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{{Short description|Exoplanet orbiting the star Kepler 1520}}
{{Infobox planet
| name                     = Kepler-1520b
| image                    = KIC 12557548.jpg
| caption                  = Artist's concept of Kepler-1520b orbiting its host star. The planet is rapidly losing mass through the [[sublimation (phase transition)|sublimation]] of its planetary surface and has a tail of dust.
<!-- DISCOVERY           -->
| discoverer               = ''[[Kepler (spacecraft)|Kepler]]'' spacecraft
| discovered               = 2012 (proposed)<br />May 12, 2016 (confirmed)
| discovery_method         = Transit
<!-- DESIGNATIONS        -->
<!-- ORBITAL             --> 
| apsis                    = astron
| semimajor                = {{convert|0.013|AU|km|abbr=on}}<ref name="Kepler-1520">{{cite web |url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-1520+b |title=Kepler-1520 b|work=NASA Exoplanet Science Institute |access-date=2016-08-02 }}</ref>
| period                   = {{val|0.6535538|0.0000001}}<ref name="Van Werkhoven2014"/> [[day|d]]
| inclination              = ~90
| star                     = [[Kepler-1520]]
<!-- PHYS CHARS          --> 
| mean_radius              = <1 (for albedo of 0.5)<ref name="Van Werkhoven2014"/> {{Earth radius|link=y}}
| mass                     = <0.02<ref name="Perez-Becker2013"/> {{Earth mass|link=y}}
| single_temperature       = {{convert|2255|K|C F}}<ref name=ouellette-2012/>
<!-- ATMOSPHERE          --> 
<!-- NOTES               --> 
}}
'''Kepler-1520b''' (initially published as '''KIC 12557548 b'''<ref name="Rappaport2012"/>), is a confirmed [[exoplanet]] orbiting the [[K-type main sequence star]] [[Kepler-1520]]. It is located about 2,020 [[light-year]]s (620 [[parsec]]s) away from Earth in the constellation of [[Cygnus (constellation)|Cygnus]]. 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 was previously proposed in 2012 when reports of its host star recorded drops in its luminosity varying from 0.2% to 1.3%, which indicated a possible planetary companion rapidly disintegrating. In 2015, the planetary nature of the cause of the dips was finally verified.<ref name="Bochinski2015"/> It is expected to disintegrate in about 40–400 million years.

==Physical characteristics==

===Mass, radius, and temperature===
The mass of Kepler-1520b is unknown; however, modeling of the mass loss rate of the planet indicates that it cannot be more massive than about 2% of the mass of the Earth (less than double the mass of the Moon). According to calculations, it may have lost 70% of its original mass; we may be currently observing its naked iron core.<ref name="Perez-Becker2013"/> From attempts to measure the [[secondary eclipse]], the radius of the planet is constrained to be less than one Earth radius (4600&nbsp;km) for an [[albedo]] of 0.5.<ref name="Van Werkhoven2014"/> It has a surface temperature of {{convert|2255|K|C F}}, far hotter than the surface of [[Venus]].<ref name=ouellette-2012/>

===Host star===
{{main|Kepler-1520}}
The planet orbits a ([[Stellar classification#Class K|K-type]]) [[star]] named [[Kepler-1520]]. The star has a mass of 0.76 {{solar mass}} and a radius of 0.71 {{solar radius}}. It has a temperature of 4677 [[Kelvin scale|K]] and is 4.47 billion years old. In comparison, the [[Sun]] is 4.6 billion years old<ref>{{cite web |url=http://www.universetoday.com/18237/how-old-is-the-sun/ |title=How Old is the Sun? |author=Fraser Cain |date=16 September 2008 |publisher=[[Universe Today]] |access-date=19 February 2011}}</ref> and has a surface temperature of 5778 K.<ref>{{cite web |url=http://www.universetoday.com/18092/temperature-of-the-sun/ |title=Temperature of the Sun |author=Fraser Cain |date=15 September 2008 |publisher=Universe Today |access-date=19 February 2011}}</ref>

The star's [[apparent magnitude]], or how bright it appears from Earth's perspective, is 16.7. Therefore, it is too dim to be seen with the naked eye.

===Orbit===
Kepler-1520b orbits its host star with about 14% of the Sun's luminosity with an orbital period of slightly over 12 hours and an orbital radius of about 0.01 times that of Earth's (compared to the distance of [[Mercury (planet)|Mercury]] from the Sun, which is about 0.38 [[Astronomical unit|AU]]). This is one of the closest orbital periods detected yet.

==Remaining lifetime==
Kepler-1520b orbits so close to its host star that it is essentially evaporating into space via [[sublimation (phase transition)|sublimation]], losing about 0.6 to 15.6 Earth masses per billion years.<ref name="Van Lieshout2016"/> Based on predictions made by scientists, Kepler-1520b will cease to exist in about 40–400 million years.<ref name="Perez-Becker2013"/> Calculations of mass loss rates show that the planet probably had a mass slightly smaller than Mercury in size  when it first formed, since the calculations show that planets with masses larger than 7% the Earth's barely lose any mass over billion year time-scales.<ref name="Perez-Becker2013"/>

This discovery helps shed light on how [[Future of the Earth#Red giant stage|the Earth will interact with the Sun when it becomes a red giant]], roughly 5–7 billion years from now.

==Discovery==

===2012 detections===
The existence of the planet was first evidenced in data collected by the ''Kepler'' spacecraft in 2012. However, the light curve of the star, a graph of its stellar flux versus time, showed that while there were regular drops in stellar flux approximately every 15 hours, the amount of light being blocked covered a wide range, from 0.2% to 1.3% of the starlight being blocked.<ref name="Rappaport2012"/> [[Saul Rappaport]] and collaborators proposed various possible phenomena which may have caused the anomalies in the light curve, including two planets orbiting each other,<ref name=hufpo-2012>{{cite news | url=http://www.huffingtonpost.com/2012/05/19/exoplanet-dust-parent-star-heat_n_1529695.html | title=Exoplanet Turning To Dust Under Parent Star's Intense Heat, Scientists Say | work=HuffPost Science | date=May 20, 2012 | agency=TheHuffingtonPost.com, Inc. | access-date=June 11, 2012 | author=Howard, Jacqueline}}</ref> and an eclipsing binary orbiting the star in a larger triple-star system.<ref name="Rappaport2012"/> However, the authors found the hypothetical binary planet system to be unstable<ref name="Rappaport2012"/> and the latter scenario to be poorly supported by the data collected by ''Kepler''.<ref name="Rappaport2012"/>

Therefore, the authors posited that the most likely cause of the observed light curve was a closely orbiting planet, about twice the mass of [[Mercury (planet)|Mercury]], which was rapidly emitting small particles into independent orbits around the star.<ref name="Rappaport2012"/> Exactly the cause of this phenomenon could be the direct [[sublimation (phase transition)|sublimation]] of the planetary surface and its emission into space, the intense volcanism caused by the tidal effects of orbiting extremely close to the host star, or both processes mutually reinforcing the strength of each other in a [[positive feedback loop]].<ref name="Rappaport2012"/>

===2016 confirmation===
Following a campaign of observations using [[William Herschel Telescope]], another group of astronomers was able to detect color dependence of the transit depth, providing independent, direct evidence in favor of this object being a disrupting low-mass rocky planet, feeding a transiting dust cloud.<ref name="Bochinski2015">{{cite journal | title=Direct Evidence for an Evolving Dust Cloud from the Exoplanet KIC 12557548 b | last1=Bochinski | first1=Jakub | last2=Haswell | first2=Carole | last3=Marsh | first3=Tom | last4=Dhillon | first4=Vikram | last5=Littlefair | first5=Stuart | display-authors=1 | journal=Astrophysical Journal Letters | volume=800 | issue=2 | at=L21 | year=2015 | arxiv=1502.04612 | bibcode=2015ApJ...800L..21B  | doi=10.1088/2041-8205/800/2/L21 | s2cid=13917988 | url=https://iopscience.iop.org/article/10.1088/2041-8205/800/2/L21}}</ref> In the new database released by ''Kepler'' in May 2016, the planetary nature of then-KIC 12554578 b was confirmed, and was then upgraded to the name Kepler-1520 b.

==See also==
*[[K2-22b]]
*[[WASP-12b]]
*[[WD 1145+017 b]]

==References==
{{reflist|refs=

<ref name=ouellette-2012>{{cite news | title=Dust to Dust: The Death of an Exoplanet | url=http://news.discovery.com/space/dust-to-dust-death-of-an-exoplanet-120526.html | work=Discovery News | date=May 26, 2012 | agency=Discovery Communications, LLC | access-date=June 9, 2012 | author=Ouellette, Jennifer | archive-date=July 2, 2012 | archive-url=https://web.archive.org/web/20120702234116/http://news.discovery.com/space/dust-to-dust-death-of-an-exoplanet-120526.html | url-status=dead }}</ref>

<ref name="Perez-Becker2013">{{cite journal | title=Catastrophic evaporation of rocky planets | last1=Perez-Becker | first1=Daniel | last2=Chiang | first2=Eugene | journal=Monthly Notices of the Royal Astronomical Society | volume=433 | issue=3 | pages=2294–2309 | year=2013 | arxiv=1302.2147 | bibcode=2013MNRAS.433.2294P | doi=10.1093/mnras/stt895 | doi-access=free }}</ref>

<ref name="Rappaport2012">{{cite journal | title=Possible Disintegrating Short-Period Super-Mercury Orbiting KIC 12557548 | last1=Rappaport | first1=S. | last2=Levine | first2=A. | last3=Chiang | first3=E. | last4=El Mellah | first4=I. | last5=Jenkins | first5=J. | last6=Kalomeni | first6=B. | last7=Kite | first7=E. S. | last8=Kotson | first8=M. | last9=Nelson | first9=L. | last10=Rousseau-Nepton | first10=L. | last11=Tran | first11=K. | display-authors=1 | journal=The Astrophysical Journal | volume=752 | issue=1 | at=1 | year=2012 | arxiv=1201.2662 | bibcode=2012ApJ...752....1R | doi=10.1088/0004-637X/752/1/1 | s2cid=7229181 }}</ref>

<ref name="Van Lieshout2016">{{cite journal | title=Dusty tails of evaporating exoplanets | url=https://www.aanda.org/articles/aa/full_html/2016/12/aa29250-16/aa29250-16.html | last1=Van Lieshout | first1=R. | last2=Min | first2=M. | last3=Dominik | first3=C. | last4=Brogi | first4=M. | last5=De Graaff | first5=T. | last6=Hekker | first6=S. | last7=Kama | first7=M. | last8=Keller | first8=C. U. | last9=Ridden-Harper | first9=A. | last10=Van Werkhoven | first10=T. I. M. | display-authors=1 | journal=Astronomy and Astrophysics | volume=596 | at=A32 | year=2016 | arxiv=1609.00275 | bibcode=2016A&A...596A..32V | doi=10.1051/0004-6361/201629250 | s2cid=67827843 }}</ref>

<ref name="Van Werkhoven2014">{{cite journal | title=Analysis and interpretation of 15 quarters of Kepler data of the disintegrating planet KIC 12557548 b | url=https://www.aanda.org/articles/aa/full_html/2014/01/aa22398-13/aa22398-13.html | last1=Van Werkhoven | first1=T. I. M. | last2=Brogi | first2=M. | last3=Snellen | first3=I. A. G. | last4=Keller | first4=C. U. | display-authors=1 | journal=Astronomy and Astrophysics | volume=561 | at=A3 | year=2014 | arxiv=1311.5688 | bibcode=2014A&A...561A...3V | doi=10.1051/0004-6361/201322398 | s2cid=118701597 }}</ref>

}}

==External links==
* [https://www.google.com/search?hl=en&gl=us&tbm=nws&q=disintegrating+planet&oq=disintegrating+planet&aq=f&aqi=d2&aql=&gs_l=news-cc.3..43j43i400.2031.8101.0.8229.21.4.0.17.0.0.133.493.0j4.4.0...0.0.dbSImTzLwyw Google News link for "disintegrating planet"]

{{Sky|19|23|51.89|+|51|30|17}}
{{2016 in space}}
{{Exoplanets}}
{{Portal bar|Astronomy}}

[[Category:Exoplanets discovered in 2016]]
[[Category:Transiting exoplanets]]
[[Category:Cygnus (constellation)]]
[[Category:Exoplanets discovered by the Kepler space telescope|1520]]
[[Category:Sub-Earth exoplanets]]

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