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{{Short description|Terrestrial exoplanet orbiting Kepler-10}}
{{good article}} {{good article}}
__NOTOC__
{{Planetbox begin
⚫ | name=Kepler-10b
}}
{{Planetbox image
⚫ | image = Exoplanet Comparison Kepler-10 b.png
⚫ | caption = Size comparison of Kepler-10b with Earth
}}
{{Planetbox star
⚫ | star = ]<ref name="datatable"/>
| constell= ]
| RA = {{RA|19|02|43}}<ref name="datatable"/>
| DEC= {{DEC|+50|14|29}}<ref name="datatable"/>
| app_mag = 11.157<ref name="harps"/>
| dist_ly = 564 ± 88
| dist_pc = 173 ± 27<ref name="datatable"/>
| class = G
| mass = 0.910±0.021<ref name="harps"/>
| radius= 1.065±0.009<ref name="harps"/>
| temperature = 5708±28<ref name="harps"/>
⚫ | metallicity = −0.15 ± 0.04<ref name="Batalha2011"/>
⚫ | age = 10.6{{±|1.5|1.3}}<ref name="harps"/>
}}


{{Infobox planet
{{Planetbox character
⚫ | name = Kepler-10b
| radius_earth =1.47{{±|0.03|0.02}}<ref name="harps"/>
⚫ | image = Exoplanet Comparison Kepler-10 b.png
| density_cgs = 5.8±0.8<ref name="harps"/>
⚫ | caption = Size comparison of Kepler-10b with Earth
| mass_earth = 3.33±0.49<ref name="harps"/>
| gravity = 15<ref name="harps"/><!--log gp =3.18 =15 m/s^2--> | discovery_ref = <ref name="Batalha2011"/>
⚫ | discoverer = Batalha ''et al.''
| bond_albedo = ~0.5
| discovered = January 10, 2011
| geometric_albedo = 0.5
⚫ | discovery_method = ] (])
⚫ | temperature = 2500-3040 (day side) <br> 50-75 (night side, assuming no atmosphere)<ref> : Daniel Rouan, Hans J. Deeg, Olivier Demangeon, Benjamin Samuel, Céline Cavarroc, Bruce Fegley, Alain Léger</ref>
| apsis = astron
⚫ | semimajor = 0.01684 {{±|0.00032|0.00034}}<ref name="Batalha2011"/> ]
⚫ | eccentricity = 0<ref name="Batalha2011"/>
⚫ | period = 0.837495<ref name="Batalha2011"/> ]<br>20.0999 ]
⚫ | inclination = 84.4<ref name="Batalha2011"/>
⚫ | semi-amplitude = 3.3 {{±|0.8|1.0}}<ref name="Batalha2011"/>
⚫ | star = ]<ref name="datatable"/>
| mean_radius = {{val|1.47|0.03}}<ref name=Brinkman/> {{earth radius|link=y}}
| mass = {{val|3.58|0.33}}<ref name=Brinkman/> {{Earth mass|link=y}}
| density = {{val|6.46|0.73}} g/cm<sup>3</sup><ref name="Weiss2016"/>
| surface_grav = {{convert|15|m/s2|lk=on|abbr=on}}<ref name="harps"/>
| albedo = 0.5
| single_temperature = {{convert|1833|K|C F}} (day side) <br> {{convert|50|K|C F}} (night side)<ref>{{Cite journal |last=Rouan |first=D. |last2=Deeg |first2=H. J. |last3=Demangeon |first3=O. |last4=Samuel |first4=B. |last5=Cavarroc |first5=C. |last6=Fegley |first6=B. |last7=Léger |first7=A. |date=2011 |title=The orbital phases and secondary transit of Kepler-10b - A physical interpretation based on the ''Lava-ocean'' planet model |journal=The Astrophysical Journal |volume=741 |issue=2 |pages=L30 |arxiv=1109.2768 |bibcode=2011ApJ...741L..30R |doi=10.1088/2041-8205/741/2/L30}}</ref>
}} }}
⚫ '''Kepler-10b''' is the first confirmed ] to have been discovered outside the ] by the Kepler Space Telescope.<ref name= "BBCNews"/> Discovered after several months of data collection during the course of the ]-directed ], which aims to discover ]-like planets ] their host stars, the planet's discovery was announced on January 10, 2011. Kepler-10b has a mass of 3.72±0.42 ]es and a radius of 1.47 ]. However, it lies extremely close to its star, ], and as a result is too hot to support life as we know it. Its existence was confirmed using measurements from the ] in Hawaii.
{{Planetbox orbit
⚫ | period = 0.837495<ref name="Batalha2011"/>
| period_hour = 20.0999
⚫ | semimajor = 0.01684 {{±|0.00032|0.00034}}<ref name="Batalha2011"/>
| semimajor_gm = 2.520
| eccentricity = 0<ref name="Batalha2011"/>
⚫ | inclination = 84.4<ref name="Batalha2011"/>
| semi-amp = 3.3 {{±|0.8|1.0}}<ref name="Batalha2011"/>
}}
{{Planetbox discovery
| discovery_date = 2011-01-10
⚫ | discoverers = Batalha ''et al.''
⚫ | discovery_method = ] (])
| detection_methods = Radial velocity<br>Reflection/emission modulations
| discovery_status = Confirmed
}}
{{Planetbox end}}

⚫ '''Kepler-10b''' is the first confirmed ] to have been discovered outside the ].<ref name= "BBCNews"/> Discovered after several months of data collection during the course of the ]-directed ], which aims to discover ]-like planets ] their host stars, the planet's discovery was announced on January 10, 2011. Kepler-10b has a mass of 3.33±0.49 ]es and a radius of 1.4 ]. However, it lies extremely close to its star, ], and as a result is too hot to support life. Its existence was confirmed using measurements from the ] in Hawaii.


==Nomenclature and history== ==Nomenclature and history==
], the star that hosts Kepler-10b, is located 560 ]s from our solar system in the ]. It is approximately the same size as the ], with an estimated age of 12&nbsp;billion years.<ref name="kepler10bData" /> Planet Kepler-10b was the first planet to be discovered in the orbit of its star. For this, it was designated the star's ''b'' planet. The star, in turn, was named for the Kepler Mission, a NASA-led operation aimed at discovering terrestrial planets that ], or cross in front of, their host stars with respect to Earth.<ref>{{cite web |url=http://kepler.nasa.gov/Mission/QuickGuide/ |title=Kepler: About the Mission |author= |year=2010 |work=Kepler Mission |publisher=] |accessdate=6 March 2011}}</ref> The planet's discovery was announced to the public on January 10, 2011.<ref name="Dennis Overbye">{{cite news |url=http://www.nytimes.com/2011/01/11/science/space/11planet.html |title=Kepler-10b, a Lethally Hot Exoplanet, Is Discovered |author=Dennis Overbye |date=10 January 2011 |work= |publisher='']'' |accessdate=6 March 2011}}</ref> ], the star that hosts Kepler-10b, is located 560 ]s from the Solar System in the ]. It is approximately the same size as the ], with an estimated age of 12&nbsp;billion years.<ref name="kepler10bData" /> Planet Kepler-10b was the first planet to be discovered in the orbit of its star. For this, it was designated the star's ''b'' planet. The star, in turn, was named for the Kepler Mission, a NASA-led operation aimed at discovering terrestrial planets that ], or cross in front of, their host stars with respect to Earth.<ref name="Mission overview"/> The planet's discovery was announced to the public on January 10, 2011.<ref name="Dennis Overbye">{{cite news | url=https://www.nytimes.com/2011/01/11/science/space/11planet.html |title=Kepler-10b, a Lethally Hot Exoplanet, Is Discovered | author=Dennis Overbye | date=10 January 2011 | newspaper=] | access-date=6 March 2011}}</ref>
] for Kepler-10b, demonstrating the dimming effect as it ] its star]] ] for Kepler-10b, demonstrating the dimming effect as it ] its star]]
The transit method of discovering ]s relies upon carefully monitoring the brightness of a star. If a planet is present and crosses the line of sight between Earth and the star, the star will dim at a regular interval by an amount that depends upon the radius of the transiting planet. In order to measure the mass of a planet, and rule out other phenomena that can mimic the presence of a planet transiting a star, candidate transiting planets are followed up with the ] of detecting extrasolar planets.<ref name="Seager2003" /> The transit method of discovering ]s relies upon carefully monitoring the brightness of a star. If a planet is present and crosses the line of sight between Earth and the star, the star will dim at a regular interval by an amount that depends upon the radius of the transiting planet. In order to measure the mass of a planet, and rule out other phenomena that can mimic the presence of a planet transiting a star, candidate transiting planets are followed up with the ] of detecting extrasolar planets.<ref name="Seager2003" />


Kepler-10b's discovery was based on eight months of data collected with the Kepler telescope from May 2009 to January 2010. The planet's first transits were observed in July 2009. According to the collected data, Kepler-10 dimmed by one part in ten thousand every 0.83 days.<ref name="NASANews"/><ref name="WiredScience" /> Kepler-10 was the first star in the ] of the Kepler telescope identified as capable of harboring a small transiting planet, and was considered a high priority target for ground based radial velocity observations intended to confirm the mass of Kepler-10b. Radial velocity measurements with the ] telescope taken intermittently between August 2009 and August 2010 revealed a periodic ] in the spectrum of Kepler-10 consistent with a planet of the nature observed by Kepler, confirming the planet's existence and allowing its mass to be determined.<ref name="Batalha2011">{{cite journal |last1= Batalha |first=N. M. |author2=et al. |year= 2011 |title=Kepler's First Rocky Planet: Kepler-10b |journal=] |volume=729 |issue= |pages=27 |arxiv=1102.0605 |bibcode= 2011ApJ...729...27B|doi=10.1088/0004-637X/729/1/27}}</ref><ref name="NASANews"/> The planet's discovery was announced to the public on January 10, 2011.<ref name="Dennis Overbye"/> Kepler-10b's discovery was based on eight months of data collected with the Kepler telescope from May 2009 to January 2010. The planet's first transits were observed in July 2009. According to the collected data, Kepler-10 dimmed by one part in ten thousand every 0.83 days.<ref name="NASANews"/><ref name="WiredScience" /> Kepler-10 was the first star in the ] of the Kepler telescope identified as capable of harboring a small transiting planet, and was considered a high priority target for ground-based radial velocity observations intended to confirm the mass of Kepler-10b. Radial velocity measurements with the ] telescope taken intermittently between August 2009 and August 2010 revealed a periodic ] in the spectrum of Kepler-10 consistent with a planet of the nature observed by Kepler, confirming the planet's existence and allowing its mass to be determined.<ref name="Batalha2011"/><ref name="NASANews"/> The planet's discovery was announced to the public on January 10, 2011.<ref name="Dennis Overbye"/>


⚫ In September 2011, the detection of secondary transit and phases were announced. This allowed to determine the temperature and albedo of the planet. This is the first terrestrial exoplanet with observed phases. Detection of phases was possible due to extreme day/night side temperature variations and the amount of starlight the planet receives due to its proximity to the host star.<ref> : Daniel Rouan, Hans J. Deeg, Olivier Demangeon, Benjamin Samuel, Céline Cavarroc, Bruce Fegley, Alain Léger</ref>
On January 13, 2011, 3 days after the planet's discovery was announced, '']'' published an article suggesting “Vulcan” as an unofficial name for the planet, after both ], and the ].<ref>{{cite news| url=http://www.economist.com/node/17899742 | work=The Economist | title=Vulcan? | date=2011-01-13}}</ref>

In September 2011, the detection of secondary transit and phases were announced. This allowed to determine the temperature and albedo of the planet. This is the first terrestrial exoplanet with observed phases. Detection of phases was possible due to extreme day/night side temperature variations and the amount of starlight the planet receives due to its proximity to the host star. <ref> : Daniel Rouan, Hans J. Deeg, Olivier Demangeon, Benjamin Samuel, Céline Cavarroc, Bruce Fegley, Alain Léger</ref>


===Reaction=== ===Reaction===
Kepler-10b's discovery excited astronomers, who hoped to use data about it to inquire into the formation and structure that terrestrial, Earth-size planets tend to have in common.<ref>{{cite news |url=http://content.usatoday.com/communities/sciencefair/post/2011/01/rocky-exoplanet-reaction-round-up/1 |title=Kepler's rocky exoplanet reaction round-up |author=Dan Vergano |date=10 January 2011 |work=Science Fair |publisher='']'' |accessdate=11 March 2011}}</ref> ] of the ] at ] said that the discovery was ranked “as among the most profound scientific discoveries in human history,” and that the planet “will go into every textbook worldwide.” Marcy also described Kepler-10b as "a bridge between the gas giant planets we’ve been finding and the Earth itself."<ref>{{cite news |url=http://www.dailymail.co.uk/sciencetech/article-1346085/Kepler-10b-planet-missing-link-Earth-Alien-world-rock-gas.html |title=Planet could be 'missing link' to Earth: Alien world is made of rock, not gas|author=David Derbyshire |date=12 January 2011 |work=Science & Tech |publisher=] |accessdate=11 March 2011 |location=London}}</ref> Diana Valencia at the University of Côte d'Azur in Nice, France considered the planet more of a "super-Mercury" than a super-Earth, granted its physical characteristics.<ref>{{cite web |url=http://www.sciencenews.org/view/generic/id/68586/title/New_planet_small_but_tough |title=New Planet Small But Tough |author=Ron Cowen |date=12 February 2011 |work= |publisher=ScienceNews |accessdate=11 March 2011}}</ref> Kepler-10b's discovery excited astronomers, who hoped to use data about it to inquire into the formation and structure that terrestrial, Earth-size planets tend to have in common.<ref>{{cite news |url=http://content.usatoday.com/communities/sciencefair/post/2011/01/rocky-exoplanet-reaction-round-up/1 |title=Kepler's rocky exoplanet reaction round-up |author=Dan Vergano |date=10 January 2011 |work=Science Fair |publisher=] |access-date=11 March 2011}}</ref> Diana Valencia at the University of Côte d'Azur in Nice, France considered the planet more of a "super-Mercury" than a super-Earth, granted its physical characteristics.<ref>{{cite web |url=http://www.sciencenews.org/view/generic/id/68586/title/New_planet_small_but_tough |title=New Planet Small But Tough |author=Ron Cowen |date=12 February 2011 |publisher=ScienceNews |access-date=11 March 2011}}</ref>


==Characteristics== ==Characteristics==
] ]
Kepler-10b is most noted for its rocky surface. It has a diameter 1.4&nbsp;times that of the ], and a mass of 3.33±0.49 times that of Earth.<ref name="harps"/> The density of Kepler-10b is 5.8±0.8 ] cm<sup>−3</sup>. It orbits its star, ], in less than a day, at less than a twentieth of the distance from ] to the ]. Its surface temperature on the star lit side is approximately 1833&nbsp;],<ref name="Kepler-10b">{{cite web|date=2011-01-10|title=Kepler Discoveries: Kepler-10b|publisher=Kepler @ NASA|url=http://kepler.nasa.gov/Mission/discoveries/kepler10b/|accessdate=2011-01-12}}</ref> which is as hot as a ] and hot enough to melt iron.<ref name="WiredScience" /> Kepler-10b is most noted for its rocky surface. It has a diameter 1.47&nbsp;times that of the ]. The mass of Kepler-10b is 3.58 times that of Earth<ref name=Brinkman/> and the average density is {{val|6.46}} ].<ref name="Weiss2016"/> It orbits its star, ], in less than a day, at less than a twentieth of the distance from ] to the ]. Its surface temperature on the star lit side is approximately 1,833&nbsp;],<ref name="Kepler-10b">{{cite web|date=2011-01-10|title=Kepler Discoveries: Kepler-10b|publisher=Kepler @ NASA|url=http://kepler.nasa.gov/Mission/discoveries/kepler10b/|archive-url=https://web.archive.org/web/20110721122709/http://kepler.nasa.gov/Mission/discoveries/kepler10b/|url-status=dead|archive-date=2011-07-21|access-date=2011-01-12}}</ref> which is as hot as a ] and hot enough to melt iron.<ref name="WiredScience" />


Though ] was discovered before Kepler-10b and has been claimed to be rocky, there is more room for other interpretations in the case of CoRoT-7b's composition than there is for Kepler-10b.<ref name="WiredScience" /> This is due to the much larger uncertainty in CoRoT-7b's mass (and, to a lesser extent, its radius) which is illustrated in the plot to the left. Consequently, CoRoT-7b may be revealed to be a ],{{clarify||Lava planets are also terrestrial, i.e. "predominantly made of rock or iron"|date=March 2014}} whereas Kepler-10b must be predominantly made of rock or iron. In addition to showing the range of masses and radii consistent with the observations of each planet, the plot includes curves of compositions implied by certain masses and radii. Though ] was discovered before Kepler-10b and has been claimed to be rocky, there is more room for other interpretations in the case of CoRoT-7b's composition than there is for Kepler-10b, due to its highly uncertain mass — for example, it could be predominantly water rather than rock and iron.<ref name="WiredScience" />


Kepler-10b is tidally locked to its parent star and has extreme variations in temperature between day and night sides. It also reflects about half of the starlight it receives. Kepler-10b is tidally locked to its parent star and has extreme variations in temperature between day and night sides. It also reflects about half of the starlight it receives. One possible explanation for the high Bond albedo could be that Kepler-10b is a ] with surface magma oceans rich in iron oxides.<ref>Modirrousta-Galian, D., Ito, Y. and Micela, G., (2020). Exploring super-Earth surfaces: Albedo of near-airless magma ocean planets and topography. Icarus, p.114175.</ref>


==See also== ==See also==
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* ] * ]
* ], ], ], ], ], ], ] * ], ], ], ], ], ], ]
* ] * ]


==References== ==References==
{{reflist|refs= {{reflist|refs=

⚫ <ref name="BBCNews">
⚫ {{cite news |url=https://www.bbc.co.uk/news/science-environment-12158028 |title= BBC News|date=2010-01-10 |publisher=BBC|access-date=2010-11-01}}</ref>

<ref name="Batalha2011">{{cite journal | title=Kepler's First Rocky Planet: Kepler-10b | last1=Batalha | first1=Natalie M. | last2=Borucki | first2=William J. | last3=Bryson | first3=Stephen T. | last4=Buchhave | first4=Lars A. | last5=Caldwell | first5=Douglas A. | last6=Christensen-Dalsgaard | first6=Jørgen | last7=Ciardi | first7=David | last8=Dunham | first8=Edward W. | last9=Fressin | first9=Francois | last10=Gautier | first10=Thomas N. | last11=Gilliland | first11=Ronald L. | last12=Haas | first12=Michael R. | last13=Howell | first13=Steve B. | last14=Jenkins | first14=Jon M. | last15=Kjeldsen | first15=Hans | last16=Koch | first16=David G. | last17=Latham | first17=David W. | last18=Lissauer | first18=Jack J. | last19=Marcy | first19=Geoffrey W. | last20=Rowe | first20=Jason F. | last21=Sasselov | first21=Dimitar D. | last22=Seager | first22=Sara | last23=Steffen | first23=Jason H. | last24=Torres | first24=Guillermo | last25=Basri | first25=Gibor S. | last26=Brown | first26=Timothy M. | last27=Charbonneau | first27=David | last28=Christiansen | first28=Jessie | last29=Clarke | first29=Bruce | last30=Cochran | first30=William D. | display-authors=1 | journal=The Astrophysical Journal | volume=729 | issue=1 | pages=27 | year=2011 | arxiv=1102.0605 | bibcode=2011ApJ...729...27B | doi=10.1088/0004-637X/729/1/27 | s2cid=55059000 }}</ref>


<ref name="datatable"> <ref name="datatable">
{{cite web |url=http://kepler.nasa.gov/Mission/discoveries/ |title=Summary Table of Kepler Discoveries |date=2010-08-26 |work= |publisher=NASA|accessdate=2010-09-01}}</ref> {{cite web |url=http://kepler.nasa.gov/Mission/discoveries/ |archive-url=https://web.archive.org/web/20100527104316/http://kepler.nasa.gov/Mission/discoveries/ |url-status=dead |archive-date=2010-05-27 |title=Summary Table of Kepler Discoveries |date=2010-08-26 |publisher=NASA|access-date=2010-09-01}}</ref>

<ref name="harps">{{Cite journal |last=Dumusque |first=Xavier |last2=Bonomo |first2=Aldo S. |last3=Haywood |first3=Raphaelle D. |last4=Malavolta |first4=Luca |last5=Segransan |first5=Damien |last6=Buchhave |first6=Lars A. |last7=Cameron |first7=Andrew Collier |last8=Latham |first8=David W. |last9=Molinari |first9=Emilio |last10=Pepe |first10=Francesco |last11=Udry |first11=Stephane |last12=Charbonneau |first12=David |last13=Cosentino |first13=Rosario |last14=Dressing |first14=Courtney D. |last15=Figueira |first15=Pedro |date=2014-06-24 |title=The Kepler-10 planetary system revisited by HARPS-N: A hot rocky world and a solid Neptune-mass planet |url=https://arxiv.org/abs/1405.7881 |journal=The Astrophysical Journal |volume=789 |issue=2 |pages=154 |doi=10.1088/0004-637X/789/2/154 |issn=0004-637X}}</ref>


<ref name="kepler10bData"> <ref name="kepler10bData">
{{cite web | url = http://kepler.nasa.gov/Mission/discoveries/kepler10b/ | title = Kepler-10b | date = 2011-01-10 | publisher = NASA | accessdate = 2010-01-15}}</ref> {{cite web | url = http://kepler.nasa.gov/Mission/discoveries/kepler10b/ | archive-url = https://web.archive.org/web/20110721122709/http://kepler.nasa.gov/Mission/discoveries/kepler10b/ | url-status = dead | archive-date = 2011-07-21 | title = Kepler-10b | date = 2011-01-10 | publisher = NASA | access-date = 2010-01-15}}</ref>


<ref name="Mission overview">{{cite web | title=Mission overview | url=https://www.nasa.gov/mission_pages/kepler/overview/index.html | work=Kepler and K2 | date=13 April 2015 | publisher=NASA | access-date=3 December 2017}}</ref>
⚫ <ref name="BBCNews">
⚫ {{cite news |url=http://www.bbc.co.uk/news/science-environment-12158028 |title= BBC News|date=2010-01-10 |publisher=BBC|accessdate=2010-11-01}}</ref>


⚫ <ref name="NASANews">{{cite web |url=http://www.nasa.gov/topics/universe/features/rocky_planet.html |title=NASA'S Kepler Mission Discovers Its First Rocky Planet |date=2011-01-10 |publisher=NASA |access-date=2011-01-10 |archive-date=2015-06-27 |archive-url=https://web.archive.org/web/20150627200219/http://www.nasa.gov/topics/universe/features/rocky_planet.html |url-status=dead }}</ref>
<ref name="NASANews">

⚫ {{cite web |url=http://www.nasa.gov/topics/universe/features/rocky_planet.html |title=NASA'S Kepler Mission Discovers Its First Rocky Planet |date=2011-01-10 |work= |publisher=NASA|accessdate=2011-01-10}}</ref>
⚫ <ref name="Seager2003">{{Cite journal | last1 = Seager | first1 = S. | last2 = Mallen‐ornelas | first2 = G. | date = 2003 | title = A Unique Solution of Planet and Star Parameters from an Extrasolar Planet Transit Light Curve | journal = ] | volume = 585 | issue = 2 | pages = 1038–1055 | arxiv = astro-ph/0206228 | bibcode=2003ApJ...585.1038S | doi = 10.1086/346105| s2cid = 14274640 }}</ref>


<ref name="WiredScience"> <ref name="WiredScience">
{{cite web | url = http://www.wired.com/wiredscience/2011/01/kepler-rocky-world/ | title = Kepler Finds First Definitively Rocky Exoplanet | author = Grossman, Lisa | date = 2010-01-10 | publisher = Wired | accessdate = 2011-01-15}}</ref> {{cite magazine | url = https://www.wired.com/wiredscience/2011/01/kepler-rocky-world/ | title = Kepler Finds First Definitively Rocky Exoplanet | author = Grossman, Lisa | date = 2010-01-10 | magazine = Wired | access-date = 2011-01-15 | archive-url = https://web.archive.org/web/20140602142730/http://www.wired.com/2011/01/kepler-rocky-world/ | archive-date = 2014-06-02 }}</ref>

⚫ <ref name="Seager2003">{{Cite journal | last1 = Seager | first1 = S. | last2 = Mallen‐ornelas | first2 = G. | year = 2003 | title = A Unique Solution of Planet and Star Parameters from an Extrasolar Planet Transit Light Curve | journal = ] | volume = 585 | issue = 2 | pages = 1038–1055 | arxiv = astro-ph/0206228 | bibcode=2003ApJ...585.1038S | doi = 10.1086/346105}}</ref>


<ref name = "Weiss2016">,
<ref name="harps">, Xavier Dumusque, Aldo S. Bonomo, Raphaelle D. Haywood, Luca Malavolta, Damien Segransan, Lars A. Buchhave, Andrew Collier Cameron, David W. Latham, Emilio Molinari, Francesco Pepe, Stephane Udry, David Charbonneau, Rosario Cosentino, Courtney D. Dressing, Pedro Figueira, Aldo F. M. Fiorenzano, Sara Gettel, Avet Harutyunyan, Keith Horne, Mercedes Lopez-Morales, Christophe Lovis, Michel Mayor, Giusi Micela, Fatemeh Motalebi, Valerio Nascimbeni, David F. Phillips, Giampaolo Piotto, Don Pollacco, Didier Queloz, Ken Rice, Dimitar Sasselov, Alessandro Sozzetti, Andrew Szentgyorgyi, Chris Watson, (Submitted on 30 May 2014)</ref>
Weiss L. M., et al., 2016, Astrophys. J., 819, 83</ref>
}} }}


==External links== ==External links==
{{commonscat-inline|Kepler-10 b}} * {{Commons category-inline|Kepler-10 b}}
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{{Kepler-10}} {{Kepler-10}}
{{2011 in space}}
{{Stars of Draco}}


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Latest revision as of 23:24, 8 October 2024

Terrestrial exoplanet orbiting Kepler-10

Kepler-10b
Size comparison of Kepler-10b with Earth
Discovery
Discovered byBatalha et al.
Discovery dateJanuary 10, 2011
Detection methodTransit (Kepler Mission)
Orbital characteristics
Semi-major axis0.01684
−0.00034 AU
Eccentricity0
Orbital period (sidereal)0.837495 d
20.0999 h
Inclination84.4
Semi-amplitude3.3
−1.0
StarKepler-10
Physical characteristics
Mean radius1.47±0.03 R🜨
Mass3.58±0.33 ME
Mean density6.46±0.73 g/cm
Surface gravity15 m/s (49 ft/s)
Albedo0.5
Temperature1,833 K (1,560 °C; 2,840 °F) (day side)
50 K (−223.2 °C; −369.7 °F) (night side)

Kepler-10b is the first confirmed terrestrial planet to have been discovered outside the Solar System by the Kepler Space Telescope. Discovered after several months of data collection during the course of the NASA-directed Kepler Mission, which aims to discover Earth-like planets crossing in front of their host stars, the planet's discovery was announced on January 10, 2011. Kepler-10b has a mass of 3.72±0.42 Earth masses and a radius of 1.47 Earth radii. However, it lies extremely close to its star, Kepler-10, and as a result is too hot to support life as we know it. Its existence was confirmed using measurements from the W.M. Keck Observatory in Hawaii.

Nomenclature and history

Kepler-10, the star that hosts Kepler-10b, is located 560 light-years from the Solar System in the Draco constellation. It is approximately the same size as the Sun, with an estimated age of 12 billion years. Planet Kepler-10b was the first planet to be discovered in the orbit of its star. For this, it was designated the star's b planet. The star, in turn, was named for the Kepler Mission, a NASA-led operation aimed at discovering terrestrial planets that transit, or cross in front of, their host stars with respect to Earth. The planet's discovery was announced to the public on January 10, 2011.

The light curve for Kepler-10b, demonstrating the dimming effect as it transits its star

The transit method of discovering exoplanets relies upon carefully monitoring the brightness of a star. If a planet is present and crosses the line of sight between Earth and the star, the star will dim at a regular interval by an amount that depends upon the radius of the transiting planet. In order to measure the mass of a planet, and rule out other phenomena that can mimic the presence of a planet transiting a star, candidate transiting planets are followed up with the radial velocity method of detecting extrasolar planets.

Kepler-10b's discovery was based on eight months of data collected with the Kepler telescope from May 2009 to January 2010. The planet's first transits were observed in July 2009. According to the collected data, Kepler-10 dimmed by one part in ten thousand every 0.83 days. Kepler-10 was the first star in the field of view of the Kepler telescope identified as capable of harboring a small transiting planet, and was considered a high priority target for ground-based radial velocity observations intended to confirm the mass of Kepler-10b. Radial velocity measurements with the Keck I telescope taken intermittently between August 2009 and August 2010 revealed a periodic Doppler shift in the spectrum of Kepler-10 consistent with a planet of the nature observed by Kepler, confirming the planet's existence and allowing its mass to be determined. The planet's discovery was announced to the public on January 10, 2011.

In September 2011, the detection of secondary transit and phases were announced. This allowed to determine the temperature and albedo of the planet. This is the first terrestrial exoplanet with observed phases. Detection of phases was possible due to extreme day/night side temperature variations and the amount of starlight the planet receives due to its proximity to the host star.

Reaction

Kepler-10b's discovery excited astronomers, who hoped to use data about it to inquire into the formation and structure that terrestrial, Earth-size planets tend to have in common. Diana Valencia at the University of Côte d'Azur in Nice, France considered the planet more of a "super-Mercury" than a super-Earth, granted its physical characteristics.

Characteristics

Diagram showing composition of Kepler-10b in comparison with other planets and exoplanets

Kepler-10b is most noted for its rocky surface. It has a diameter 1.47 times that of the Earth. The mass of Kepler-10b is 3.58 times that of Earth and the average density is 6.46 g/cm. It orbits its star, Kepler-10, in less than a day, at less than a twentieth of the distance from Mercury to the Sun. Its surface temperature on the star lit side is approximately 1,833 K, which is as hot as a blast furnace and hot enough to melt iron.

Though CoRoT-7b was discovered before Kepler-10b and has been claimed to be rocky, there is more room for other interpretations in the case of CoRoT-7b's composition than there is for Kepler-10b, due to its highly uncertain mass — for example, it could be predominantly water rather than rock and iron.

Kepler-10b is tidally locked to its parent star and has extreme variations in temperature between day and night sides. It also reflects about half of the starlight it receives. One possible explanation for the high Bond albedo could be that Kepler-10b is a coreless rocky planet with surface magma oceans rich in iron oxides.

See also

References

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  6. Rouan, D.; Deeg, H. J.; Demangeon, O.; Samuel, B.; Cavarroc, C.; Fegley, B.; Léger, A. (2011). "The orbital phases and secondary transit of Kepler-10b - A physical interpretation based on the Lava-ocean planet model". The Astrophysical Journal. 741 (2): L30. arXiv:1109.2768. Bibcode:2011ApJ...741L..30R. doi:10.1088/2041-8205/741/2/L30.
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  14. The orbital phases and secondary transit of Kepler-10b - A physical interpretation based on the Lava-ocean planet model : Daniel Rouan, Hans J. Deeg, Olivier Demangeon, Benjamin Samuel, Céline Cavarroc, Bruce Fegley, Alain Léger
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