Kepler-186f

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Kepler-186f
Kepler186f-ArtistConcept-20140417.jpg
Artist’s depiction of Kepler-186f (foreground) as a rocky Earth-like planet in the habitable zone, with the Kepler-186 system visible in the background (bottom left). The actual appearance and composition of the exoplanet is not currently known.
Discovery
Discovered by Elisa Quintana
Discovery site Kepler Space Observatory
Discovery date17 April 2014
Transit
Orbital characteristics
0.432 ± 0.01 AU [1]
Eccentricity 0.04 [1]
129.9444 ± 0.0012 d [1]
0.355772 y
Inclination 89.9 [1]
Star Kepler-186
Physical characteristics
Mean radius
1.17 ± 0.08 [1] R🜨
Mass 1.44+2.33
−1.12 [2] ME
1.17 (est.) g
Temperature Teq: 188 K (−85 °C; −121 °F)

    Kepler-186f [2] [3] (also known by its Kepler object of interest designation KOI-571.05) is an Earth-sized exoplanet orbiting within the habitable zone of the red dwarf star Kepler-186, [4] [5] [6] the outermost of five such planets discovered around the star by NASA's Kepler spacecraft. It is located about 580 light-years (180 parsecs ) from Earth in the constellation of Cygnus. [7]

    Contents

    Kepler-186f orbits its star at a distance of about 0.43 AU (64,000,000 km; 40,000,000 mi) from its host star with an orbital period of roughly 130 days, and a mass and radius around 1.44 and 1.17 times that of Earth, respectively. As one of the more promising candidates for habitability, it was the first planet with a radius similar to Earth's to be discovered in the habitable zone of another star. However, key components still need to be found to determine its habitability for life, including an atmosphere and its composition and if liquid water can exist on its surface.

    Analysis of three years of data was required to find its signal. [8] NASA’s Kepler telescope detected it using the transit method (in which the dimming effect that a planet causes as it crosses in front of its star is measured), along with four additional planets orbiting much closer to the star (all modestly larger than Earth). [5] The results were presented initially at a conference on 19 March 2014 [9] and some details were reported in the media at the time. [10] The public announcement was on 17 April 2014, [3] followed by publication in Science . [2]

    Physical characteristics

    Mass, radius and temperature

    The only physical property directly derivable from the observations (besides the orbit) is the size of the planet relative to the central star, which follows from the amount of occultation of stellar light during a transit. This ratio was measured to be 0.021, [2] giving a planetary radius of 1.17 ± 0.08 times that of Earth. [3] [5] The planet is about 11% larger in radius than Earth (between 4.5% smaller and 26.5% larger), giving a volume about 1.37 times that of Earth (between 0.87 and 2.03 times as large).

    A very wide range of possible masses can be calculated by combining the radius with densities derived from the possible types of matter from which planets can be made. For example, it could be a rocky terrestrial planet or a lower density ocean planet with a thick atmosphere. A massive hydrogen/helium (H/He) atmosphere is thought to be unlikely in a planet with a radius below 1.5 R🜨. Planets with a radius of more than 1.5 times that of Earth tend to accumulate the thick atmospheres which make them less likely to be habitable. [11] Red dwarfs emit a much stronger extreme ultraviolet (XUV) flux when young than later in life. The planet's primordial atmosphere would have been subjected to elevated photoevaporation during that period, which would probably have largely removed any H/He-rich envelope through hydrodynamic mass loss. [2]

    Mass estimates range from 0.32 ME for a pure water/ice composition to 3.77 ME if made up entirely of iron (both implausible extremes). For a body with radius 1.11 R🜨, a composition similar to that of Earth (i.e., 1/3 iron, 2/3 silicate rock) yields a mass of 1.44 ME, [2] taking into account the higher density due to the higher average pressure compared to Earth.[ citation needed ] That would make the force of gravity on the surface 17% higher than on Earth.

    The estimated equilibrium temperature for Kepler-186f, which is the surface temperature without an atmosphere, is said to be around 188 K (−85 °C; −121 °F), somewhat colder than the equilibrium temperature of Mars. [12]

    Host star

    The planet orbits Kepler-186, an M-type red dwarf star which has a total of five known planets. The star has a mass of 0.54 M☉ and a radius of 0.52 R☉. It has a temperature of 3755 K and is about 4 billion years old, [1] about 600 million years younger than the Sun, which is 4.6 billion years old [13] and has a temperature of 5,778 K (5,505 °C; 9,941 °F). [14]

    The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.62. This is too dim to be seen with the naked eye, which can only see objects with a magnitude up to at least 6.5 – 7 or lower. [15]

    Orbit

    Kepler-186f orbits its star with about 5% of the Sun's luminosity with an orbital period of 129.9 days and an orbital radius of about 0.40 [1] times that of Earth's (compared to 0.39  AU (58 million  km ; 36 million  mi ) for Mercury). The habitable zone for this system is estimated conservatively to extend over distances receiving from 88% to 25% of Earth's illumination (from 0.23 to 0.46 AU (34 to 69 million km; 21 to 43 million mi)). [16] Kepler-186f receives about 32%, placing it within the conservative zone but near the outer edge, similar to the position of Mars in our planetary system. [2]

    Habitability

    Size comparison of Kepler-186f (artist's impression) with Earth along with their projected habitable zones. Kepler186f-ComparisonGraphic-20140417.jpg
    Size comparison of Kepler-186f (artist's impression) with Earth along with their projected habitable zones.

    Kepler-186f's location within the habitable zone does not necessarily mean it is habitable; this is also dependent on its atmospheric characteristics, which are unknown. [17] However, Kepler-186f is too distant for its atmosphere to be analyzed by existing telescopes (e.g., NESSI) or next-generation instruments such as the James Webb Space Telescope. [5] [18] A simple climate model – in which the planet's inventory of volatiles is restricted to nitrogen, carbon dioxide and water, and clouds are not accounted for – suggests that the planet's surface temperature would be above 273 K (0 °C; 32 °F) if at least 0.5 to 5 bars of CO2 is present in its atmosphere, for assumed N2 partial pressures ranging from 10 bar to zero, respectively. [19]

    The star hosts four other planets discovered so far, although Kepler-186 b, c, d, and e (in order of increasing orbital radius), being too close to their star, are considered too hot to have liquid water. The four innermost planets are probably tidally locked, but Kepler-186f is in a higher orbit, where the star's tidal effects are much weaker, so the time could have been insufficient for its spin to slow down significantly. Because of the very slow evolution of red dwarfs, the age of the Kepler-186 system was poorly constrained, although it is likely to be greater than a few billion years. [19] Recent results have placed the age at around 4 billion years. [1] The chance that it is tidally locked is approximately 50%. [20] Since it is closer to its star than Earth is to the Sun, it will probably rotate much more slowly than Earth; its day could be weeks or months long (see Tidal effects on rotation rate, axial tilt and orbit). [21]

    Kepler-186f's axial tilt (obliquity) is likely very small, in which case it would not have tilt-induced seasons like Earth's. Its orbit is probably close to circular, [21] so it will also lack eccentricity-induced seasonal changes like those of Mars. However, the axial tilt could be larger (about 23 degrees) if another undetected non-transiting planet orbits between it and Kepler-186e; planetary formation simulations have shown that the presence of at least one additional planet in this region is likely. If such a planet exists, it cannot be much more massive than Earth as it would then cause orbital instabilities. [19]

    One review essay in 2015 concluded that Kepler-186f, along with the exoplanets Kepler-442b and Kepler-62f, were likely the best candidates for being potentially habitable planets. [22]

    In June 2018, studies suggest that Kepler-186f may have seasons and a climate similar to those on Earth. [23] [24]

    Follow-up studies

    NASA Exoplanet Exploration Program "travel poster" for Kepler-186f Kepler-186f 39x27 CMYK-1.jpg
    NASA Exoplanet Exploration Program "travel poster" for Kepler-186f

    Target of SETI investigation

    As part of the SETI Institute's search for extraterrestrial intelligence, the Allen Telescope Array had listened for radio emissions from the Kepler-186 system for about a month as of 17 April 2014. No signals attributable to extraterrestrial technology were found in that interval; however, to be detectable, such transmissions, if radiated in all directions equally and thus not preferentially towards the Earth, would need to be at least 10 times as strong as those from Arecibo Observatory. [8] Another search, undertaken at the crowdsourcing project SETI-Live, reports inconclusive but optimistic-looking signs in the radio noise from the Allen Array observations. [25] The more well known SETI @ Home search does not cover any object in the Kepler field of view. [26] Another follow-up survey using the Green Bank Telescope has not reviewed Kepler 186f. [27] Given the interstellar distance of 490 light-years (151 pc), the signals would have left the planet many years ago.

    Future technology and observations

    At approximately 580 light-years (180 pc) distant, Kepler-186f is too far and its star too faint for current telescopes or the next generation of planned telescopes to determine its mass or whether it has an atmosphere. However, the discovery of Kepler-186f demonstrates conclusively that there are other Earth-sized planets in habitable zones. The Kepler spacecraft focused on a single small region of the sky but next-generation planet-hunting space telescopes, such as TESS and CHEOPS, will examine nearby stars throughout the sky. Nearby stars with planets can then be studied by the James Webb Space Telescope and future large ground-based telescopes to analyze atmospheres, determine masses and infer compositions. [21] Additionally the Square Kilometer Array would significantly improve radio observations over the Arecibo Observatory and Green Bank Telescope. [27]

    Previous names

    As the Kepler telescope observational campaign proceeded, an initially identified system was entered in the Kepler Input Catalog (KIC), and then progressed as a candidate host of planets to a Kepler Object of Interest (KOI). Thus, Kepler-186 started as KIC 8120608 and then was identified as KOI-571. [28] Kepler-186f was mentioned when known as KOI-571-05 or KOI-571.05 or using similar nomenclatures in 2013 in various discussions and publications before its full confirmation. [29]

    Comparison

    The nearest-to-Earth-size planet in a habitable zone previously known was Kepler-62f with 1.4 Earth radii. Kepler-186f orbits an M-dwarf star, while Kepler-62f orbits a K-type star. A study of atmospheric evolution in Earth-size planets in habitable zones of G-Stars (a class containing the Sun, but not Kepler-186) suggested that 0.8–1.15 R🜨 is the size range for planets small enough to lose their initial accreted hydrogen envelope but large enough to retain an outgassed secondary atmosphere such as Earth's. [30]

    Notable Exoplanets – Kepler Space Telescope
    KeplerExoplanets-NearEarthSize-HabitableZone-20150106.png
    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; 6 January 2015). [31]

    See also

    Related Research Articles

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    <span class="mw-page-title-main">Super-Earth</span> Planet with a mass between Earth and Uranus

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    <span class="mw-page-title-main">Discoveries of exoplanets</span> Detecting planets located outside the Solar System

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    <span class="mw-page-title-main">Kepler-22b</span> Super-Earth exoplanet orbiting Kepler-22

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    <span class="mw-page-title-main">Kepler-69c</span> Super-Earth orbiting Kepler-69

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    <span class="mw-page-title-main">Kepler-62</span> K-type star in the constellation Lyra

    Kepler-62 is a K-type main sequence star cooler and smaller than the Sun, located roughly 980 light-years from Earth in the constellation Lyra. It resides within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets that may be transiting their stars. On April 18, 2013, it was announced that the star has five planets, two of which, Kepler-62e and Kepler-62f are within the star's habitable zone. The outermost, Kepler-62f, is likely a rocky planet.

    <span class="mw-page-title-main">Kepler-62e</span> Habitable-zone super-Earth planet orbiting Kepler-62

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    <span class="mw-page-title-main">Kepler-62f</span> Super-Earth orbiting Kepler-62

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    <span class="mw-page-title-main">Kepler-186</span> Star in the constellation Cygnus

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    <span class="mw-page-title-main">Kepler-438b</span> Super-Earth orbiting Kepler-438

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    <span class="mw-page-title-main">Kepler-442b</span> Super-Earth orbiting Kepler-442

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    <span class="mw-page-title-main">Kepler-452b</span> Super-Earth exoplanet orbiting Kepler-452

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    Kepler-186e is a confirmed exoplanet orbiting the red dwarf star Kepler-186, approximately 582 light years away from Earth in the constellation of Cygnus. It is near the optimistic habitable zone but probably not in it, possibly making it have a runaway greenhouse effect, like Venus. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. Four additional planets orbiting the star were also discovered.

    <span class="mw-page-title-main">Kepler-1229b</span> Super-Earth orbiting Kepler-1229

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    <span class="mw-page-title-main">Kepler-1649c</span> Earth-size exoplanet orbiting Kepler-1649

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      ^Bovaird, Timothy; Lineweaver, Charles H. (1 August 2013). "Exoplanet Predictions Based on the Generalised Titius-Bode Relation". Monthly Notices of the Royal Astronomical Society. 435 (2): 14–15. arXiv: 1304.3341 . Bibcode:2013MNRAS.435.1126B. doi:10.1093/mnras/stt1357. S2CID   15620163.
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