| 词条 | WD 1145+017 b |
| 释义 |
| name = WD 1145+017 b | image = Artist's impression of a white dwarf devouring a minor planet.jpg | caption = Artist's impression of a rocky planetary object being vaporized by its parent star, possibly compatible with WD 1145+017 b's known data. | discoverer = K2 (Kepler) mission | discovered = 21 October 2015 | discovery_method = Transit method | apsis = astron | semimajor = ~0.005 AU | period = 0.1875 (± 0.04)[1] d | inclination = ~89? | star = WD 1145+017 | mean_radius = ~0.15[2] {{Earth radius|link=y}} | mass = 0.0006678[1] {{Earth mass|link=y}} | single_temperature = ≥{{convert|4000|K|C F}} }} WD 1145+017 b (also known by its EPIC designation EPIC 201563164.01), is a confirmed exoplanetary object, likely rocky, orbiting the white dwarf star WD 1145+017. It was discovered by NASA's Kepler spacecraft on its "Second Light" mission. It is located about 570 light-years (174 parsecs, or nearly {{val|5.393|e=15}} km) away from Earth in the constellation of Virgo. The object 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 minor planet is notable because it is the first observed planetary object to transit a white dwarf, providing clues of its possible interactions when its parent star reached the end of its lifetime as a red giant. CharacteristicsMass, radius, and temperatureWD 1147+017 b is a dwarf planet, an exoplanet that has a mass and radius smaller than that of Earth. It likely has a surface temperature of around {{convert|4000|K|C F}} based on its extreme proximity to its star. It has a likely radius of 0.15 {{Earth radius}}, around 1,000 kilometers, about two times larger than the size of the dwarf planet Ceres in the Solar System, which has a radius of about {{convert|490|km|mi}}. The exoplanetary object has a mass of 0.0006678 {{Earth mass}}.[1] Host starThe planetary object orbits a (DB-type) white dwarf star. It has ended its main sequence lifetime and will continue to cool for billions of years to come in the future. Based on recent studies and its mass, the star was likely an early F-type main sequence star (spectral type F0) before it became a red giant.[3] The star has a mass of 0.6 {{solar mass}} and a radius of 0.02 {{solar radius}} (1.4 {{Earth radius}}). It has a temperature of 15900 K and its cooling age is 175 million years. In comparison, the Sun is 4.6 billion years old[4] and has a surface temperature of 5778 K.[5] The star's apparent magnitude, or how bright it appears from Earth's perspective, is 17. Therefore, it is too dim to be seen with the naked eye. OrbitWD 1145+017 b orbits its host star with an orbital period of 0.1875 days and an orbital radius of about 0.005 times that of Earth's (compared to the distance of Mercury from the Sun, which is about 0.38 AU). It is one of the shortest orbital periods known so far, with several other exoplanets having shorter periods. VaporizationWD 1145+047 b is currently being vaporized by its star because of its extreme proximity to it.[2] White dwarfs are usually the size of the Earth, and have half as much mass as they did during the main sequence. Due to this and the searing hot temperature of the stellar remnant, rocky minerals are being vaporized off the surface of this object, into orbit around the star, which is responsible for a hot dusty disk that was observed around its host star. It is likely that WD 1145+017 b is bound to disintegrate in the future (around 100–200 million years from now) due to further vaporization and ablation. The minor planet is likely being pelted by several smaller objects of up to {{convert|90|km|mi}}, as it is likely not just a single object orbiting the white dwarf star, but likely several planetesimals, which is probably responsible for some of the variations in the light curve data.[2] The smaller objects can also throw debris into orbit upon impact, which may also be responsible for the variations. In some way, it helps explain how a planetary system may evolve after its host star has thrown off its outer layers in a planetary nebula, eventually dying as a black dwarf.[3] DiscoveryThe planetary object was discovered by the Kepler spacecraft on its secondary mission, K2: Second Light, an extension of its original mission from 2009 to 2013. Observations were taken over a period of about a month starting from April 2015 using the 1.2-meter telescope at the Fred L. Whipple Observatory along with another telescope located in Chile.[2] The white dwarf star was not originally targeted as part of the mission, however data revealed that there was dips in this star's light curve, and as such investigations were made to figure out what causing the dips, just like the same procedure that was used on the stars that were targeted by the K2 mission. Two transits were detected on 11 April over a period of 4 hours apart, and again on 17 April, however this one was 180° out of phase (inclination probably) from the 11 April transits. The spectra of WD 1145+047 was studied and it revealed that the star contained magnesium, aluminum, silicon, calcium, iron, and nickel.[2] The settling times for these elements were much shorter than the cooling age of the white dwarf (175 Myr), so they must have been deposited fairly recently, as much as probably only 1–2 million years ago. It was suggested that this was evidence for a disintegrating rocky minor planet orbiting around WD 1145+047 with a low mass of 0.0006678 {{Earth mass}}, comparable to the mass of some of the large asteroids in the Solar System. The discovery was then published in the online journal Nature on 22 October 2015, describing the nature of the system.[6] See also
Notes{{notelist}}References1. ^1 2 {{cite web|url=http://exoplanet.eu/catalog/wd_1145%2B017_b/|title=Notes for planet WD 1145+017 b|accessdate=14 August 2016}} 2. ^1 2 3 4 {{Cite journal|arxiv=1510.06387|last1=Vanderburg|first1=Andrew|title=A disintegrating minor planet transiting a white dwarf|journal=Nature|volume=526|issue=7574|pages=546–549|author2=John Asher Johnson|last3=Rappaport|first3=Saul|last4=Bieryla|first4=Allyson|last5=Irwin|first5=Jonathan|author6=John Arban Lewis|last7=Kipping|first7=David|last8= Brown|first8=Warren R.|last9=Dufour|first9=Patrick|last10= Ciardi|first10=David R.|last11=Angus|first11=Ruth|last12=Schaefer|first12=Laura|last13= Latham|first13=David W.|last14=Charbonneau|first14=David|last15=Beichman|first15=Charles|last16=Eastman|first16=Jason|last17=McCrady|first17=Nate|last18= Wittenmyer|first18=Robert A.|last19= Wright|first19=Jason T.|year=2015|doi=10.1038/nature15527|pmid=26490620|bibcode = 2015Natur.526..546V }} 3. ^1 {{cite arXiv|eprint=1601.05419|last1=Veras|first1=Dimitri|title=Post-main-sequence planetary system evolution|class=astro-ph.EP|year=2016}} 4. ^{{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 |work= |publisher=Universe Today |accessdate=19 February 2011}} 5. ^{{cite web |url=http://www.universetoday.com/18092/temperature-of-the-sun/ |title=Temperature of the Sun |author=Fraser Cain |date=15 September 2008 |work= |publisher=Universe Today |accessdate=19 February 2011}} 6. ^A disintegrating minor planet transiting a white dwarf 22 October 2015. Retrieved 14 August 2016. External links
3 : Exoplanets discovered in 2015|Exoplanets discovered by Kepler (spacecraft)|White dwarfs |
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