Wikipedia

Habitable zone

(Redirected from Circumstellar habitable zone)
"Goldilocks Zone" redirects here. For the more general principle, see Goldilocks principle.
This article is about the circumstellar zone. For the galactic zone, see Galactic habitable zone.

In astronomy and astrobiology, the habitable zone (HZ), or more precisely the circumstellar habitable zone (CHZ), is the range of orbits around a star within which a planetary surface can support liquid water given sufficient atmospheric pressure.[1][2][3][4][5] The bounds of the HZ are based on Earth's position in the Solar System and the amount of radiant energy it receives from the Sun. Due to the importance of liquid water to Earth's biosphere, the nature of the HZ and the objects within it may be instrumental in determining the scope and distribution of planets capable of supporting Earth-like extraterrestrial life and intelligence.

A diagram depicting the habitable zone boundaries around stars, and how the boundaries are affected by star type. This plot includes Solar System planets (Venus, Earth, and Mars) as well as especially significant exoplanets such as TRAPPIST-1d, Kepler-186f, and our nearest neighbor Proxima Centauri b.

The habitable zone is also called the Goldilocks zone, a metaphor, allusion and antonomasia of the children's fairy tale of "Goldilocks and the Three Bears", in which a little girl chooses from sets of three items, rejecting the ones that are too extreme (large or small, hot or cold, etc.), and settling on the one in the middle, which is "just right".

Since the concept was first presented in 1953,[6] many stars have been confirmed to possess an HZ planet, including some systems that consist of multiple HZ planets.[7] Most such planets, being either super-Earths or gas giants, are more massive than Earth, because massive planets are easier to detect.[8] On November 4, 2013, astronomers reported, based on Kepler space telescope data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of Sun-like stars and red dwarfs in the Milky Way.[9][10] About 11 billion of these may be orbiting Sun-like stars.[11] Proxima Centauri b, located about 4.2 light-years (1.3 parsecs) from Earth in the constellation of Centaurus, is the nearest known exoplanet, and is orbiting in the habitable zone of its star.[12] The HZ is also of particular interest to the emerging field of habitability of natural satellites, because planetary-mass moons in the HZ might outnumber planets.[13]

In subsequent decades, the HZ concept began to be challenged as a primary criterion for life, so the concept is still evolving.[14] Since the discovery of evidence for extraterrestrial liquid water, substantial quantities of it are now thought to occur outside the circumstellar habitable zone. The concept of deep biospheres, like Earth's, that exist independently of stellar energy, are now generally accepted in astrobiology given the large amount of liquid water known to exist in lithospheres and asthenospheres of the Solar System.[15] Sustained by other energy sources, such as tidal heating[16][17] or radioactive decay[18] or pressurized by non-atmospheric means, liquid water may be found even on rogue planets, or their moons.[19] Liquid water can also exist at a wider range of temperatures and pressures as a solution, for example with sodium chlorides in seawater on Earth, chlorides and sulphates on equatorial Mars,[20] or ammoniates,[21] due to its different colligative properties. 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.[22]

History

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An estimate of the range of distances from the Sun allowing the existence of liquid water appears in Newton's Principia (Book III, Section 1, corol. 4).[23] The philosopher Louis Claude de Saint-Martin speculated in his 1802 work Man: His True Nature and Ministry, "... we may presume, that, being susceptible of vegetation, it [the Earth] has been placed, in the series of planets, in the rank which was necessary, and at exactly the right distance from the sun, to accomplish its secondary object of vegetation; and from this we might infer that the other planets are either too near or too remote from the sun, to vegetate."[24]

The concept of a circumstellar habitable zone was first introduced[25] in 1913, by Edward Maunder in his book "Are The Planets Inhabited?".[26] The concept was later discussed 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.[6][27] In the same year, Harlow Shapley wrote "Liquid Water Belt", which described the same concept in further scientific detail. Both works stressed the importance of liquid water to life.[28] 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.[29][30] A major early contributor to the habitable zone concept, 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.[31]

The concept of habitable zones was further developed in 1964 by Stephen H. Dole in his book Habitable Planets for Man, in which he discussed the concept of the circumstellar habitable zone 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.[2] 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.[32] 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.[33] 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.[29] Kasting was the first to present a detailed model for the habitable zone for exoplanets.[3][34]

An update to habitable zone concept 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.[35][36] 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.[35]

Subsequently, some astrobiologists propose that the concept be extended to other solvents, including dihydrogen, sulfuric acid, dinitrogen, formamide, and methane, among others, which would support hypothetical life forms that use an alternative biochemistry.[22] In 2013, further developments in habitable zone concepts were made with the proposal of a circum planetary 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.[37]

It has been noted that the current term of 'circumstellar habitable zone' poses confusion as the name suggests that planets within this region will possess a habitable environment.[38][39] However, surface conditions are dependent on a host of different individual properties of that planet.[38][39] This misunderstanding is reflected in excited reports of 'habitable planets'.[40][41][42] Since it is completely unknown whether conditions on these distant HZ worlds could host life, different terminology is needed.[39][41][43][44]

Determination

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Thermodynamic properties of water depicting the conditions at the surface of the terrestrial planets: Mars is near the triple point, Earth in the liquid; and Venus near the critical point.
 
The range of published estimates for the extent of the Sun's HZ. The conservative HZ[2] is indicated by a dark-green band crossing the inner edge of the aphelion of Venus, whereas an extended HZ,[45] 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 can remain habitable, complemented by a larger "extended habitable zone" in which a planet like Venus, with stronger greenhouse effects, can have the right temperature for liquid water to exist at the surface.[46]

Solar System estimates

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Estimates for the habitable zone within the Solar System range from 0.38 to 10.0 astronomical units,[47][48][49][50] though arriving at these estimates has been challenging for a variety of reasons. Numerous planetary mass objects orbit within, or close to, this range and as such receive sufficient sunlight to raise temperatures above the freezing point of water. However, their atmospheric conditions vary substantially.

The aphelion of Venus, for example, touches the inner edge of the zone in most estimates and while atmospheric pressure at the surface is sufficient for liquid water, a strong greenhouse effect raises surface temperatures to 462 °C (864 °F) at which water can only exist as vapor.[51] The entire orbits of the Moon,[52] Mars,[53] and numerous asteroids also lie within various estimates of the habitable zone. Only at Mars' lowest elevations (less than 30% of the planet's surface) is atmospheric pressure and temperature sufficient for water to, if present, exist in liquid form for short periods.[54] At Hellas Basin, for example, atmospheric pressures can reach 1,115 Pa and temperatures above zero Celsius (about the triple point for water) for 70 days in the Martian year.[54] Despite indirect evidence in the form of seasonal flows on warm Martian slopes,[55][56][57][58] no confirmation has been made of the presence of liquid water there. While other objects orbit partly within this zone, including comets, Ceres[59] is the only one of planetary mass. A combination of low mass and an inability to mitigate evaporation and atmosphere loss against the solar wind make it impossible for these bodies to sustain liquid water on their surface.

Despite this, studies are strongly suggestive of past liquid water on the surface of Venus,[60] Mars,[61][62][63] Vesta[64] and Ceres,[65][66] suggesting a more common phenomenon than previously thought. Since sustainable liquid water is thought to be essential to support complex life, most estimates, therefore, are inferred from the effect that a repositioned orbit would have on the habitability of Earth or Venus as their surface gravity allows sufficient atmosphere to be retained for several billion years.

According to the extended habitable zone concept, planetary-mass objects with atmospheres capable of inducing sufficient radiative forcing could possess liquid water farther out from the Sun. Such objects could include those whose atmospheres contain a high component of greenhouse gas and terrestrial planets much more massive than Earth (super-Earth class planets), that have retained atmospheres with surface pressures of up to 100 kbar. There are no examples of such objects in the Solar System to study; not enough is known about the nature of atmospheres of these kinds of extrasolar objects, and their position in the habitable zone cannot determine the net temperature effect of such atmospheres including induced albedo, anti-greenhouse or other possible heat sources.

For reference, the average distance from the Sun of some major bodies within the various estimates of the habitable zone is: Mercury, 0.39 AU; Venus, 0.72 AU; Earth, 1.00 AU; Mars, 1.52 AU; Vesta, 2.36 AU; Ceres and Pallas, 2.77 AU; Jupiter, 5.20 AU; Saturn, 9.58 AU. In the most conservative estimates, only Earth lies within the zone; in the most permissive estimates, even Saturn at perihelion, or Mercury at aphelion, might be included.

Estimates of the circumstellar habitable zone boundaries of the Solar System
Inner edge (AU) Outer edge (AU) Year Notes
0.725 1.24 1964, Dole[2] Used optically thin atmospheres and fixed albedos. Places the aphelion of Venus just inside the zone.
1.005–1.008 1969, Budyko[67] 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[68] and North 1975.[69]
0.92–0.96 1970, Rasool and De Bergh[70] Based on studies of Venus's atmosphere, Rasool and De Bergh concluded that this is the minimum distance at which Earth would have formed stable oceans.
0.958 1.004 1979, Hart[71] Based on computer modeling and simulations of the evolution of Earth's atmospheric composition and surface temperature. This estimate has often been cited by subsequent publications.
3.0 1992, Fogg[45] Used the carbon cycle to estimate the outer edge of the circumstellar habitable zone.
0.95 1.37 1993, Kasting et al.[29] Founded the most common working definition of the habitable zone used today. Assumes that CO2 and H2O are the key greenhouse gases as they are for the Earth. Argued that the habitable zone is wide because of the carbonate–silicate cycle. Noted the cooling effect of cloud albedo. Table shows conservative limits. Optimistic limits were 0.84–1.67 AU.
2.0 2010, Spiegel et al.[72] Proposed that seasonal liquid water is possible to this limit when combining high obliquity and orbital eccentricity.
0.75 2011, Abe et al.[73] Found that land-dominated "desert planets" with water at the poles could exist closer to the Sun than watery planets like Earth.
10 2011, Pierrehumbert and Gaidos[48] Terrestrial planets that accrete tens-to-thousands of bars of primordial hydrogen from the protoplanetary disc may be habitable at distances that extend as far out as 10 AU in the Solar System.
0.77–0.87 1.02–1.18 2013, Vladilo et al.[74] Inner edge of the circumstellar habitable zone is closer and outer edge is farther for higher atmospheric pressures; determined minimum atmospheric pressure required to be 15 mbar.
0.99 1.67 2013, Kopparapu et al.[4][75] Revised estimates of the Kasting et al. (1993) formulation using updated moist 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 moist greenhouse limit. As with Kasting et al. (1993), this applies to an Earth-like planet where the "water loss" (moist greenhouse) limit, at the inner edge of the habitable zone, is where the temperature has reached around 60 Celsius and is high enough, right up into the troposphere, that the atmosphere has become fully saturated with water vapor. Once the stratosphere becomes wet, water vapor photolysis releases hydrogen into space. At this point cloud feedback cooling does not increase significantly with further warming. The "maximum greenhouse" limit, at the outer edge, is where a CO2 dominated atmosphere, of around 8 bars, has produced the maximum amount of greenhouse warming, and further increases in CO2 will not create enough warming to prevent CO2 catastrophically freezing out of the atmosphere. Optimistic limits were 0.97–1.67 AU. This definition does not take into account possible radiative warming by CO2 clouds.
0.38 2013, Zsom et al.
[47]		 Estimate based on various possible combinations of atmospheric composition, pressure and relative humidity of the planet's atmosphere.
0.95 2013, Leconte et al.[76] Using 3-D models, these authors computed an inner edge of 0.95 AU for the Solar System.
0.95 2.4 2017, Ramirez and Kaltenegger
[49]		 An expansion of the classical carbon dioxide-water vapor habitable zone[29] assuming a volcanic hydrogen atmospheric concentration of 50%.
0.93–0.91 2019, Gomez-Leal et al.
[77]		 Estimation of the moist greenhouse threshold by measuring the water mixing ratio in the lower stratosphere, the surface temperature, and the climate sensitivity on an Earth analog with and without ozone, using a global climate model (GCM). It shows the correlation of a water mixing ratio value of 7 g/kg, a surface temperature of about 320 K, and a peak of the climate sensitivity in both cases.
0.99 1.004 Tightest bounded estimate from above
0.38 10 Most relaxed estimate from above

Extrasolar extrapolation

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See also: Habitability of red dwarf systems and Habitability of K-type main-sequence star systems

Astronomers use stellar flux and the inverse-square law to extrapolate circumstellar habitable zone models created for the Solar System to other stars. For example, according to Kopparapu's habitable zone estimate, although the Solar System has a circumstellar habitable zone centered at 1.34 AU from the Sun,[4] a star with 0.25 times the luminosity of the Sun would have a habitable zone centered at  , 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 HZ concept is more complex.

Spectral types and star-system characteristics

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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.[78] 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.[79][80]

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.[81] Studying ultraviolet emissions, Andrea Buccino found that only 40% of stars studied (including the Sun) had overlapping liquid water and ultraviolet habitable zones.[82] Stars smaller than the Sun, on the other hand, have distinct impediments to habitability. For example, Michael Hart proposed that only main-sequence stars of spectral class K0 or brighter could offer 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 hospitable environment for life.[83]

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 modeling from 2013 supports the idea that red dwarf stars can support planets with relatively constant temperatures over their surfaces in spite of tidal locking.[84] Astronomy professor Eric Agol argues that even white dwarfs may support a relatively brief habitable zone through planetary migration.[85] At the same time, others have written in similar support of semi-stable, temporary habitable zones around brown dwarfs.[83] Also, a habitable zone in the outer parts of stellar systems may exist during the pre-main-sequence phase of stellar evolution, especially around M-dwarfs, potentially lasting for billion-year timescales.[86]

Stellar evolution

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Natural shielding 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,[87] 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.[88][89] Even while stars are on the main sequence, though, their energy output steadily increases, pushing their habitable zones farther out; our Sun, for example, was 75% as bright in the Archaean as it is now,[90] 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.[91] 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. Like the general circumstellar habitable zone, the continuously habitable zone of a star is divided into a conservative and extended region.[91]

In red dwarf systems, gigantic stellar flares which could double a star's brightness in minutes[92] and huge starspots which can cover 20% of the star's surface area,[93] have the potential to strip an otherwise habitable planet of its atmosphere and water.[94] As with more massive stars, though, stellar evolution changes their nature and energy flux,[95] so by about 1.2 billion years of age, red dwarfs generally become sufficiently constant to allow for the development of life.[94][96]

Once a star has evolved sufficiently to become a red giant, its circumstellar habitable zone will change dramatically from its main-sequence size.[97] For example, the Sun is expected to engulf the previously habitable Earth as a red giant.[98][99] However, once a red giant star reaches the horizontal branch, it achieves a new equilibrium and can sustain a new circumstellar habitable zone, which in the case of the Sun would range from 7 to 22 AU.[100] At such stage, Saturn's moon Titan would likely be habitable in Earth's temperature sense.[101] 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.[100] However, around such a helium-burning star, important life processes like photosynthesis could only happen around planets where the atmosphere has 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.[102] Moreover, as Ramirez and Kaltenegger (2016)[99] showed, intense stellar winds would completely remove the atmospheres of such smaller planetary bodies, rendering them uninhabitable anyway. Thus, Titan would not be habitable even after the Sun becomes a red giant.[99] Nevertheless, life need not originate during this stage of stellar evolution for it to be detected. Once the star becomes a red giant, and the habitable zone extends outward, the icy surface would melt, forming a temporary atmosphere that can be searched for signs of life that may have been thriving before the start of the red giant stage.[99]

Desert planets

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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.[103][104]

Other considerations

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Earth's hydrosphere. Water covers 71% of Earth's surface, with the global ocean accounting for 97.3% of the water distribution on Earth.
See also: Planetary habitability and Habitability of natural satellites

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 not completely understood; possible sources include the result of impacts with icy bodies, outgassing, mineralization, leakage from hydrous minerals from the lithosphere, and photolysis.[105][106] 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[107] such as GJ 1214 b[108][109] or Kepler-22b may be.[110]

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.[111] Atmospheres are thought to be maintained through similar processes along with biogeochemical cycles and the mitigation of atmospheric escape.[112] 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.[74] Below an atmospheric pressure of about 15 millibars, it was found that habitability could not be maintained[74] because even a small shift in pressure or temperature could render water unable to form as a liquid.[113]

Although traditional definitions of the habitable zone assume that carbon dioxide and water vapor are the most important greenhouse gases (as they are on the Earth),[29] a study[49] led by Ramses Ramirez and co-author Lisa Kaltenegger has shown that the size of the habitable zone is greatly increased if prodigious volcanic outgassing of hydrogen is also included along with the carbon dioxide and water vapor. The outer edge in the Solar System would extend out as far as 2.4 AU in that case. Similar increases in the size of the habitable zone were computed for other stellar systems. An earlier study by Ray Pierrehumbert and Eric Gaidos[48] had eliminated the CO2-H2O concept entirely, arguing that young planets could accrete many tens to hundreds of bars of hydrogen from the protoplanetary disc, providing enough of a greenhouse effect to extend the solar system outer edge to 10 AU. In this case, though, the hydrogen is not continuously replenished by volcanism and is lost within millions to tens of millions of years.

In the case of planets orbiting in the HZs 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 thought to cause extreme heat on the star-facing side and bitter cold on the opposite side, making many red dwarf planets uninhabitable; however, three-dimensional climate models in 2013 showed that the side of a red dwarf planet facing the host star could have extensive cloud cover, increasing its bond albedo and reducing significantly temperature differences between the two sides.[84]

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.[37] More specifically, moons need to be far enough from their host giant planets that they are not transformed by tidal heating into volcanic worlds like Io,[37] but must remain within the Hill radius of the planet so that they are not pulled out of the orbit of their host planet.[114] Red dwarfs that have masses less than 20% 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 the 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.[37]

 
Artist's concept of a planet on an eccentric orbit that passes through the HZ for only part of its orbit

A planetary object that orbits a star with high orbital eccentricity may spend only some of its year in the HZ 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 temperature between 0.150 K (−273 °C)[115] and 424 K (151 °C).[116] Life on a planetary object orbiting outside HZ 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.[117]

Extrasolar discoveries

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See also: List of potentially habitable exoplanets

A 2015 review concluded that the exoplanets Kepler-62f, Kepler-186f and Kepler-442b were likely the best candidates for being potentially habitable.[118] These are at a distance of 990, 490 and 1,120 light-years away, respectively. Of these, Kepler-186f is closest in size to Earth with 1.2 times Earth's radius, and it is located towards the outer edge of the habitable zone around its red dwarf star. Among nearest terrestrial exoplanet candidates, Tau Ceti e is 11.9 light-years away. It is in the inner edge of its planetary system's habitable zone, giving it an estimated average surface temperature of 68 °C (154 °F).[119]

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 HZ, at 0.48,[4] meaning that there may be roughly 95–180 billion habitable planets in the Milky Way.[120] However, this is merely a statistical prediction; only a small fraction of these possible planets have yet been discovered.[121]

Previous studies have been more conservative. In 2011, Seth Borenstein concluded that there are roughly 500 million habitable planets in the Milky Way.[122] NASA's Jet Propulsion Laboratory 2011 study, based on observations from the Kepler mission, raised the number somewhat, estimating 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 HZs.[123][124]

Early findings

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See also: Category:Giant planets in the habitable zone

The first discoveries of extrasolar planets in the HZ occurred just a few years after the first extrasolar planets were discovered. However, these early detections were all gas giant-sized, and many were in eccentric orbits. Despite this, studies indicate the possibility of large, Earth-like moons around these planets supporting liquid water.[125] 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.[126] 16 Cygni Bb, also discovered in 1996, has an extremely eccentric orbit that spends only part of its time in the HZ, such an orbit would causes extreme seasonal effects. In spite of this, simulations have suggested that a sufficiently large companion could support surface water year-round.[127]

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 that may also have large moons.[128] Another gas giant, Upsilon Andromedae d was discovered in 1999 orbiting Upsilon Andromidae's habitable zone.

Announced on April 4, 2001, HD 28185 b is a gas giant found to orbit entirely within its star's circumstellar habitable zone[129] and has a low orbital eccentricity, comparable to that of Mars in the Solar System.[130] Tidal interactions suggest it could harbor habitable Earth-mass satellites in orbit around it for many billions of years,[131] though it is unclear whether such satellites could form in the first place.[132]

HD 69830 d, a gas giant with 17 times the mass of Earth, was found in 2006 orbiting within the circumstellar habitable zone of HD 69830, 41 light years away from Earth.[133] The following year, 55 Cancri f was discovered within the HZ of its host star 55 Cancri A.[134][135] Hypothetical satellites with sufficient mass and composition are thought to be able to support liquid water at their surfaces.[136]

Though, in theory, such giant planets could possess moons, the technology did not exist to detect moons around them, and no extrasolar moons had been discovered. Planets within the zone with the potential for solid surfaces were therefore of much higher interest.

Habitable super-Earths

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See also: Category:Super-Earths in the habitable zone
 
The habitable zone of Gliese 581 compared with the Solar System's habitable zone.

The 2007 discovery of Gliese 581c, 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 extreme surface conditions that may resemble Venus.[137] 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, but only for a short time. As of 2015, the planet has no newer disconfirmations. 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,[138] and astronomers are divided about its existence.

 
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

Discovered in August 2011, HD 85512 b was initially speculated to be habitable,[139] but the new circumstellar habitable zone criteria devised by Kopparapu et al. in 2013 place the planet outside the circumstellar habitable zone.[121]

Kepler-22 b, discovered in December 2011 by the Kepler space probe,[140] is the first transiting exoplanet discovered around a Sun-like star. With a radius 2.4 times that of Earth, Kepler-22b has been predicted by some to be an ocean planet.[141] Gliese 667 Cc, discovered in 2011 but announced in 2012,[142] is a super-Earth orbiting in the circumstellar habitable zone of Gliese 667 C. It is one of the most Earth-like planets known.

Gliese 163 c, discovered in September 2012 in orbit around the red dwarf Gliese 163[143] 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.[144][145][146] HD 40307 g, a candidate planet tentatively discovered in November 2012, is in the circumstellar habitable zone of HD 40307.[147] In December 2012, Tau Ceti e and Tau Ceti f were found in the circumstellar habitable zone of Tau Ceti, a Sun-like star 12 light years away.[148] Although more massive than Earth, they are among the least massive planets found to date orbiting in the habitable zone;[149] however, Tau Ceti f, like HD 85512 b, did not fit the new circumstellar habitable zone criteria established by the 2013 Kopparapu study.[150] It is now considered as uninhabitable.

Near Earth-sized planets and Solar analogs

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Comparison of the HZ position of Earth-radius planet Kepler-186f and the Solar System (17 April 2014)
 
While larger than Kepler 186f, Kepler-452b's orbit and star are more similar to Earth's.

Recent discoveries have uncovered planets that are thought to be similar in size or mass to Earth. "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 R🜨 the average planet density rapidly decreases with increasing radius, indicating these planets have a significant fraction of volatiles by volume overlying a rocky core.[151] A genuinely Earth-like planet – an Earth analog or "Earth twin" – would need to meet many conditions beyond size and mass; such properties are not observable using current technology.

A solar analog (or "solar twin") is a star that resembles the Sun. No solar twin with an exact match as that of the Sun has been found. However, some stars are nearly identical to the Sun and are considered solar twins. An exact solar twin would be a G2V star with a 5,778 K temperature, be 4.6 billion years old, with the correct metallicity and a 0.1% solar luminosity variation.[152] Stars with an age of 4.6 billion years are at the most stable state. Proper metallicity and size are also critical to low luminosity variation.[153][154][155]

Using data collected by NASA's Kepler space telescope and the W. M. Keck Observatory, scientists have estimated that 22% of solar-type stars in the Milky Way galaxy have Earth-sized planets in their habitable zone.[156]

On 7 January 2013, astronomers from the Kepler team announced the discovery of Kepler-69c (formerly KOI-172.02), an Earth-size exoplanet candidate (1.7 times the radius of Earth) orbiting Kepler-69, a star similar to the Sun, in the HZ and expected to offer habitable conditions.[157][158][159][160] 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.[159][160][161]

With a radius estimated 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[162][163][164] though its mass remains unknown and its parent star is not a Solar analog.

Kapteyn b, discovered in June 2014 is a possible rocky world of about 4.8 Earth masses and about 1.5 Earth radii were found orbiting the habitable zone of the red subdwarf Kapteyn's Star, 12.8 light-years away.[165]

On 6 January 2015, NASA announced the 1000th confirmed exoplanet discovered by the Kepler Space Telescope. Three of the newly confirmed exoplanets were found to orbit within habitable zones of their related stars: two of the three, Kepler-438b and Kepler-442b, are near-Earth-size and likely rocky; the third, Kepler-440b, is a super-Earth.[166] However, Kepler-438b is found to be a subject of powerful flares, so it is now considered uninhabitable. 16 January, K2-3d a planet of 1.5 Earth radii was found orbiting within the habitable zone of K2-3, receiving 1.4 times the intensity of visible light as Earth.[167]

Kepler-452b, announced on 23 July 2015 is 50% bigger than Earth, likely rocky and takes approximately 385 Earth days to orbit the habitable zone of its G-class (solar analog) star Kepler-452.[168][169]

The discovery of a system of three tidally-locked planets orbiting the habitable zone of an ultracool dwarf star, TRAPPIST-1, was announced in May 2016.[170] The discovery is considered significant because it dramatically increases the possibility of smaller, cooler, more numerous and closer stars possessing habitable planets.

Two potentially habitable planets, discovered by the K2 mission in July 2016 orbiting around the M dwarf K2-72 around 227 light years from the Sun: K2-72c and K2-72e are both of similar size to Earth and receive similar amounts of stellar radiation.[171]

Announced on the 20 April 2017, LHS 1140b is a super-dense super-Earth 39 light years away, 6.6 times Earth's mass and 1.4 times radius, its star 15% the mass of the Sun but with much less observable stellar flare activity than most M dwarfs.[172] The planet is one of few observable by both transit and radial velocity that's mass is confirmed with an atmosphere may be studied.

Discovered by radial velocity in June 2017, with approximately three times the mass of Earth, Luyten b orbits within the habitable zone of Luyten's Star just 12.2 light-years away.[173]

At 11 light-years away, the second closest planet, Ross 128 b, was announced in November 2017 following a decade's radial velocity study of relatively "quiet" red dwarf star Ross 128. At 1.35 times Earth's mass, is it roughly Earth-sized and likely rocky in composition.[174]

Discovered in March 2018, K2-155d is about 1.64 times the radius of Earth, is likely rocky and orbits in the habitable zone of its red dwarf star 203 light years away.[175][176][177]

One of the earliest discoveries by the Transiting Exoplanet Survey Satellite (TESS) announced on July 31, 2019, is a Super-Earth planet GJ 357 d orbiting the outer edge of a red dwarf 31 light years away.[178]

K2-18b is an exoplanet 124 light-years away, orbiting in the habitable zone of the K2-18, a red dwarf. This planet is significant for water vapor found in its atmosphere; this was announced on September 17, 2019.

In September 2020, astronomers identified 24 superhabitable planet (planets better than Earth) contenders, from among more than 4000 confirmed exoplanets at present, based on astrophysical parameters, as well as the natural history of known life forms on the Earth.[179]

Notable exoplanets – Kepler space telescope
 
Confirmed small exoplanets in habitable zones.
(Kepler-62e, Kepler-62f, Kepler-186f, Kepler-296e, Kepler-296f, Kepler-438b, Kepler-440b, Kepler-442b)
(Kepler Space Telescope; January 6, 2015).[166]

Habitability outside the HZ

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

Liquid-water environments have been found to exist in the absence of atmospheric pressure and at temperatures outside the HZ temperature range. For example, Saturn's moons Titan and Enceladus and Jupiter's moons Europa and Ganymede, all of which are outside the habitable zone, may hold large volumes of liquid water in subsurface oceans.[180]

Outside the HZ, tidal heating and radioactive decay are two possible heat sources that could contribute to the existence of liquid water.[16][17] Abbot and Switzer (2011) put forward the possibility that subsurface water could exist on rogue planets as a result of radioactive decay-based heating and insulation by a thick surface layer of ice.[19]

With some theorising that life on Earth may have actually originated in stable, subsurface habitats,[181][182] it has been suggested that it may be common for wet subsurface extraterrestrial habitats such as these to 'teem with life'.[183] On Earth itself, living organisms may be found more than 6 km (3.7 mi) below the surface.[184]

Another possibility is that outside the HZ organisms may use alternative biochemistries that do not require water at all. Astrobiologist Christopher McKay, has suggested that methane (CH
4) may be a solvent conducive to the development of "cryolife", with the Sun's "methane habitable zone" being centered on 1,610,000,000 km (1.0×109 mi; 11 AU) from the star.[22] This distance is coincident with the location of Titan, whose lakes and rain of methane make it an ideal location to find McKay's proposed cryolife.[22] In addition, testing of a number of organisms has found some are capable of surviving in extra-HZ conditions.[185]

Significance for complex and intelligent life

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The Rare Earth hypothesis argues that complex and intelligent life is uncommon and that the HZ is one of many critical factors. According to Ward & Brownlee (2004) and others, not only is a HZ 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)[35] and biochemical (the role of radiant energy in supporting photosynthesis for necessary atmospheric oxygenation).[186] 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 HZ.[187] Intelligent life outside the HZ may have evolved in subsurface environments, from alternative biochemistries[187] or even from nuclear reactions.[188]

On Earth, several complex multicellular life forms (or eukaryotes) have been identified with the potential to survive conditions that might exist outside the conservative habitable zone. Geothermal energy sustains ancient circumvent ecosystems, supporting large complex life forms such as Riftia pachyptila.[189] Similar environments may be found in oceans pressurised beneath solid crusts, such as those of Europa and Enceladus, outside of the habitable zone.[190] Numerous microorganisms have been tested in simulated conditions and in low Earth orbit, including eukaryotes. An animal example is the Milnesium tardigradum, which can withstand extreme temperatures well above the boiling point of water and the cold vacuum of outer space.[191] In addition, the lichens Rhizocarpon geographicum and Xanthoria elegans have 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.[192][193][194] The fungi Cryomyces antarcticus and Cryomyces minteri are also able to survive and reproduce in Mars-like conditions.[194]

Species, including humans, known to possess animal cognition require large amounts of energy,[195] and have adapted to specific conditions, including an abundance of atmospheric oxygen and the availability of large quantities of chemical energy synthesized from radiant energy. If humans are to colonize other planets, true Earth analogs in the HZ are most likely to provide the closest natural habitat; 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 or space habitat analogs on the surface may be eliminated, and complex Earth life can thrive.[2]

Planets in the HZ remain of paramount interest to researchers looking for intelligent life elsewhere in the universe.[196] The Drake equation, sometimes used to estimate the number of intelligent civilizations in our galaxy, contains the factor or parameter ne, which is the average number of planetary-mass objects orbiting within the HZ of each star. 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.[35] A 1971 NASA report by Drake and Bernard Oliver proposed the "water hole", based on the spectral absorption lines of the hydrogen and hydroxyl components of water, as a good, obvious band for communication with extraterrestrial intelligence[197][198] that has since been widely adopted by astronomers involved in the search for extraterrestrial intelligence. According to Jill Tarter, Margaret Turnbull and many others, HZ candidates are the priority targets to narrow waterhole searches[199][200] and the Allen Telescope Array now extends Project Phoenix to such candidates.[201]

Because the HZ 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 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 HZ.[202][203][204][205] The Teen Age Message was also directed to the 55 Cancri system, which has a gas giant in its HZ.[134] A Message from Earth in 2008,[206] and Hello From Earth in 2009, were directed to the Gliese 581 system, containing three planets in the HZ—Gliese 581 c, d, and the unconfirmed g.

See also

edit

References

edit
  1. ^ Su-Shu Huang, American Scientist 47, 3, pp. 397–402 (1959)
  2. ^ a b c d e Dole, Stephen H. (1964). Habitable Planets for Man. Blaisdell Publishing Company. p. 103.
  3. ^ a b J. F. Kasting, D. P. Whitmire, R. T. Reynolds, Icarus 101, 108 (1993).
  4. ^ 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. S2CID 119103101.
  5. ^ Cruz, Maria; Coontz, Robert (2013). "Exoplanets - Introduction to Special Issue". Science. 340 (6132): 565. doi:10.1126/science.340.6132.565. PMID 23641107.
  6. ^ a b Huggett, Richard J. (1995). Geoecology: An Evolutionary Approach. Routledge, Chapman & Hall. p. 10. ISBN 978-0-415-08689-9.
  7. ^ Overbye, Dennis (January 6, 2015). "As Ranks of Goldilocks Planets Grow, Astronomers Consider What's Next". The New York Times. Retrieved January 6, 2015.
  8. ^ Peale, S. J. (January 2021). "Probability of Detecting a Planetary Companion during a Microlensing Event". The Astrophysical Journal. 552 (2): 889–911. arXiv:astro-ph/0101316. doi:10.1086/320562. S2CID 17080374.
  9. ^ Overbye, Dennis (November 4, 2013). "Far-Off Planets Like the Earth Dot the Galaxy". The New York Times. Retrieved November 5, 2013.
  10. ^ 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. 110 (48): 19273–19278. arXiv:1311.6806. Bibcode:2013PNAS..11019273P. doi:10.1073/pnas.1319909110. PMC 3845182. PMID 24191033.
  11. ^ Khan, Amina (November 4, 2013). "Milky Way may host billions of Earth-size planets". Los Angeles Times. Retrieved November 5, 2013.
  12. ^ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv:1609.03449. Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID 27558064. S2CID 4451513.
  13. ^ Schirber, Michael (26 Oct 2009). "Detecting Life-Friendly Moons". Astrobiology Magazine. NASA. Archived from the original on 29 October 2009. Retrieved 9 May 2013.
  14. ^ Lammer, H.; Bredehöft, J. H.; Coustenis, A.; Khodachenko, M. L.; et al. (2009). "What makes a planet habitable?" (PDF). The Astronomy and Astrophysics Review. 17 (2): 181–249. Bibcode:2009A&ARv..17..181L. doi:10.1007/s00159-009-0019-z. S2CID 123220355. Archived from the original (PDF) on 2016-06-02. Retrieved 2016-05-03.
  15. ^ Edwards, Katrina J.; Becker, Keir; Colwell, Frederick (2012). "The Deep, Dark Energy Biosphere: Intraterrestrial Life on Earth". Annual Review of Earth and Planetary Sciences. 40 (1): 551–568. Bibcode:2012AREPS..40..551E. doi:10.1146/annurev-earth-042711-105500. ISSN 0084-6597.
  16. ^ a b Cowen, Ron (2008-06-07). "A Shifty Moon". Science News. Archived from the original on 2011-11-04. Retrieved 2013-04-22.
  17. ^ a b Bryner, Jeanna (24 June 2009). "Ocean Hidden Inside Saturn's Moon". Space.com. TechMediaNetwork. Retrieved 22 April 2013.
  18. ^ 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. S2CID 73631942.
  19. ^ a b "Rogue Planets Could Harbor Life in Interstellar Space, Say Astrobiologists". MIT Technology Review. MIT Technology Review. 9 February 2011. Archived from the original on 7 October 2015. Retrieved 24 June 2013.
  20. ^ Wall, Mike (28 September 2015). "Salty Water Flows on Mars Today, Boosting Odds for Life". Space.com. Retrieved 2015-09-28.
  21. ^ Sun, Jiming; Clark, Bryan K.; Torquato, Salvatore; Car, Roberto (2015). "The phase diagram of high-pressure superionic ice". Nature Communications. 6: 8156. Bibcode:2015NatCo...6.8156S. doi:10.1038/ncomms9156. ISSN 2041-1723. PMC 4560814. PMID 26315260.
  22. ^ 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.
  23. ^ Newton, Isaac (1729). "Book III - Section I - Proposition VIII - Corol. 4". Philosophiae Naturalis Principia Mathematica (PDF) (3rd ed.). p. 739. Archived (PDF) from the original on 13 November 2023.
  24. ^ de Saint-Martin, Louis Claude (1802). Man: His True Nature and Ministry. p. 78.
  25. ^ Lorenz, Ralph (2019). Exploring Planetary Climate: A History of Scientific Discovery on Earth, Mars, Venus and Titan. Cambridge University Press. p. 53. ISBN 978-1108471541.
  26. ^ Lorenz, Ralph (2020). "Maunder's Work on Planetary Habitability in 1913: Early Use of the term "Habitable Zone" and a "Drake Equation" Calculation". Research Notes of the American Astronomical Society. 4 (6): 79. Bibcode:2020RNAAS...4...79L. doi:10.3847/2515-5172/ab9831. S2CID 219930646.
  27. ^ Strughold, Hubertus (1953). The Green and Red Planet: A Physiological Study of the Possibility of Life on Mars. University of New Mexico Press.
  28. ^ Kasting, James (2010). How to Find a Habitable Planet. Princeton University Press. p. 127. ISBN 978-0-691-13805-3. Retrieved 4 May 2013.
  29. ^ a b c d e 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.
  30. ^ 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. Bibcode:1966elab.book.....S.
  31. ^ 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.
  32. ^ Gilster, Paul (2004). Centauri Dreams: Imagining and Planning Interstellar Exploration. Springer. p. 40. ISBN 978-0-387-00436-5.
  33. ^ "The Goldilocks Zone" (Press release). NASA. October 2, 2003. Archived from the original on August 29, 2011. Retrieved April 22, 2013.
  34. ^ Seager, Sara (2013). "Exoplanet Habitability". Science. 340 (577): 577–581. Bibcode:2013Sci...340..577S. doi:10.1126/science.1232226. PMID 23641111. S2CID 206546351.
  35. ^ a b c d Brownlee, Donald; Ward, Peter (2004). Rare Earth: Why Complex Life Is Uncommon in the Universe. New York: Copernicus. ISBN 978-0-387-95289-5.
  36. ^ Gonzalez, Guillermo; Brownlee, Donald; Ward, Peter (July 2001). "The Galactic Habitable Zone I. Galactic Chemical Evolution". Icarus. 152 (1): 185–200. arXiv:astro-ph/0103165. Bibcode:2001Icar..152..185G. doi:10.1006/icar.2001.6617. S2CID 18179704.
  37. ^ a b c d Hadhazy, Adam (April 3, 2013). "The 'Habitable Edge' of Exomoons". Astrobiology Magazine. NASA. Archived from the original on May 2, 2013. Retrieved April 22, 2013.
  38. ^ a b Tasker, Elizabeth; Tan, Joshua; Heng, Kevin; Kane, Stephen; Spiegel, David; Brasser, Ramon; Casey, Andrew; Desch, Steven; Dorn, Caroline; Hernlund, John; Houser, Christine (2017-02-02). "The language of exoplanet ranking metrics needs to change". Nature Astronomy. 1 (2): 0042. arXiv:1708.01363. Bibcode:2017NatAs...1E..42T. doi:10.1038/s41550-017-0042. S2CID 118952886.
  39. ^ a b c Neel V. Patel (2 October 2019). "No one agrees what it means for a planet to be "habitable"". MIT Technology Review. surface conditions are dependent on a host of different individual properties of that planet, such as internal and geological processes, magnetic field evolution, climate, atmospheric escape, rotational effects, tidal forces, orbits, star formation and evolution, unusual conditions like binary star systems, and gravitational perturbations from passing bodies.
  40. ^ Tan, Joshua (8 February 2017). "Until we get better tools, excited reports of 'habitable planets' need to come back down to Earth". The Conversation. Retrieved 2019-10-21.
  41. ^ a b "Why just being in the habitable zone doesn't make exoplanets livable". Science News. 2019-10-04. Retrieved 2019-10-21.
  42. ^ No, the Exoplanet K2-18b Is Not Habitable. News outlets that said otherwise are just crying wolf—but they're not the only ones at fault. Laura Kreidberg, Scientific American. 23 September 2019.
  43. ^ Tasker, Elizabeth. "Let's Lose the Term "Habitable Zone" for Exoplanets". Scientific American Blog Network. Retrieved 2019-10-21.
  44. ^ Ruher, Hugo (2019-10-20). "Exoplanètes: faut-il en finir avec la "zone d'habitabilité"? - Sciences". Numerama (in French). Retrieved 2019-10-21.
  45. ^ 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.
  46. ^ Kasting, James F. (June 1988). "Runaway and moist greenhouse atmospheres and the evolution of Earth and Venus". Icarus. 74 (3): 472–494. Bibcode:1988Icar...74..472K. doi:10.1016/0019-1035(88)90116-9. PMID 11538226.
  47. ^ a b Zsom, Andras; Seager, Sara; De Wit, Julien (2013). "Towards the Minimum Inner Edge Distance of the Habitable Zone". The Astrophysical Journal. 778 (2): 109. arXiv:1304.3714. Bibcode:2013ApJ...778..109Z. doi:10.1088/0004-637X/778/2/109. S2CID 27805994.
  48. ^ a b c Pierrehumbert, Raymond; Gaidos, Eric (2011). "Hydrogen Greenhouse Planets Beyond the Habitable Zone". The Astrophysical Journal Letters. 734 (1): L13. arXiv:1105.0021. Bibcode:2011ApJ...734L..13P. doi:10.1088/2041-8205/734/1/L13. S2CID 7404376.
  49. ^ a b c Ramirez, Ramses; Kaltenegger, Lisa (2017). "A Volcanic Hydrogen Habitable Zone". The Astrophysical Journal Letters. 837 (1): L4. arXiv:1702.08618. Bibcode:2017ApJ...837L...4R. doi:10.3847/2041-8213/aa60c8. S2CID 119333468.
  50. ^ "Stellar habitable zone calculator". University of Washington. Retrieved 17 December 2015.
  51. ^ "Venus". Case Western Reserve University. 13 September 2006. Archived from the original on 2012-04-26. Retrieved 2011-12-21.
  52. ^ Sharp, Tim. "Atmosphere of the Moon". Space.com. TechMediaNetwork. Retrieved April 23, 2013.
  53. ^ Bolonkin, Alexander A. (2009). Artificial Environments on Mars. Berlin Heidelberg: Springer. pp. 599–625. ISBN 978-3-642-03629-3.
  54. ^ a b Haberle, Robert M.; McKay, Christopher P.; Schaeffer, James; Cabrol, Nathalie A.; Grin, Edmon A.; Zent, Aaron P.; Quinn, Richard (2001). "On the possibility of liquid water on present-day Mars". Journal of Geophysical Research. 106 (E10): 23317. Bibcode:2001JGR...10623317H. doi:10.1029/2000JE001360. ISSN 0148-0227.
  55. ^ Mann, Adam (February 18, 2014). "Strange Dark Streaks on Mars Get More and More Mysterious". Wired. Retrieved February 18, 2014.
  56. ^ "NASA Finds Possible Signs of Flowing Water on Mars". voanews.com. 3 August 2011. Archived from the original on September 17, 2011. Retrieved August 5, 2011.
  57. ^ "Is Mars Weeping Salty Tears?". news.sciencemag.org. Archived from the original on August 14, 2011. Retrieved August 5, 2011.
  58. ^ Webster, Guy; Brown, Dwayne (December 10, 2013). "NASA Mars Spacecraft Reveals a More Dynamic Red Planet". NASA. Retrieved December 10, 2013.
  59. ^ 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.
  60. ^ Salvador, A.; Massol, H.; Davaille, A.; Marcq, E.; Sarda, P.; Chassefière, E. (2017). "The relative influence of H2 O and CO2 on the primitive surface conditions and evolution of rocky planets" (PDF). Journal of Geophysical Research: Planets. 122 (7): 1458–1486. Bibcode:2017JGRE..122.1458S. doi:10.1002/2017JE005286. ISSN 2169-9097. S2CID 135136696.
  61. ^ "Flashback: Water on Mars Announced 10 Years Ago". SPACE.com. June 22, 2000. Retrieved December 19, 2010.
  62. ^ "Flashback: Water on Mars Announced 10 Years Ago". SPACE.com. June 22, 2010. Retrieved May 13, 2018.
  63. ^ "Science@NASA, The Case of the Missing Mars Water". Archived from the original on March 27, 2009. Retrieved March 7, 2009.
  64. ^ Scully, Jennifer E.C.; Russell, Christopher T.; Yin, An; Jaumann, Ralf; Carey, Elizabeth; Castillo-Rogez, Julie; McSween, Harry Y.; Raymond, Carol A.; Reddy, Vishnu; Le Corre, Lucille (2015). "Geomorphological evidence for transient water flow on Vesta". Earth and Planetary Science Letters. 411: 151–163. Bibcode:2015E&PSL.411..151S. doi:10.1016/j.epsl.2014.12.004. ISSN 0012-821X.
  65. ^ Raponi, Andrea; De Sanctis, Maria Cristina; Frigeri, Alessandro; Ammannito, Eleonora; Ciarniello, Mauro; Formisano, Michelangelo; Combe, Jean-Philippe; Magni, Gianfranco; Tosi, Federico; Carrozzo, Filippo Giacomo; Fonte, Sergio; Giardino, Marco; Joy, Steven P.; Polanskey, Carol A.; Rayman, Marc D.; Capaccioni, Fabrizio; Capria, Maria Teresa; Longobardo, Andrea; Palomba, Ernesto; Zambon, Francesca; Raymond, Carol A.; Russell, Christopher T. (2018). "Variations in the amount of water ice on Ceres' surface suggest a seasonal water cycle". Science Advances. 4 (3): eaao3757. Bibcode:2018SciA....4.3757R. doi:10.1126/sciadv.aao3757. ISSN 2375-2548. PMC 5851659. PMID 29546238.
  66. ^ NASA.gov PIA21471: Landslides on Ceres
  67. ^ Budyko, M. I. (1969). "The effect of solar radiation variations on the climate of the Earth". Tellus. 21 (5): 611–619. Bibcode:1969Tell...21..611B. CiteSeerX 10.1.1.696.824. doi:10.1111/j.2153-3490.1969.tb00466.x.
  68. ^ 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.
  69. ^ 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.
  70. ^ Rasool, I.; De Bergh, C. (13 Jun 1970). "The Runaway Greenhouse and the Accumulation of CO2 in the Venus Atmosphere" (PDF). Nature. 226 (5250): 1037–1039. Bibcode:1970Natur.226.1037R. doi:10.1038/2261037a0. ISSN 0028-0836. PMID 16057644. S2CID 4201521. Archived (PDF) from the original on 14 November 2023.
  71. ^ Hart, M. H. (1979). "Habitable zones about main sequence stars". Icarus. 37 (1): 351–357. Bibcode:1979Icar...37..351H. doi:10.1016/0019-1035(79)90141-6.
  72. ^ 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): 1308–1318. arXiv:1002.4877. Bibcode:2010ApJ...721.1308S. doi:10.1088/0004-637X/721/2/1308. S2CID 15899053.
  73. ^ 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.
  74. ^ 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. 767 (1): 65–?. arXiv:1302.4566. Bibcode:2013ApJ...767...65V. doi:10.1088/0004-637X/767/1/65. S2CID 49553651.
  75. ^ Kopparapu, Ravi Kumar; et al. (10 March 2013). "Habitable Zones Around Main-Sequence Stars: New Estimates". The Astrophysical Journal. 765 (2): 131. arXiv:1301.6674. Bibcode:2013ApJ...765..131K. doi:10.1088/0004-637X/765/2/131. S2CID 76651902.
  76. ^ Leconte, Jeremy; Forget, Francois; Charnay, Benjamin; Wordsworth, Robin; Pottier, Alizee (2013). "Increased insolation threshold for runaway greenhouse processes on Earth like planets". Nature. 504 (7479): 268–71. arXiv:1312.3337. Bibcode:2013Natur.504..268L. doi:10.1038/nature12827. PMID 24336285. S2CID 2115695.
  77. ^ Gomez-Leal, Illeana; Kaltenegger, Lisa; Lucarini, Valerio; Lunkeit, Frank (2019). "Climate sensitivity to ozone and its relevance on the habitability of Earth-like planets". Icarus. 321: 608–618. arXiv:1901.02897. Bibcode:2019Icar..321..608G. doi:10.1016/j.icarus.2018.11.019. S2CID 119209241.
  78. ^ Cuntz, Manfred (2013). "S-Type and P-Type Habitability in Stellar Binary Systems: A Comprehensive Approach. I. Method and Applications". The Astrophysical Journal. 780 (1): 14. arXiv:1303.6645. Bibcode:2014ApJ...780...14C. doi:10.1088/0004-637X/780/1/14. S2CID 118610856.
  79. ^ 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. CiteSeerX 10.1.1.41.621. doi:10.1126/science.278.5341.1273. PMID 9360920.
  80. ^ 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.
  81. ^ Vu, Linda. "Planets Prefer Safe Neighborhoods" (Press release). Spitzer.caltech.edu. NASA/Caltech. Retrieved April 22, 2013.
  82. ^ 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. CiteSeerX 10.1.1.337.8642. doi:10.1016/j.icarus.2006.03.007. S2CID 2241081.
  83. ^ 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.
  84. ^ 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. S2CID 14119086.
  85. ^ Agol, Eric (April 2011). "Transit Surveys for Earths in the Habitable Zones of White Dwarfs". The Astrophysical Journal Letters. 731 (2): L31. arXiv:1103.2791. Bibcode:2011ApJ...731L..31A. doi:10.1088/2041-8205/731/2/L31. S2CID 118739494.
  86. ^ Ramirez, Ramses; Kaltenegger, Lisa (2014). "Habitable Zones of Pre-Main-Sequence Stars". The Astrophysical Journal Letters. 797 (2): L25. arXiv:1412.1764. Bibcode:2014ApJ...797L..25R. doi:10.1088/2041-8205/797/2/L25. S2CID 119276912.
  87. ^ Carroll, Bradley W.; Ostlie, Dale A. (2007). An Introduction to Modern Astrophysics (2nd ed.).
  88. ^ Richmond, Michael (November 10, 2004). "Late stages of evolution for low-mass stars". Rochester Institute of Technology. Retrieved 2007-09-19.
  89. ^ 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): 367–373. arXiv:1003.1368. Bibcode:2009Ap&SS.323..367G. doi:10.1007/s10509-009-0081-z. S2CID 118500534.
  90. ^ 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. Bibcode:1986Sci...234.1383K. doi:10.1126/science.11539665. PMID 11539665.
  91. ^ 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" (PDF). In Montesinos, Benjamin; Giménez, Alvaro; Guinan, Edward F. (eds.). 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.
  92. ^ Croswell, Ken (January 27, 2001). "Red, willing and able". New Scientist. Retrieved August 5, 2007. Full reprint
  93. ^ Alekseev, I. Y.; Kozlova, O. V. (2002). "Starspots and active regions on the emission red dwarf star LQ Hydrae". Astronomy and Astrophysics. 396: 203–211. Bibcode:2002A&A...396..203A. doi:10.1051/0004-6361:20021424.
  94. ^ a b Alpert, Mark (November 7, 2005). "Red Star Rising". Scientific American. 293 (5): 28. Bibcode:2005SciAm.293e..28A. doi:10.1038/scientificamerican1105-28. PMID 16318021.
  95. ^ "Andrew West: 'Fewer flares, starspots for older dwarf stars'". EarthSky. December 19, 2006. Retrieved April 27, 2013.
  96. ^ Cain, Fraser; Gay, Pamela (2007). "AstronomyCast episode 40: American Astronomical Society Meeting, May 2007". Universe Today. Archived from the original on 2007-09-26. Retrieved 2007-06-17.
  97. ^ Ray Villard (27 July 2009). "Living in a Dying Solar System, Part 1". Astrobiology. Archived from the original on 24 April 2016. Retrieved 8 April 2016.
  98. ^ Christensen, Bill (April 1, 2005). "Red Giants and Planets to Live On". Space.com. TechMediaNetwork. Retrieved April 27, 2013.
  99. ^ a b c d Ramirez, Ramses; Kaltenegger, Lisa (2016). "Habitable Zones of Post-Main Sequence Stars". The Astrophysical Journal. 823 (1): 6. arXiv:1605.04924. Bibcode:2016ApJ...823....6R. doi:10.3847/0004-637X/823/1/6. S2CID 119225201.
  100. ^ 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): 974–985. arXiv:astro-ph/0503520. Bibcode:2005ApJ...627..974L. doi:10.1086/430416. S2CID 17075384.
  101. ^ 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. CiteSeerX 10.1.1.683.8827. doi:10.1029/97GL52843. ISSN 0094-8276. PMID 11542268. S2CID 14172341.
  102. ^ Voisey, Jon (February 23, 2011). "Plausibility Check – Habitable Planets around Red Giants". Universe Today. Retrieved April 27, 2013.
  103. ^ Alien Life More Likely on 'Dune' Planets Archived December 2, 2013, at the Wayback Machine, 09/01/11, Charles Q. Choi, Astrobiology Magazine
  104. ^ Abe, Y; Abe-Ouchi, A; Sleep, NH; Zahnle, KJ (2011). "Habitable zone limits for dry planets". Astrobiology. 11 (5): 443–60. Bibcode:2011AsBio..11..443A. doi:10.1089/ast.2010.0545. PMID 21707386.
  105. ^ Drake, Michael J. (April 2005). "Origin of water in the terrestrial planets". Meteoritics & Planetary Science. 40 (4): 519–527. Bibcode:2005M&PS...40..519D. doi:10.1111/j.1945-5100.2005.tb00960.x. S2CID 12808812.
  106. ^ 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. Vol. 1. 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.
  107. ^ Kuchner, Marc (2003). "Volatile-rich Earth-Mass Planets in the Habitable Zone". Astrophysical Journal. 596 (1): L105–L108. arXiv:astro-ph/0303186. Bibcode:2003ApJ...596L.105K. doi:10.1086/378397. S2CID 15999168.
  108. ^ Charbonneau, David; Zachory K. Berta; Jonathan Irwin; Christopher J. Burke; Philip Nutzman; Lars A. Buchhave; Christophe Lovis; Xavier Bonfils; et al. (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. S2CID 4360404.
  109. ^ Kuchner, Seager; Hier-Majumder, M.; Militzer, C. A. (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. S2CID 8369390.
  110. ^ Vastag, Brian (December 5, 2011). "Newest alien planet is just the right temperature for life". The Washington Post. Retrieved April 27, 2013.
  111. ^ 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. S2CID 54997095.
  112. ^ 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. S2CID 7852371.
  113. ^ Chaplin, Martin (April 8, 2013). "Water Phase Diagram". Ices. London South Bank University. Retrieved April 27, 2013.
  114. ^ D.P. Hamilton; J.A. Burns (1992). "Orbital stability zones about asteroids. II – The destabilizing effects of eccentric orbits and solar radiation" (PDF). Icarus. 96 (1): 43–64. Bibcode:1992Icar...96...43H. CiteSeerX 10.1.1.488.4329. doi:10.1016/0019-1035(92)90005-R.
  115. ^ 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. Acad. Sci. Paris (in French). 231: 261–263.
  116. ^ Horikawa, Daiki D. (2012). "Survival of Tardigrades in Extreme Environments: A Model Animal for Astrobiology". In Alexander V. Altenbach, Joan M. Bernhard & Joseph Seckbach (ed.). Anoxia Evidence for Eukaryote Survival and Paleontological Strategies. Cellular Origin, Life in Extreme Habitats and Astrobiology. Vol. 21 (21 ed.). Springer Netherlands. pp. 205–217. doi:10.1007/978-94-007-1896-8_12. ISBN 978-94-007-1895-1.
  117. ^ 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. S2CID 10551100.
  118. ^ Paul Gilster; Andrew LePage (2015-01-30). "A Review of the Best Habitable Planet Candidates". Centauri Dreams, Tau Zero Foundation. Retrieved 2015-07-24.
  119. ^ Giovanni F. Bignami (2015). The Mystery of the Seven Spheres: How Homo sapiens will Conquer Space. Springer. p. 110. ISBN 978-3-319-17004-6.
  120. ^ Wethington, Nicholos (September 16, 2008). "How Many Stars are in the Milky Way?". Universe Today. Retrieved April 21, 2013.
  121. ^ a b Torres, Abel Mendez (April 26, 2013). "Ten potentially habitable exoplanets now". Habitable Exoplanets Catalog. University of Puerto Rico. Archived from the original on October 21, 2019. Retrieved April 29, 2013.
  122. ^ Borenstein, Seth (19 February 2011). "Cosmic census finds crowd of planets in our galaxy". Associated Press. Archived from the original on 27 September 2011. Retrieved 24 April 2011.
  123. ^ Choi, Charles Q. (21 March 2011). "New Estimate for Alien Earths: 2 Billion in Our Galaxy Alone". Space.com. Retrieved 2011-04-24.
  124. ^ 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. S2CID 119290692.
  125. ^ 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. S2CID 37593615.
  126. ^ "70 Virginis b". Extrasolar Planet Guide. Extrasolar.net. Archived from the original on 2012-06-19. Retrieved 2009-04-02.
  127. ^ 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. S2CID 37593615.
  128. ^ 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. S2CID 16004653.
  129. ^ 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): 1010–1019. arXiv:astro-ph/0603200. Bibcode:2006ApJ...649.1010J. doi:10.1086/506557. S2CID 119078585.
  130. ^ 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 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701. S2CID 119067572.
  131. ^ Barnes, J. W.; O'Brien, D. P. (2002). "Stability of Satellites around Close-in Extrasolar Giant Planets". The Astrophysical Journal. 575 (2): 1087–1093. arXiv:astro-ph/0205035. Bibcode:2002ApJ...575.1087B. doi:10.1086/341477. S2CID 14508244.
  132. ^ 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. S2CID 4327454.
  133. ^ 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. S2CID 4343578.
  134. ^ 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.
  135. ^ 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. S2CID 55779685.
  136. ^ Ian Sample (7 November 2007). "Could this be Earth's near twin? Introducing planet 55 Cancri f". The Guardian. London. Archived from the original on 2 October 2008. Retrieved 17 October 2008.
  137. ^ Than, Ker (2007-02-24). "Planet Hunters Edge Closer to Their Holy Grail". space.com. Retrieved 2007-04-29.
  138. ^ 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. 345 (6195): 440–444. arXiv:1407.1049. Bibcode:2014Sci...345..440R. CiteSeerX 10.1.1.767.2071. doi:10.1126/science.1253253. PMID 24993348. S2CID 206556796.
  139. ^ "Researchers find potentially habitable planet" (in French). maxisciences.com. 2011-08-30. Archived from the original on 2019-04-13. Retrieved 2011-08-31.
  140. ^ "Kepler 22-b: Earth-like planet confirmed". BBC. December 5, 2011. Retrieved May 2, 2013.
  141. ^ 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".
  142. ^ Anglada-Escude, Guillem; Arriagada, Pamela; Vogt, Steven; Rivera, Eugenio J.; Butler, R. Paul; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B.; Minniti, Dante (2012). "A planetary system around the nearby M dwarf GJ 667C with at least one super-Earth in its habitable zone". The Astrophysical Journal. 751 (1): L16. arXiv:1202.0446. Bibcode:2012ApJ...751L..16A. doi:10.1088/2041-8205/751/1/L16. S2CID 16531923.
  143. ^ "LHS 188 – High proper-motion Star". Centre de données astronomiques de Strasbourg (Strasbourg astronomical Data Center). September 20, 2012. Retrieved September 20, 2012.
  144. ^ Méndez, Abel (August 29, 2012). "A Hot Potential Habitable Exoplanet around Gliese 163". University of Puerto Rico at Arecibo (Planetary Habitability Laboratory). Archived from the original on October 21, 2019. Retrieved September 20, 2012.
  145. ^ Redd (September 20, 2012). "Newfound Alien Planet a Top Contender to Host Life". Space.com. Retrieved September 20, 2012.
  146. ^ "A Hot Potential Habitable Exoplanet around Gliese 163". Spacedaily.com. Retrieved 2013-02-10.
  147. ^ Tuomi, Mikko; Anglada-Escudé, Guillem; Gerlach, Enrico; Jones, Hugh R. A.; Reiners, Ansgar; Rivera, Eugenio J.; Vogt, Steven S.; Butler, R. Paul (17 December 2012). "Habitable-zone super-Earth candidate in a six-planet system around the K2.5V star HD 40307". Astronomy & Astrophysics. 549: A48. arXiv:1211.1617. Bibcode:2013A&A...549A..48T. doi:10.1051/0004-6361/201220268. S2CID 7424216.
  148. ^ Aron, Jacob (December 19, 2012). "Nearby Tau Ceti may host two planets suited to life". New Scientist. Reed Business Information. Retrieved April 1, 2013.
  149. ^ 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. S2CID 2390534.
  150. ^ Torres, Abel Mendez (May 1, 2013). "The Habitable Exoplanets Catalog". University of Puerto Rico. Retrieved May 1, 2013.
  151. ^ Lauren M. Weiss, and Geoffrey W. Marcy. "The mass-radius relation for 65 exoplanets smaller than 4 Earth radii"
  152. ^ "Solar Variability and Terrestrial Climate". NASA Science. 2013-01-08.
  153. ^ "Stellar Luminosity Calculator". University of Nebraska-Lincoln astronomy education group.
  154. ^ Council, National Research (18 September 2012). The Effects of Solar Variability on Earth's Climate: A Workshop Report. doi:10.17226/13519. ISBN 978-0-309-26564-5.
  155. ^ Ethan (June 5, 2013). "Most of Earth's twins aren't identical, or even close!". ScienceBlogs.com.
  156. ^ "Are there oceans on other planets?". National Oceanic and Atmospheric Administration. 6 July 2017. Retrieved 2017-10-03.
  157. ^ Moskowitz, Clara (January 9, 2013). "Most Earth-Like Alien Planet Possibly Found". Space.com. Retrieved January 9, 2013.
  158. ^ 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. S2CID 51490784.
  159. ^ a b Johnson, Michele; Harrington, J.D. (18 April 2013). "NASA's Kepler Discovers Its Smallest 'Habitable Zone' Planets to Date". NASA. Archived from the original on 8 May 2020. Retrieved 18 April 2013.
  160. ^ a b Overbye, Dennis (18 April 2013). "Two Promising Places to Live, 1,200 Light-Years from Earth". The New York Times. Retrieved 18 April 2013.
  161. ^ 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): 587–90. arXiv:1304.7387. Bibcode:2013Sci...340..587B. doi:10.1126/science.1234702. hdl:1721.1/89668. PMID 23599262. S2CID 21029755.
  162. ^ Chang, Kenneth (17 April 2014). "Scientists Find an 'Earth Twin,' or Maybe a Cousin". The New York Times. Retrieved 17 April 2014.
  163. ^ Chang, Alicia (17 April 2014). "Astronomers spot most Earth-like planet yet". AP News. Retrieved 17 April 2014.
  164. ^ Morelle, Rebecca (17 April 2014). "'Most Earth-like planet yet' spotted by Kepler". BBC News. Retrieved 17 April 2014.
  165. ^ Wall, Mike (3 June 2014). "Found! Oldest Known Alien Planet That Might Support Life". Space.com. Retrieved 10 January 2015.
  166. ^ a b Clavin, Whitney; Chou, Felicia; Johnson, Michele (6 January 2015). "NASA's Kepler Marks 1,000th Exoplanet Discovery, Uncovers More Small Worlds in Habitable Zones". NASA. Retrieved 6 January 2015.
  167. ^ Jensen, Mari N. (16 January 2015). "Three nearly Earth-size planets found orbiting nearby star: One in 'Goldilocks' zone". Science Daily. Retrieved 25 July 2015.
  168. ^ Jenkins, Jon M.; Twicken, Joseph D.; Batalha, Natalie M.; Caldwell, Douglas A.; Cochran, William D.; Endl, Michael; Latham, David W.; Esquerdo, Gilbert A.; Seader, Shawn; Bieryla, Allyson; Petigura, Erik; Ciardi, David R.; Marcy, Geoffrey W.; Isaacson, Howard; Huber, Daniel; Rowe, Jason F.; Torres, Guillermo; Bryson, Stephen T.; Buchhave, Lars; Ramirez, Ivan; Wolfgang, Angie; Li, Jie; Campbell, Jennifer R.; Tenenbaum, Peter; Sanderfer, Dwight; Henze, Christopher E.; Catanzarite, Joseph H.; Gilliland, Ronald L.; Borucki, William J. (23 July 2015). "Discovery and Validation of Kepler-452b: A 1.6 R🜨 Super Earth Exoplanet in the Habitable Zone of a G2 Star". The Astronomical Journal. 150 (2): 56. arXiv:1507.06723. Bibcode:2015AJ....150...56J. doi:10.1088/0004-6256/150/2/56. ISSN 1538-3881. S2CID 26447864.
  169. ^ "NASA telescope discovers Earth-like planet in star's habitable zone". BNO News. 23 July 2015. Retrieved 23 July 2015.
  170. ^ "Three Potentially Habitable Worlds Found Around Nearby Ultracool Dwarf Star". European Southern Observatory. 2 May 2016.
  171. ^ Dressing, Courtney D.; Vanderburg, Andrew; Schlieder, Joshua E.; Crossfield, Ian J. M.; Knutson, Heather A.; Newton, Elisabeth R.; Ciardi, David R.; Fulton, Benjamin J.; Gonzales, Erica J.; Howard, Andrew W.; Isaacson, Howard; Livingston, John; Petigura, Erik A.; Sinukoff, Evan; Everett, Mark; Horch, Elliott; Howell, Steve B. (2017). "Characterizing K2 Candidate Planetary Systems Orbiting Low-mass Stars. II. Planetary Systems Observed During Campaigns 1–7" (PDF). The Astronomical Journal. 154 (5): 207. arXiv:1703.07416. Bibcode:2017AJ....154..207D. doi:10.3847/1538-3881/aa89f2. ISSN 1538-3881. S2CID 13419148.
  172. ^ Dittmann, Jason A.; Irwin, Jonathan M.; Charbonneau, David; Bonfils, Xavier; Astudillo-Defru, Nicola; Haywood, Raphaëlle D.; Berta-Thompson, Zachory K.; Newton, Elisabeth R.; Rodriguez, Joseph E.; Winters, Jennifer G.; Tan, Thiam-Guan; Almenara, Jose-Manuel; Bouchy, François; Delfosse, Xavier; Forveille, Thierry; Lovis, Christophe; Murgas, Felipe; Pepe, Francesco; Santos, Nuno C.; Udry, Stephane; Wünsche, Anaël; Esquerdo, Gilbert A.; Latham, David W.; Dressing, Courtney D. (2017). "A temperate rocky super-Earth transiting a nearby cool star". Nature. 544 (7650): 333–336. arXiv:1704.05556. Bibcode:2017Natur.544..333D. doi:10.1038/nature22055. PMID 28426003. S2CID 2718408.
  173. ^ Bradley, Sian (2017-11-16). "Astronomers are beaming techno into space for aliens to decode". Wired UK.
  174. ^ "In Earth's Backyard: Newfound Alien Planet May be Good Bet for Life". Space.com. 15 November 2017.
  175. ^ "K2-155 d". Exoplanet Exploration. 2018.
  176. ^ Mack, Eric (March 13, 2018). "A super-Earth around a red star could be wet and wild". CNET.
  177. ^ Whitwam, Ryan (March 14, 2018). "Kepler Spots Potentially Habitable Super-Earth Orbiting Nearby Star". ExtremeTech.
  178. ^ Luque, R.; Pallé, E.; Kossakowski, D.; Dreizler, S.; Kemmer, J.; Espinoza, N. (2019). "Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization". Astronomy & Astrophysics. 628: A39. arXiv:1904.12818. Bibcode:2019A&A...628A..39L. doi:10.1051/0004-6361/201935801. ISSN 0004-6361.
  179. ^ Schulze-Makuch, Dirk; Heller, Rene; Guinan, Edward (18 September 2020). "In Search for a Planet Better than Earth: Top Contenders for a Superhabitable World". Astrobiology. 20 (12): 1394–1404. Bibcode:2020AsBio..20.1394S. doi:10.1089/ast.2019.2161. PMC 7757576. PMID 32955925.
  180. ^ Torres, Abel (2012-06-12). "Liquid Water in the Solar System". Archived from the original on 2013-11-18. Retrieved 2013-12-15.
  181. ^ Munro, Margaret (2013), "Miners deep underground in northern Ontario find the oldest water ever known", National Post, retrieved 2013-10-06
  182. ^ Davies, Paul (February 2001). "The Origin of Life II: How did it begin?". Science Progress. 84 (1): 17–29. doi:10.3184/003685001783239096. ISSN 2047-7163. PMC 10367499. PMID 11382135.
  183. ^ Taylor, Geoffrey (1996), "Life Underground" (PDF), Planetary Science Research Discoveries, retrieved 2013-10-06
  184. ^ Doyle, Alister (4 March 2013), "Deep underground, worms and "zombie microbes" rule", Reuters, retrieved 2013-10-06
  185. ^ Nicholson, W. L.; Moeller, R.; Horneck, G. (2012). "Transcriptomic Responses of Germinating Bacillus subtilis Spores 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.
  186. ^ 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.
  187. ^ a b Stewart, Ian; Cohen, Jack (2002). Evolving the Alien. Ebury Press. ISBN 978-0-09-187927-3.
  188. ^ Goldsmith, Donald; Owen, Tobias (1992). The Search for Life in the Universe (2 ed.). Addison-Wesley. p. 247. ISBN 978-0-201-56949-0.
  189. ^ Vaclav Smil (2003). The Earth's Biosphere: Evolution, Dynamics, and Change. MIT Press. p. 166. ISBN 978-0-262-69298-4.
  190. ^ Reynolds, R.T.; McKay, C.P.; Kasting, J.F. (1987). "Europa, Tidally Heated Oceans, and Habitable Zones Around Giant Planets". Advances in Space Research. 7 (5): 125–132. Bibcode:1987AdSpR...7e.125R. doi:10.1016/0273-1177(87)90364-4. PMID 11538217.
  191. ^ Guidetti, R.; Jönsson, K.I. (2002). "Long-term anhydrobiotic survival in semi-terrestrial micrometazoans". Journal of Zoology. 257 (2): 181–187. CiteSeerX 10.1.1.630.9839. doi:10.1017/S095283690200078X.
  192. ^ Baldwin, Emily (26 April 2012). "Lichen survives harsh Mars environment". Skymania News. Archived from the original on 28 May 2012. Retrieved 27 April 2012.
  193. ^ 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" (PDF). European Geosciences Union. Archived from the original (PDF) on 4 May 2012. Retrieved 27 April 2012.
  194. ^ a b Onofri, Silvano; de Vera, Jean-Pierre; Zucconi, Laura; Selbmann, Laura; Scalzi, Giuliano; Venkateswaran, Kasthuri J.; Rabbow, Elke; de la Torre, Rosa; Horneck, Gerda (2015). "Survival of Antarctic Cryptoendolithic Fungi in Simulated Martian Conditions On Board the International Space Station". Astrobiology. 15 (12): 1052–1059. Bibcode:2015AsBio..15.1052O. doi:10.1089/ast.2015.1324. ISSN 1531-1074. PMID 26684504.
  195. ^ Isler, K.; van Schaik, C. P (2006). "Metabolic costs of brain size evolution". Biology Letters. 2 (4): 557–560. doi:10.1098/rsbl.2006.0538. ISSN 1744-9561. PMC 1834002. PMID 17148287.
  196. ^ Palca, Joe (September 29, 2010). "'Goldilocks' Planet's Temperature Just Right For Life". NPR. NPR. Retrieved April 5, 2011.
  197. ^ "Project Cyclops: A design study of a system for detecting extraterrestrial intelligent life" (PDF). NASA. 1971. Retrieved June 28, 2009.
  198. ^ Joseph A. Angelo (2007). Life in the Universe. Infobase Publishing. p. 163. ISBN 978-1-4381-0892-6. Retrieved 26 June 2013.
  199. ^ 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. S2CID 14734094.
  200. ^ 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. S2CID 119302350.
  201. ^ Wall, Mike (2011). "HabStars: Speeding Up In the Zone". Space.com. Retrieved 2013-06-26.
  202. ^ Zaitsev, A. L. (June 2004). "Transmission and reasonable signal searches in the Universe" (PDF). Horizons of the Universe Передача и поиски разумных сигналов во Вселенной. Plenary presentation at the National Astronomical Conference WAC-2004 "Horizons of the Universe", Moscow, Moscow State University, June 7, 2004 (in Russian). Moscow. Archived from the original on 2019-05-30. Retrieved 2013-06-30.
  203. ^ David Grinspoon (July 13, 2012) [December 12, 2007]. "Who Speaks for Earth?". Seed. Archived from the original on 2012-07-13. Retrieved 2021-06-24.
  204. ^ 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. S2CID 16722873.
  205. ^ 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. S2CID 119089227.
  206. ^ 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.
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