Kepler-20f
{{Short description|Terrestrial planet orbiting Kepler-20}}
{{Infobox planet
| name = Kepler-20f
| image = Kepler-20f_Planet.jpg
| caption = An artist's depiction of Kepler-20f.
| discoverer = Kepler team
| discovered = 20 December 2011
| discovery_method = Transit (Kepler Mission)
| apsis = astron
| semimajor = {{convert|0.1387|±|0.0027|AU|km|abbr=on}}
| eccentricity = <0.094
| period = {{val|19.578328|(48)}} d
| inclination = {{val|88.788|0.430|0.072}}
| star = Kepler-20 (KOI-70)
| mean_radius = {{val|0.952|0.047|0.087|ul=Earth radius}}
| mass = {{val|p=<|1.4|ul=Earth mass}}
| single_temperature = {{val|681|9|ul=K}} ({{val|{{convert|681|K|C|disp=number}}|u=°C}}, {{val|{{convert|681|K|F|disp=number}}|u=°F}})
}}
Kepler-20f (also known by its Kepler Object of Interest designation KOI-070.05) is an exoplanet orbiting the Sun-like star Kepler-20, the second outermost of five such planets discovered by NASA's Kepler spacecraft. It is located approximately 929 light-years (285 parsecs, or about {{val|8.988|e=15}} km) from Earth in the constellation Lyra. 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. The planet is notable as it has the closest radius to Earth known so far.
Characteristics
File:Kepler 20 - planet lineup.jpg and Kepler-20f compared to Venus and Earth]]
=Mass, radius and temperature =
Kepler-20f is very likely (>95% chance) a rocky planet because of its radius, which is notable as being the closest to Earth yet: {{earth radius|1.004}}, though a newer estimate suggest a value of {{val|0.952|0.047|0.087|ul=Earth radius}}. However, although its radius is almost the same as Earth's, its surface conditions are not Earth-like in any way. The equilibrium temperature of Kepler-20f is approximately {{convert|705|K|C F}}, too hot to support liquid water on its surface and hot enough to melt some types of metal.{{cite web|url=http://www.nasa.gov/mission_pages/kepler/news/kepler-20-system.html#.V2cfuGM_VuU|title=NASA Discovers First Earth-size Planets Beyond Our Solar System|work=NASA|date=20 December 2011|access-date=19 June 2016|archive-date=16 May 2020|archive-url=https://web.archive.org/web/20200516230313/https://www.nasa.gov/mission_pages/kepler/news/kepler-20-system.html#.V2cfuGM_VuU|url-status=dead}} But because of its size, it can be expected to have an atmosphere of water vapor. The mass of the planet can be approximated to around 0.66–3.04 {{earth mass}}, depending on its composition. An Earth-like composition would have its mass to be around 1.2 {{earth mass}}. Radial velocity measurements suggest an upper limit of {{earth mass|1.4}}.
=Host star=
Kepler-20 is a Sun-like star in the constellation Lyra with a mass of {{Val|0.91|0.03|ul=solar mass}} and a radius of {{Val|0.94|0.06|ul=solar radius}}, and is thought to be 8.8 billion years old, though there is a large uncertainty in its age.{{citation|first1=Jean |last1=Schneider |title=Star : Kepler-20 |url=http://exoplanet.eu/star.php?st=Kepler-20 |access-date=2011-12-21 |url-status=dead |archive-url=https://web.archive.org/web/20120119135819/http://exoplanet.eu/star.php?st=Kepler-20 |encyclopedia=Extrasolar Planets Encyclopaedia |archive-date=2012-01-19 }} The star's metallicity is {{Val|0.01|0.04}}, meaning that the level of iron (and, presumably, other elements) in the star is almost the same as that of the Sun. Metallicity plays an important role in planetary systems, and stars with higher metallicity are more likely to have planets detected around them.{{cite journal|title=The planet-metallicity correlation|journal=The Astrophysical Journal|date=2005-04-01|first=Debra A.|last=Fischer|author2=Valenti, Jeff |volume=622|pages=1102–1117|doi=10.1086/428383|bibcode=2005ApJ...622.1102F|issue=2|doi-access=free}} This may be because the higher metallicity provides more material with which to quickly build planets into gas giants or because the higher metallicity increases planet migration towards the host star, making the planet easier to detect.{{cite book| author = Seager, Sara | title = Exoplanets | chapter = Statistical Distribution of Exoplanets by Andrew Cumming | publisher = University of Arizona Press | date = 2010 | pages = 191–214 | isbn = 978-0-8165-2945-2}} The star has four other known planets in orbit: Kepler-20b, Kepler-20c, Kepler-20d, and Kepler-20e. All of the planets in the system would fit inside the orbit of Mercury.
Kepler-20 has an apparent magnitude of 12.51, too dim to be seen from Earth with the naked eye.
=Orbit=
Kepler-20f revolves around its parent star every 19.58 days at a semi-major axis of {{convert|0.1387|AU|km|abbr=on}}, little over a third of the mean distance between Mercury and the Sun (0.387 AU). This gives the planet an insolation flux (i.e. the amount of radiation it receives from the star) 35.9 times that of the Earth, hence its high temperature. The eccentricity of the orbit is low (below 0.094), similarly to planets in the Solar System (e.g., Mars has an eccentricity of 0.0934). It is the fourth closest planet from the star, the three closer planets being b, e, and c. At least one more planet (d) and possibly another planetary candidate (g) lie farther beyond.
Discovery
In 2009, NASA's Kepler spacecraft was completing observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed {{val|50,000}} stars in the Kepler Input Catalog, including Kepler-20; the preliminary light curves were sent to the Kepler science team for analysis, who chose obvious planetary companions from the bunch for follow-up at observatories. Observations for the potential exoplanet candidates took place between 13 May 2009 and 17 March 2012. After observing the respective transits, which for Kepler-20f occurred roughly every 19 days (its orbital period), it was eventually concluded that a planetary body was responsible for the periodic 19-day transits. The exoplanet, along with the other planets of the Kepler-20 system and other planets around stars studied by Kepler, were announced on December 20, 2011.
References
{{Reflist|refs=
{{Cite journal |last=Bonomo |first=A. S. |last2=Dumusque |first2=X. |last3=Massa |first3=A. |last4=Mortier |first4=A. |last5=Bongiolatti |first5=R. |last6=Malavolta |first6=L. |last7=Sozzetti |first7=A. |last8=Buchhave |first8=L. A. |last9=Damasso |first9=M. |last10=Haywood |first10=R. D. |last11=Morbidelli |first11=A. |last12=Latham |first12=D. W. |last13=Molinari |first13=E. |last14=Pepe |first14=F. |last15=Poretti |first15=E. |date=2023-09-01 |title=Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems |bibcode=2023A&A...677A..33B |journal=Astronomy and Astrophysics |volume=677 |pages=A33 |doi=10.1051/0004-6361/202346211 |issn=0004-6361|arxiv=2304.05773 }}
{{cite web |date=April 7, 2008 |first=Donald K. |last=Yeomans |url=https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%271%27&TABLE_TYPE=%27ELEMENTS%27&START_TIME=%272000-01-01%27&STOP_TIME=%272000-01-02%27&STEP_SIZE=%27200%20years%27&CENTER=%27@Sun%27&OUT_UNITS=%27AU-D%27 |title=HORIZONS Web-Interface for Mercury Major Body |publisher=JPL Horizons On-Line Ephemeris System |access-date=April 7, 2008 |archive-date=August 18, 2023 |archive-url=https://web.archive.org/web/20230818120425/https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND=%271%27&TABLE_TYPE=%27ELEMENTS%27&START_TIME=%272000-01-01%27&STOP_TIME=%272000-01-02%27&STEP_SIZE=%27200%20years%27&CENTER=%27%40Sun%27&OUT_UNITS=%27AU-D%27 |url-status=live }} – Select "Ephemeris Type: Orbital Elements", "Time Span: 2000-01-01 12:00 to 2000-01-02". ("Target Body: Mercury" and "Center: Sun" should be defaulted to.) Results are instantaneous osculating values at the precise J2000 epoch.
}}
{{Sky|19|10|47.524|+|42|20|19.30}}
{{Kepler-20|state=uncollapsed}}
Category:Exoplanets discovered in 2011