovered around a sunlike star. With a radius 2.4 times that of Earth, Kepler-22b has been predicted by some to be an ocean planet.[101] Gliese 667 Cc, discovered in 2011 but announced in 2012,[102] is a super-Earth orbiting in the circumstellar habitable zone of Gliese 667 C. Subsequently in June 2013, two other habitable super-Earths orbiting the same star, Gliese 667 Cf and Gliese 667 Ce, were discovered in the CHZ.[103]

Gliese 163 c, discovered in September 2012 in orbit around the red dwarf Gliese 163[104] is located 49 light years from Earth. The planet has 6.9 Earth masses and 1.8–2.4 Earth radii, and with its close orbit receives 40 percent more stellar radiation than Earth, leading to surface temperatures of about 60° C.[105][106][107] HD 40307 g, a candidate planet tentatively discovered in November 2012, is in the circumstellar habitable zone of HD 40307.[108] In December 2012, Tau Ceti e and Tau Ceti f were found in the circumstellar habitable zone of Tau Ceti, a sunlike star just 12 light years away.[109] Although more massive than Earth, they are among the least massive planets found to date orbiting in the zone;[110] however, Tau Ceti f, like HD 85512 b, did not fit the new circumstellar-habitable-zone criteria established by the 2013 Kopparapu study.[111]

Earth-sized planets[edit]

Comparison of the CHZ position of Earth-radius planet Kepler-186f and the Solar System (17 April 2014)

Recent discoveries have uncovered planets that are believed to be similar in many ways to the Earth (that is Earth analogs, or terrestrial planets relatively high Earth Similarity Indexes). While there is no universal definition of "Earth-sized", ranges are typically defined by mass. The lower range used in many definitions of the Super-Earth class is 1.9 Earth masses, likewise, Sub-Earths range up to the size of Venus (~0.815 Earth masses). An upper limit of 1.5 Earth radii is also considered given that above 1.5 radii the average planet density rapidly decreases with increasing radius, indicating that these planets have a large fraction of volatiles by volume overlying a rocky core.[112]

On January 7, 2013, astronomers from the Kepler team announced the discovery of Kepler-69c (formerly KOI-172.02), an Earth-like exoplanet candidate (1.7 times the radius of Earth) orbiting Kepler-69, a star similar to our Sun, in the CHZ and a "prime candidate to host alien life".[113][114][115][116] The discovery of two planets orbiting in the habitable zone of Kepler-62, by the Kepler team was announced on April 19, 2013. The planets, named Kepler-62e and Kepler-62f, are likely solid planets with sizes 1.6 and 1.4 times the radius of Earth, respectively.[115][116][117]

With a radius measured at 1.1 Earth, Kepler-186f, discovery announced in April 2014, is the closest yet size to Earth of an exoplanet confirmed by the transit method[118][119][120] though its mass remains unknown and its parent star is not a Solar analog.

Habitability outside the CHZ[edit]

The discovery of hydrocarbon lakes on Saturn's moon Titan has begun to call into question the carbon chauvinism that underpins CHZ theory.

Liquid water environments suitable for sustaining a diversity of organisms, both simple and complex, have been found to exist in isolation of atmospheric pressure and at temperatures outside the CHZ temperature range. Titan and Europa, both outside the habitable zone, may possess liquid water as well.[121]

In addition, testing of a number of organisms has found some are capable of surviving in extra-CHZ conditions.[122]

Tidal heating and radioactive decay are two possible heat sources which could contribute to surface water environments outside the CHZ.[8][9] Abbot & Switzer (2011) put forward the possibility that surface water could exist on rogue systems as a result of these mechanisms.[11]

With some theorising that life on Earth may have actually originated beneath the surface in stable habitats protected from chaotic surface conditions early in the planet's history[123][124] it has been suggested that it may be common for wet subsurface extraterrestrial habitats to 'teem with life'.[125] Indeed, life on Earth is found more than 6 kilometres below the surface.[126]

Alternatives to water[edit]

Another possibility is that outside the CHZ organisms may use alternative biochemistries that do not require water at all. Astrobiologists, including NASA's Christopher McKay, have suggested that methane may be a solvent conducive to the development of "cryolife", with the Sun's methane habitable zone being centered on 1.6×109 km (1,000,000,000 mi) from the star.[12] This distance is coincidental with the location of Saturn's moon Titan, whose lakes and rain of methane make it an ideal location to find McKay's proposed cryolife.[12]

Significance for complex and intelligent life[edit]

The Rare Earth hypothesis argues that complex and intelligent life is uncommon and that the CHZ is a critical factor. According to Ward & Brownlee (2004) and others, not only is a CHZ orbit and surface water a primary requirement to sustain life but a requirement to support the secondary conditions required for multicellular life to emerge and evolve. The secondary habitability factors are both geological (the role of surface water in sustaining necessary plate tectonics)[21] and biochemical (the role of radiant energy in support photosynthesis for necessary atmospheric oxygenation).[127] But others, such as Ian Stewart and Jack Cohen in their 2002 book Evolving the Alien argue that complex intelligent life may arise outside the CHZ.[128] Intelligent life outside the CHZ may have evolved in subsurface environments, from alternative biochemistries[128] or even from nuclear reactions.[129] Complex multicellular life has been found with the potential to survive the sort of conditions that might exist outside the CHZ. An animal example of such a life form is the tardigrade, which can withstand both temperatures well above the boiling point of water and the vacuum of outer space.[130] In addition, the plant Rhizocarpon geographicum has been found to survive in an environment where the atmospheric pressure is far too low for surface liquid water and where the radiant energy is also much lower than that which most plants require to photosynthesize.[131][132] If the human race, however, is to colonize other planets, true Earth analogs in the CHZ are most likely to provide the closest natural habitats for human beings; this concept was the basis of Stephen H. Dole's 1964 study. With suitable temperature, gravity, atmospheric pressure and the presence of water, the necessity of spacesuits may be eliminated and complex Earth-life can be allowed to flourish.[18]

Planets in the CHZ remain of paramount interest to researchers looking for intelligent life elsewhere in the universe.[133] The 1961 Drake equation, still used as means of calculating the number of intelligent civilizations in our galaxy, contains a parameter ηe, which is generally considered to imply the fraction of stars that have planetary mass objects orbiting within the CHZ. A low value lends support to the Rare Earth hypothesis, which posits that intelligent life is a rarity in the Universe, whereas a high value provides evidence for the Copernican mediocrity principle, the view that habitability—and therefore life—is common throughout the Universe.[21] A 1971 NASA report by Drake and Bernard Oliver proposed the "waterhole", based on the spectral absorption lines of the hydrogen and hydroxyl components of water, as a good, obvious band for communication with extraterrestrial intelligence[134][135] that has since been widely adopted by astronomers involved in the search for extraterrestrial intelligence. According to Jill Tarter, Margaret Turnbull and many others, CHZ candidates are the priority targets to narrow waterhole searches[136][137] and the Allen Telescope Array now extends Project Phoenix to such candidates.[138]

Because the CHZ is considered the most likely habitat for intelligent life, METI efforts have also been focused on systems likely to have planets there. The 2001 Teen Age Message and the 2003 Cosmic Call 2, for example, were sent to the 47 Ursae Majoris system, known to contain three Jupiter-mass planets and possibly with a terrestrial planet in the CHZ.[139][140][141][142] The Teen Age Message, and the later Wow! reply, were also directed to the 55 Cancri system, which has a gas giant in its CHZ.[93] A Message to Earth in 2008, and Hello From Earth in 2009, were directed to the Gliese 581 system, containing three planets in the CHZ—Gliese 581 c, d, and the unconfirmed g.[143]

See also[edit]

References[edit]

  1. ^ a b c d 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. 
  2. ^ 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. 
  3. ^ a b Huggett, Richard J. (1995). Geoecology: An Evolutionary Approach. Routledge, Chapman & Hall. p. 10. ISBN 978-0-415-08689-9. 
  4. ^ a b Overbye, Dennis (November 4, 2013). "Far-Off Planets Like the Earth Dot the Galaxy". New York Times. Retrieved November 5, 2013. 
  5. ^ a b Petigura, Eric A.; Howard, Andrew W.; Marcy, Geoffrey W. (October 31, 2013). "Prevalence of Earth-size planets orbiting Sun-like stars". Proceedings of the National Academy of Sciences of the United States of America. arXiv:1311.6806. Bibcode:2013PNAS..11019273P. doi:10.1073/pnas.1319909110. Retrieved November 5, 2013. 
  6. ^ Khan, Amina (November 4, 2013). "Milky Way may host billions of Earth-size planets". Los Angeles Times. Retrieved November 5, 2013. 
  7. ^ Schirber, Michael (26 Oct 2009). "Detecting Life-Friendly Moons". Astrobiology Magazine. NASA. Retrieved 9 May 2013. 
  8. ^ a b Cowen, Ron (2008-06-07). "A Shifty Moon". Science News. 
  9. ^ a b Bryner, Jeanna (24 June 2009). "Ocean Hidden Inside Saturn's Moon". Space.com. TechMediaNetwork. Retrieved 22 April 2013. 
  10. ^ Abbot, D. S.; Switzer, E. R. (2011). "The Steppenwolf: A Proposal for a Habitable Planet in Interstellar Space". The Astrophysical Journal 735 (2): L27. arXiv:1102.1108. Bibcode:2011ApJ...735L..27A. doi:10.1088/2041-8205/735/2/L27. 
  11. ^ a b "Rogue Planets Could Harbor Life in Interstellar Space, Say Astrobiologists". MIT Technology Review. MIT Technology Review. 9 February 2011. Retrieved 24 June 2013. 
  12. ^ a b c d Villard, Ray (November 18, 2011). "Alien Life May Live in Various Habitable Zones : Discovery News". News.discovery.com. Discovery Communications LLC. Retrieved April 22, 2013. 
  13. ^ Strughold, Hubertus (1953). The Green and Red Planet: A Physiological Study of the Possibility of Life on Mars. University of New Mexico Press. 
  14. ^ Kasting, James (2010). How to Find a Habitable Planet. Princeton University Press. p. 127. ISBN 978-0-691-13805-3. Retrieved 4 May 2013. 
  15. ^ a b c Kasting, James F.; Whitmire, Daniel P.; Reynolds, Ray T. (January 1993). "Habitable Zones around Main Sequence Stars". Icarus 101 (1): 108–118. Bibcode:1993Icar..101..108K. doi:10.1006/icar.1993.1010. PMID 11536936. 
  16. ^ Huang, Su-Shu (1966). Extraterrestrial life: An Anthology and Bibliography. National Research Council (U.S.). Study Group on Biology and the Exploration of Mars. Washington, D. C.: National Academy of Sciences. pp. 87–93. 
  17. ^ Huang, Su-Shu (April 1960). "Life-Supporting Regions in the Vicinity of Binary Systems". Publications of the Astronomical Society of the Pacific 72 (425): 106–114. Bibcode:1960PASP...72..106H. doi:10.1086/127489. 
  18. ^ a b c d Dole, Stephen H (1964). Habitable Planets for Man. Blaisdell Publishing Company. p. 103. 
  19. ^ Gilster, Paul (2004). Centauri Dreams: Imagining and Planning Interstellar Exploration. Springer. p. 40. ISBN 978-0-387-00436-5. 
  20. ^ "The Goldilocks Zone" (Press release). NASA. October 2, 2003. Retrieved April 22, 2013. 
  21. ^ a b c d Brownlee, Donald; Ward, Peter (2004). Rare Earth: Why Complex Life Is Uncommon in the Universe. New York: Copernicus. ISBN 0-387-95289-6. 
  22. ^ Gonzalez, Guillermo; Brownlee, Donald; Ward, Peter (July 2001). "The Galactic Habitable Zone I. Galactic Chemical Evolution". Icarus 152 (1): 185–200. arXiv:0103165. Bibcode:2001Icar..152..185G. doi:10.1006/icar.2001.6617. 
  23. ^ a b c d Hadhazy, Adam (April 3, 2013). "The 'Habitable Edge' of Exomoons". Astrobiology Magazine. NASA. Retrieved April 22, 2013. 
  24. ^ a b Fogg, M. J. (1992). "An Estimate of the Prevalence of Biocompatible and Habitable Planets". Journal of the British Interplanetary Society 45 (1): 3–12. Bibcode:1992JBIS...45....3F. PMID 11539465. 
  25. ^ Redd, Nola Taylor (25 August 2011). "Greenhouse Effect Could Extend Habitable Zone". Astrobiology Magazine. NASA. Retrieved 25 June 2013. 
  26. ^ "Venus". Case Western Reserve University. 13 September 2006. Retrieved 2011-12-21. 
  27. ^ Sharp, Tim. "Atmosphere of the Moon". Space.com. TechMediaNetwork. Retrieved April 23, 2013. 
  28. ^ Bolonkin, Alexander A. (2009). Artificial Environments on Mars. Berlin Heidelberg: Springer. pp. 599–625. ISBN 978-3-642-03629-3. 
  29. ^ A'Hearn, Michael F.; Feldman, Paul D. (1992). "Water vaporization on Ceres". Icarus 98 (1): 54–60. Bibcode:1992Icar...98...54A. doi:10.1016/0019-1035(92)90206-M. 
  30. ^ Chow, Denise (February 2, 2012). "Newfound Alien Planet is Best Candidate Yet to Support Life, Scientists Say". Space.com. Retrieved February 3, 2012. 
  31. ^ von Bloh, W. et al. (2008). "Habitability of Super-Earths: Gliese 581c and 581d". Proceedings of the International Astronomical Union 3. arXiv:0712.3219. doi:10.1017/S1743921308017031. 
  32. ^ "A Habitable World After All?". Centauri-dreams.org. December 13, 2007. Retrieved January 18, 2009. 
  33. ^ Budyko, M. I. (1969). "The effect of solar radiation variations on the climate of the Earth". Tellus 21 (5): 611. doi:10.1111/j.2153-3490.1969.tb00466.x.  edit
  34. ^ Sellers, William D. (June 1969). "A Global Climatic Model Based on the Energy Balance of the Earth-Atmosphere System". Journal of Applied Meteorology 8 (3): 392–400. Bibcode:1969JApMe...8..392S. doi:10.1175/1520-0450(1969)008<0392:AGCMBO>2.0.CO;2. 
  35. ^ North, Gerald R. (November 1975). "Theory of Energy-Balance Climate Models". Journal of the Atmospheric Sciences 32 (11): 2033–2043. Bibcode:1975JAtS...32.2033N. doi:10.1175/1520-0469(1975)032<2033:TOEBCM>2.0.CO;2. 
  36. ^ Rasool, I.; De Bergh, C. (Jun 1970). "The Runaway Greenhouse and the Accumulation of CO2 in the Venus Atmosphere". Nature 226 (5250): 1037–1039. Bibcode:1970Natur.226.1037R. doi:10.1038/2261037a0. ISSN 0028-0836. PMID 16057644.  edit
  37. ^ Hart, M. H. (1979). "Habitable zones about main sequence stars". Icarus 37: 351–357. Bibcode:1979Icar...37..351H. doi:10.1016/0019-1035(79)90141-6.  edit
  38. ^ Spiegel, D. S.; Raymond, S. N.; Dressing, C. D.; Scharf, C. A.; Mitchell, J. L. (2010). "Generalized Milankovitch Cycles and Long-Term Climatic Habitability". The Astrophysical Journal 721 (2): 1308. arXiv:1002.4877. Bibcode:2010ApJ...721.1308S. doi:10.1088/0004-637X/721/2/1308.  edit
  39. ^ Abe, Y.; Abe-Ouchi, A.; Sleep, N. H.; Zahnle, K. J. (2011). "Habitable Zone Limits for Dry Planets". Astrobiology 11 (5): 443–460. Bibcode:2011AsBio..11..443A. doi:10.1089/ast.2010.0545. PMID 21707386.  edit
  40. ^ a b c Vladilo, Giovanni; Murante, Giuseppe; Silva, Laura; Provenzale, Antonello; Ferri, Gaia; Ragazzini, Gregorio (March 2013). "The habitable zone of Earth-like planets with different levels of atmospheric pressure". The Astrophysical Journal (accepted) 767 (1): 65–?. arXiv:1302.4566. Bibcode:2013ApJ...767...65V. doi:10.1088/0004-637X/767/1/65. 
  41. ^ Zsom, Andras; Seager, Sara; De Wit, Julien (2013). "Towards the Minimum Inner Edge Distance of the Habitable Zone". arXiv:1304.3714 [astro-ph.EP].
  42. ^ Cuntz, Manfred (2013). "S-Type and P-Type Habitability in Stellar Binary Systems: A Comprehensive Approach. I. Method and Applications". arXiv:1303.6645 [astro-ph.EP].
  43. ^ Forget, F.; Pierrehumbert, RT (1997). "Warming Early Mars with Carbon Dioxide Clouds That Scatter Infrared Radiation". Science 278 (5341): 1273–6. Bibcode:1997Sci...278.1273F. doi:10.1126/science.278.5341.1273. PMID 9360920. 
  44. ^ Mischna, M; Kasting, JF; Pavlov, A; Freedman, R (2000). "Influence of Carbon Dioxide Clouds on Early Martian Climate". Icarus 145 (2): 546–54. Bibcode:2000Icar..145..546M. doi:10.1006/icar.2000.6380. PMID 11543507. 
  45. ^ Vu, Linda. "Planets Prefer Safe Neighborhoods" (Press release). Spitzer.caltech.edu. NASA/Caltech. Retrieved April 22, 2013. 
  46. ^ Buccino, Andrea P.; Lemarchand, Guillermo A.; Mauas, Pablo J.D. (2006). "Ultraviolet radiation constraints around the circumstellar habitable zones". Icarus 183 (2): 491–503. arXiv:astro-ph/0512291. Bibcode:2006Icar..183..491B. doi:10.1016/j.icarus.2006.03.007. 
  47. ^ a b Barnes, Rory; Heller, René (March 2013). "Habitable Planets Around White and Brown Dwarfs: The Perils of a Cooling Primary". Astrobiology 13 (3): 279–291. arXiv:1203.5104. Bibcode:2013AsBio..13..279B. doi:10.1089/ast.2012.0867. PMC 3612282. PMID 23537137. 
  48. ^ a b Yang, J.; Cowan, N. B.; Abbot, D. S. (2013). "Stabilizing Cloud Feedback Dramatically Expands the Habitable Zone of Tidally Locked Planets". The Astrophysical Journal 771 (2): L45. arXiv:1307.0515. Bibcode:2013ApJ...771L..45Y. doi:10.1088/2041-8205/771/2/L45.  edit
  49. ^ Agol, Eric (April 2011). "Transit Surveys for Earths in the Habitable Zones of White Dwarfs". The Astrophysical Journal Letters 731 (2): 1–5. arXiv:1103.2791. Bibcode:2011ApJ...731L..31A. doi:10.1088/2041-8205/731/2/L31. 
  50. ^ Carroll, Bradley; Ostlie, Dale (2007). An Introduction to Modern Astrophysics (2 ed.). 
  51. ^ Richmond, Michael (November 10, 2004). "Late stages of evolution for low-mass stars". Rochester Institute of Technology. Retrieved 2007-09-19. 
  52. ^ Guo, J.; Zhang, F.; Chen, X.; Han, Z. (2009). "Probability distribution of terrestrial planets in habitable zones around host stars". Astrophysics and Space Science 323 (4): 367. arXiv:1003.1368. Bibcode:2009Ap&SS.323..367G. doi:10.1007/s10509-009-0081-z.  edit
  53. ^ Kasting, J.F.; Ackerman, T.P. (1986). "Climatic Consequences of Very High Carbon Dioxide Levels in the Earth's Early Atmosphere". Science 234 (4782): 1383–1385. doi:10.1126/science.11539665. PMID 11539665. 
  54. ^ a b Franck, S.; von Bloh, W.; Bounama, C.; Steffen, M.; Schönberner, D.; Schellnhuber, H.-J. (2002). "Habitable Zones and the Number of Gaia's Sisters". In Montesinos, Benjamin; Giménez, Alvaro; Guinan, Edward F. ASP Conference Series. The Evolving Sun and its Influence on Planetary Environments. Astronomical Society of the Pacific. pp. 261–272. Bibcode:2002ASPC..269..261F. ISBN 1-58381-109-5. Retrieved April 26, 2013. 
  55. ^ Croswell, Ken (January 27, 2001). "Red, willing and able" (Full reprint). New Scientist. Retrieved August 5, 2007. 
  56. ^ Alekseev, I. Y.; Kozlova, O. V. (2002). "Starspots and active regions on the emission red dwarf star LQ Hydrae". Astronomy and Astrophysics 396: 203. Bibcode:2002A&A...396..203A. doi:10.1051/0004-6361:20021424.  edit
  57. ^ a b Alpert, Mark (November 7, 2005). "Red Star Rising". Scientific American. Retrieved January 19, 2013. 
  58. ^ Research Corporation (December 19, 2006). "Andrew West: 'Fewer flares, starspots for older dwarf stars'". EarthSky. Retrieved April 27, 2013. 
  59. ^ Cain, Fraser; Gay, Pamela (2007). "AstronomyCast episode 40: American Astronomical Society Meeting, May 2007". Universe Today. Retrieved 2007-06-17. 
  60. ^ Christensen, Bill (April 1, 2005). "Red Giants and Planets to Live On". Space.com. TechMediaNetwork. Retrieved April 27, 2013. 
  61. ^ a b Lopez, B.; Schneider, J.; Danchi, W. C. (2005). "Can Life Develop in the Expanded Habitable Zones around Red Giant Stars?". The Astrophysical Journal 627 (2): 974. arXiv:astro-ph/0503520. Bibcode:2005ApJ...627..974L. doi:10.1086/430416.  edit
  62. ^ Lorenz, Ralph D.; Lunine, Jonathan I.; McKay, Christopher P. (1997). "Titan under a red giant sun: A new kind of "habitable" moon". Geophysical Research Letters 24 (22): 2905–2908. Bibcode:1997GeoRL..24.2905L. doi:10.1029/97GL52843. ISSN 0094-8276. PMID 11542268. 
  63. ^ Voisey, Jon (February 23, 2011). "Plausibility Check – Habitable Planets around Red Giants". Universe Today. Retrieved April 27, 2013. 
  64. ^ Alien Life More Likely on 'Dune' Planets, 09/01/11, Charles Q. Choi, Astrobiology Magazine
  65. ^ Habitable Zone Limits for Dry Planets, Yutaka Abe, Ayako Abe-Ouchi, Norman H. Sleep, and Kevin J. Zahnle. Astrobiology. June 2011, 11(5): 443–460. doi:10.1089/ast.2010.0545
  66. ^ Drake, Michael J. (April 2005). "Origin of water in the terrestrial planets". Meteoritics & Planetary Science (John Wiley & Sons) 40 (4): 519–527. Bibcode:2005M&PS...40..519D. doi:10.1111/j.1945-5100.2005.tb00960.x. 
  67. ^ Drake, Michael J. et al. (August 2005). "Origin of water in the terrestrial planets". Asteroids, Comets, and Meteors (IAU S229). 229th Symposium of the International Astronomical Union 1 (4). Búzios, Rio de Janeiro, Brazil: Cambridge University Press. pp. 381–394. Bibcode:2006IAUS..229..381D. doi:10.1017/S1743921305006861. ISBN 978-0-521-85200-5. 
  68. ^ Kuchner, Marc (2003). "Volatile-rich Earth-Mass Planets in the Habitable Zone". Astrophysical Journal 596: L105–L108. arXiv:astro-ph/0303186. Bibcode:2003ApJ...596L.105K. doi:10.1086/378397. 
  69. ^ Charbonneau, David; Zachory K. Berta, Jonathan Irwin, Christopher J. Burke, Philip Nutzman, Lars A. Buchhave, Christophe Lovis, Xavier Bonfils, David W. Latham, Stéphane Udry, Ruth A. Murray-Clay, Matthew J. Holman, Emilio E. Falco, Joshua N. Winn, Didier Queloz, Francesco Pepe, Michel Mayor, Xavier Delfosse, Thierry Forveille (2009). "A super-Earth transiting a nearby low-mass star". Nature 462 (17 December 2009): 891–894. arXiv:0912.3229. Bibcode:2009Natur.462..891C. doi:10.1038/nature08679. PMID 20016595. Retrieved 2009-12-15. 
  70. ^ Kuchner, Seager; M., Hier-Majumder, C. A., Militzer (2007). "Mass–radius relationships for solid exoplanets". The Astrophysical Journal 669 (2): 1279–1297. arXiv:0707.2895. Bibcode:2007ApJ...669.1279S. doi:10.1086/521346. 
  71. ^ Vastag, Brian (December 5, 2011). "Newest alien planet is just the right temperature for life". The Washington Post. Retrieved April 27, 2013. 
  72. ^ Robinson, Tyler D.; Catling, David C. (2012). "An Analytic Radiative-Convective Model for Planetary Atmospheres". The Astrophysical Journal 757 (1): 104. arXiv:1209.1833. Bibcode:2012ApJ...757..104R. doi:10.1088/0004-637X/757/1/104. 
  73. ^ Shizgal, B. D.; Arkos, G. G. (1996). "Nonthermal escape of the atmospheres of Venus, Earth, and Mars". Reviews of Geophysics 34 (4): 483–505. Bibcode:1996RvGeo..34..483S. doi:10.1029/96RG02213. 
  74. ^ Chaplin, Martin (April 8, 2013). "Water Phase Diagram". Ices. London South Bank University. Retrieved April 27, 2013. 
  75. ^ D.P. Hamilton & J.A. Burns (1992). "Orbital stability zones about asteroids. II - The destabilizing effects of eccentric orbits and of solar radiation". Icarus 96 (1): 43. Bibcode:1992Icar...96...43H. doi:10.1016/0019-1035(92)90005-R. 
  76. ^ Becquerel P. (1950). "La suspension de la vie au dessous de 1/20 K absolu par demagnetization adiabatique de l'alun de fer dans le vide les plus eléve". C. R. Hebd. Séances Acad. Sci. Paris (in French) 231: 261–263. 
  77. ^ Horikawa, Daiki D. (2012). Alexander V. Altenbach, Joan M. Bernhard & Joseph Seckbach, ed. Anoxia Evidence for Eukaryote Survival and Paleontological Strategies. (21 ed.). Springer Netherlands. pp. 205–217. ISBN 978-94-007-1895-1. Retrieved 21 January 2012. 
  78. ^ Kane, Stephen R., Gelino, Dawn M. (2012). "The Habitable Zone and Extreme Planetary Orbits". Astrobiology 12 (10): 940–945. arXiv:1205.2429. Bibcode:2012AsBio..12..940K. doi:10.1089/ast.2011.0798. PMID 23035897. 
  79. ^ Wethington, Nicholos (September 16, 2008). "How Many Stars are in the Milky Way?". UniverseToday. Retrieved April 21, 2013. 
  80. ^ a b Torres, Abel Mendez (April 26, 2013). "Ten potentially habitable exoplanets now". Habitable Exoplanets Catalog. University of Puerto Rico. Retrieved April 29, 2013. 
  81. ^ Borenstein, Seth (19 February 2011). "Cosmic census finds crowd of planets in our galaxy". Associated Press. Retrieved 24 April 2011. 
  82. ^ Choi, Charles Q. (21 March 2011). "New Estimate for Alien Earths: 2 Billion in Our Galaxy Alone". Space.com. Retrieved 2011-04-24. 
  83. ^ Catanzarite, J.; Shao, M. (2011). "The Occurrence Rate of Earth Analog Planets Orbiting Sun-Like Stars". The Astrophysical Journal 738 (2): 151. arXiv:1103.1443. Bibcode:2011ApJ...738..151C. doi:10.1088/0004-637X/738/2/151.  edit
  84. ^ "70 Virginis b". Extrasolar Planet Guide. Extrasolar.net. Retrieved 2009-04-02. 
  85. ^ Williams, D., Pollard, D. (2002). "Earth-like worlds on eccentric orbits: excursions beyond the habitable zone". International Journal of Astrobiology 1 (1): 61–69. Bibcode:2002IJAsB...1...61W. doi:10.1017/S1473550402001064. 
  86. ^ Sudarsky, David et al. (2003). "Theoretical Spectra and Atmospheres of Extrasolar Giant Planets". The Astrophysical Journal 588 (2): 1121–1148. arXiv:astro-ph/0210216. Bibcode:2003ApJ...588.1121S. doi:10.1086/374331. 
  87. ^ Williams, D., Pollard, D. (2002). "Earth-like worlds on eccentric orbits: excursions beyond the habitable zone". International Journal of Astrobiology (Cambridge University Press) 1 (1): 61–69. Bibcode:2002IJAsB...1...61W. doi:10.1017/S1473550402001064. 
  88. ^ Jones, B. W.; Sleep, P. N.; Underwood, D. R. (2006). "Habitability of Known Exoplanetary Systems Based on Measured Stellar Properties". The Astrophysical Journal 649 (2): 1010. arXiv:astro-ph/0603200. Bibcode:2006ApJ...649.1010J. doi:10.1086/506557.  edit
  89. ^ Butler, R. P.; Wright, J. T.; Marcy, G. W.; Fischer, D. A.; Vogt, S. S.; Tinney, C. G.; Jones, H. R. A.; Carter, B. D.; Johnson, J. A.; McCarthy, C.; Penny, A. J. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal 646: 505. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.  edit
  90. ^ Barnes, J. W.; O’Brien, D. P. (2002). "Stability of Satellites around Close‐in Extrasolar Giant Planets". The Astrophysical Journal 575: 1087. arXiv:astro-ph/0205035. Bibcode:2002ApJ...575.1087B. doi:10.1086/341477.  edit
  91. ^ Canup, R. M.; Ward, W. R. (2006). "A common mass scaling for satellite systems of gaseous planets". Nature 441 (7095): 834–839. Bibcode:2006Natur.441..834C. doi:10.1038/nature04860. PMID 16778883.  edit
  92. ^ Lovis et al. (2006). "An extrasolar planetary system with three Neptune-mass planets". Nature 441 (7091): 305–309. arXiv:astro-ph/0703024. Bibcode:2006Natur.441..305L. doi:10.1038/nature04828. PMID 16710412. 
  93. ^ a b "Astronomers Discover Record Fifth Planet Around Nearby Star 55 Cancri". Sciencedaily.com. November 6, 2007. Archived from the original on 26 September 2008. Retrieved 2008-09-14. 
  94. ^ Fischer, Debra A. et al. (2008). "Five Planets Orbiting 55 Cancri". The Astrophysical Journal 675 (1): 790–801. arXiv:0712.3917. Bibcode:2008ApJ...675..790F. doi:10.1086/525512. 
  95. ^ Ian Sample, science correspondent (7 November 2007). "Could this be Earth's near twin? Introducing planet 55 Cancri f". London: The Guardian. Archived from the original on 2 October 2008. Retrieved 17 October 2008. 
  96. ^ Than, Ker (2007-02-24). "Planet Hunters Edge Closer to Their Holy Grail". space.com. Retrieved 2007-04-29. 
  97. ^ Robertson, Paul; Mahadevan, Suvrath; Endl, Michael; Roy, Arpita (3 July 2014). "Stellar activity masquerading as planets in the habitable zone of the M dwarf Gliese 581". Science (journal). arXiv:1407.1049. doi:10.1126/science.1253253. 
  98. ^ "Researchers find potentially habitable planet" (in French). maxisciences.com. Retrieved 2011-08-31. 
  99. ^ Schulze-Makuch, D.; Méndez, A.; Fairén, A. G.; Von Paris, P.; Turse, C.; Boyer, G.; Davila, A. F.; António, M. R. D. S.; Catling, D.; Irwin, L. N. (2011). "A Two-Tiered Approach to Assessing the Habitability of Exoplanets". Astrobiology 11 (10): 1041–1052. Bibcode:2011AsBio..11.1041S. doi:10.1089/ast.2010.0592. PMID 22017274.  edit
  100. ^ "Kepler 22-b: Earth-like planet confirmed". BBC. December 5, 2011. Retrieved May 2, 2013. 
  101. ^ Scharf, Caleb A. (2011-12-08). "You Can't Always Tell an Exoplanet by Its Size". Scientific American. Retrieved 2012-09-20. : "If it [Kepler-22b] had a similar composition to Earth, then we're looking at a world in excess of about 40 Earth masses".
  102. ^ Anglada-Escude, Guillem; Arriagada, Pamela; Vogt, Steven; Rivera, Eugenio J.; Butler, R. Paul; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B. et al. (2012). "A planetary system around the nearby M dwarf GJ 667C with at least one super-Earth in its habitable zone". arXiv:1202.0446 [astro-ph.EP].
  103. ^ Anglada-Escudé, Guillem; Tuomi, Mikko; Gerlach, Enrico; Barnes, Rory; Heller, René; Jenkins, James S.; Wende, Sebastian; Vogt, Steven S.; Butler, R. Paul; Reiners, Ansgar; Jones, Hugh R. A. (2013-06-07). "A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone". Astronomy & Astrophysics. arXiv:1306.6074. Bibcode:2013A&A...556A.126A. doi:10.1051/0004-6361/201321331. Retrieved 2013-06-25. 
  104. ^ Staff (September 20, 2012). "LHS 188 -- High proper-motion Star". Centre de données astronomiques de Strasbourg (Strasbourg astronomical Data Center). Retrieved September 20, 2012. 
  105. ^ Méndez, Abel (August 29, 2012). "A Hot Potential Habitable Exoplanet around Gliese 163". University of Puerto Rico at Arecibo (Planetary Habitability Laboratory). Retrieved September 20, 2012. 
  106. ^ Redd (September 20, 2012). "Newfound Alien Planet a Top Contender to Host Life". Space.com. Retrieved September 20, 2012. 
  107. ^ "A Hot Potential Habitable Exoplanet around Gliese 163". Spacedaily.com. Retrieved 2013-02-10. 
  108. ^ Tuomi, Mikko; Anglada-Escude, Guillem; Gerlach, Enrico; Jones, Hugh R. R.; Reiners, Ansgar; Rivera, Eugenio J.; Vogt, Steven S.; Butler, Paul (2012). "Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307". Astronomy and Astrophysics (accepted) 549: A48. arXiv:1211.1617. Bibcode:2013A&A...549A..48T. doi:10.1051/0004-6361/201220268. 
  109. ^ Aron, Jacob (December 19, 2012). "Nearby Tau Ceti may host two planets suited to life". New Scientist. Reed Business Information. Retrieved April 1, 2013. 
  110. ^ Tuomi, M.; Jones, H. R. A.; Jenkins, J. S.; Tinney, C. G.; Butler, R. P.; Vogt, S. S.; Barnes, J. R.; Wittenmyer, R. A.; o’Toole, S.; Horner, J.; Bailey, J.; Carter, B. D.; Wright, D. J.; Salter, G. S.; Pinfield, D. (2013). "Signals embedded in the radial velocity noise". Astronomy & Astrophysics 551: A79. arXiv:1212.4277. Bibcode:2013A&A...551A..79T. doi:10.1051/0004-6361/201220509.  edit
  111. ^ Torres, Abel Mendez (May 1, 2013). "The Habitable Exoplanets Catalog". Habitable Exoplanets Catalog. University of Puerto Rico. Retrieved May 1, 2013. 
  112. ^ Lauren M. Weiss, and Geoffrey W. Marcy. "The mass-radius relation for 65 exoplanets smaller than 4 Earth radii"
  113. ^ Moskowitz, Clara (January 9, 2013). "Most Earth-Like Alien Planet Possibly Found". Space.com. Retrieved January 9, 2013. 
  114. ^ Barclay, Thomas; Burke, Christopher J.; Howell, Steve B.; Rowe, Jason F.; Huber, Daniel; Isaacson, Howard; Jenkins, Jon M.; Kolbl, Rea; Marcy, Geoffrey W. (2013). "A Super-Earth-Sized Planet Orbiting in or Near the Habitable Zone Around a Sun-Like Star". The Astrophysical Journal 768 (2): 101. arXiv:1304.4941. Bibcode:2013ApJ...768..101B. doi:10.1088/0004-637X/768/2/101. 
  115. ^ a b Johnson, Michele; Harrington, J.D. (18 April 2013). "NASA's Kepler Discovers Its Smallest 'Habitable Zone' Planets to Date". NASA. Retrieved 18 April 2013. 
  116. ^ a b Overbye, Dennis (18 April 2013). "Two Promising Places to Live, 1,200 Light-Years from Earth". New York Times. Retrieved 18 April 2013. 
  117. ^ Borucki, William J.; et al. (18 April 2013). "Kepler-62: A Five-Planet System with Planets of 1.4 and 1.6 Earth Radii in the Habitable Zone". Science Express 340 (6132): 587. arXiv:1304.7387. Bibcode:2013Sci...340..587B. doi:10.1126/science.1234702. Retrieved 18 April 2013. 
  118. ^ Chang, Kenneth (17 April 2014). "Scientists Find an ‘Earth Twin,’ or Maybe a Cousin". New York Times. Retrieved 17 April 2014. 
  119. ^ Chang, Alicia (17 April 2014). "Astronomers spot most Earth-like planet yet". AP News. Retrieved 17 April 2014. 
  120. ^ Morelle, Rebecca (17 April 2014). "'Most Earth-like planet yet' spotted by Kepler". BBC News. Retrieved 17 April 2014. 
  121. ^ Torres, Abel (2012-06-12). "Liquid Water in the Solar System". Retrieved 2013-12-15. 
  122. ^ Nicholson, W. L.; Moeller, R.; Horneck, G.; (The Protect Team) (2012). "Transcriptomic Responses of GerminatingBacillus subtilisSpores Exposed to 1.5 Years of Space and Simulated Martian Conditions on the EXPOSE-E Experiment PROTECT". Astrobiology 12 (5): 469–86. Bibcode:2012AsBio..12..469N. doi:10.1089/ast.2011.0748. PMID 22680693. 
  123. ^ Munro, Margaret (2013), "Miners deep underground in northern Ontario find the oldest water ever known", National Post, retrieved 2013-10-06 
  124. ^ Davies, Paul (2013), The Origin of Life II: How did it begin?, retrieved 2013-10-06 
  125. ^ Taylor, Geoffrey (1996), "Life Underground", Planetary Science Research, retrieved 2013-10-06 
  126. ^ Doyle, Alister (4 March 2013), "Deep underground, worms and "zombie microbes" rule", Reuters, retrieved 2013-10-06 
  127. ^ Decker, Heinz; Holde, Kensal E. (2011). "Oxygen and the Exploration of the Universe". Oxygen and the Evolution of Life. pp. 157–168. doi:10.1007/978-3-642-13179-0_9. ISBN 978-3-642-13178-3. 
  128. ^ a b Stewart, Ian; Cohen, Jack (2002). Evolving the Alien. Ebury Press. ISBN 978-0-09-187927-3. 
  129. ^ Goldsmith, Donald; Owen, Tobias (1992). The Search for Life in the Universe (2 ed.). Addison-Wesley. p. 247. ISBN 0-201-56949-3. 
  130. ^ Guidetti, R. & Jönsson, K.I. (2002). "Long-term anhydrobiotic survival in semi-terrestrial micrometazoans". Journal of Zoology 257 (2): 181–187. doi:10.1017/S095283690200078X. 
  131. ^ Baldwin, Emily (26 April 2012). "Lichen survives harsh Mars environment". Skymania News. Retrieved 27 April 2012. 
  132. ^ de Vera, J.-P.; Kohler, Ulrich (26 April 2012). "The adaptation potential of extremophiles to Martian surface conditions and its implication for the habitability of Mars". European Geosciences Union. Retrieved 27 April 2012. 
  133. ^ Palca, Joe (September 29, 2010). "'Goldilocks' Planet's Temperature Just Right For Life". NPR (NPR). Retrieved April 5, 2011. 
  134. ^ "Project Cyclops: A design study of a system for detecting extraterrestrial intelligent life". NASA. 1971. Retrieved June 28, 2009. 
  135. ^ Joseph A. Angelo (2007). Life in the Universe. Infobase Publishing. p. 163. ISBN 978-1-4381-0892-6. Retrieved 26 June 2013. 
  136. ^ Turnbull, Margaret C.; Tarter, Jill C. (2003). "Target Selection for SETI. I. A Catalog of Nearby Habitable Stellar Systems". The Astrophysical Journal Supplement Series 145 (1): 181–198. arXiv:astro-ph/0210675. Bibcode:2003ApJS..145..181T. doi:10.1086/345779. 
  137. ^ Siemion, Andrew P. V.; Demorest, Paul; Korpela, Eric; Maddalena, Ron J.; Werthimer, Dan; Cobb, Jeff; Howard, Andrew W.; Langston, Glen; Lebofsky, Matt (2013). "A 1.1 to 1.9 GHz SETI Survey of the Kepler Field: I. A Search for Narrow-band Emission from Select Targets". The Astrophysical Journal 767 (1): 94. arXiv:1302.0845. Bibcode:2013ApJ...767...94S. doi:10.1088/0004-637X/767/1/94. 
  138. ^ Wall, Mike (2011). "HabStars: Speeding Up In the Zone". Retrieved 2013-06-26 
  139. ^ Zaitsev, A. L. (June 2004). "Передача и поиски разумных сигналов во Вселенной". Horizons of the Universe. National Astronomical Conference (in Russian). Moscow. Retrieved 2013-06-30. 
  140. ^ Grinspoon, David (12 December 2007). "Who Speaks for Earth?". Seedmagazine.com. Retrieved 2012-08-21. 
  141. ^ P. C. Gregory, D. A. Fischer (2010). "A Bayesian periodogram finds evidence for three planets in 47 Ursae Majoris". Monthly Notices of the Royal Astronomical Society 403 (2): 731–747. arXiv:1003.5549. Bibcode:2010MNRAS.403..731G. doi:10.1111/j.1365-2966.2009.16233.x. 
  142. ^ B. Jones; Underwood, David R. et al. (2005). "Prospects for Habitable "Earths" in Known Exoplanetary Systems". Astrophysical Journal 622 (2): 1091–1101. arXiv:astro-ph/0503178. Bibcode:2005ApJ...622.1091J. doi:10.1086/428108. 
  143. ^ Moore, Matthew (October 9, 2008). "Messages from Earth sent to distant planet by Bebo". London: .telegraph.co.uk. Archived from the original on 11 October 2008. Retrieved 2008-10-09. 

External links[edit]