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Debris disk
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<h2 id="observation-history">Observation history</h2> <p>In 1984 a debris disk was detected around the star <a href="/facts/Vega/G3wJwhhl">Vega</a> using the <a href="/facts/IRAS/MaYMxytq">IRAS</a> satellite. Initially this was believed to be a <a href="/facts/Protoplanetary_disk/FtfSbP61">protoplanetary disk</a>, but it is now known to be a debris disk due to the lack of gas in the disk and the age of the star. The first four debris disks discovered with IRAS are known as the "fabulous four": <a href="/facts/Vega/G3wJwhhl">Vega</a>, <a href="/facts/Beta_Pictoris/QyTtCCHu">Beta Pictoris</a>, <a href="/facts/Fomalhaut/eQ4LC29E">Fomalhaut</a>, and <a href="/facts/Epsilon_Eridani/5LMmzaXl">Epsilon Eridani</a>. Subsequently, direct images of the Beta Pictoris disk showed irregularities in the dust, which were attributed to gravitational perturbations by an unseen <a href="/facts/Exoplanet/zjfmqfUf">exoplanet</a>.<a class="footnote-ref" id="fnref:4" href="#fn:4"><sup>4</sup></a> That explanation was confirmed with the 2008 discovery of the exoplanet <a href="/facts/Beta_Pictoris_b/9XhDUa7u">Beta Pictoris b</a>.<a class="footnote-ref" id="fnref:5" href="#fn:5"><sup>5</sup></a> </p><p>Other exoplanet-hosting stars, including the first discovered by direct imaging (<a href="/facts/HR_8799/kFBfC1WL">HR 8799</a>), are known to also host debris disks. The nearby star <a href="/facts/55_Cancri/z00cuRxe">55 Cancri</a>, a system that is also known to contain five planets, also was reported to have a debris disk,<a class="footnote-ref" id="fnref:6" href="#fn:6"><sup>6</sup></a> but that detection could not be confirmed.<a class="footnote-ref" id="fnref:7" href="#fn:7"><sup>7</sup></a> Structures in the debris disk around <a href="/facts/Epsilon_Eridani/5LMmzaXl">Epsilon Eridani</a> suggest perturbations by a planetary body in orbit around that star, which may be used to constrain the mass and orbit of the planet.<a class="footnote-ref" id="fnref:8" href="#fn:8"><sup>8</sup></a> </p><p>On 24 April 2014, NASA reported detecting debris disks in archival images of several young stars, HD 141943 and HD 191089, first viewed between 1999 and 2006 with the <a href="/facts/Hubble_Space_Telescope/NQeIf0vw">Hubble Space Telescope</a>, by using newly improved imaging processes.<a class="footnote-ref" id="fnref:9" href="#fn:9"><sup>9</sup></a> </p><p>In 2021, observations of a star, VVV-WIT-08, that became obscured for a period of 200 days may have been the result of a debris disk passing between the star and observers on Earth.<a class="footnote-ref" id="fnref:10" href="#fn:10"><sup>10</sup></a> Two other stars, <a href="/facts/Epsilon_Aurigae/8X6QdQ2n">Epsilon Aurigae</a> and <a href="/facts/AS_Leonis_Minoris/0LSvSLTK">TYC 2505-672-1</a>, are reported to be eclipsed regularly and it has been determined that the phenomenon is the result of disks orbiting them in varied periods, suggesting that VVV-WIT-08 may be similar and have a much longer orbital period that just has been experienced by observers on Earth. VVV-WIT-08 is ten times the size of the Sun in the constellation of <a href="/facts/Sagittarius_(constellation)/ljtU4DQ2">Sagittarius</a>. </p> <h2 id="origin">Origin</h2> <p>During the formation of a Sun-like star, the object passes through the <a href="/facts/T_Tauri_star/vX5WL56u">T-Tauri</a> phase during which it is surrounded by a gas-rich, disk-shaped nebula. Out of this material are formed <a href="/facts/Planetesimal/PK60dofs">planetesimals</a>, which can continue accreting other planetesimals and disk material to form planets. The nebula continues to orbit the <a href="/facts/Pre-main-sequence_star/IKheFVse">pre-main-sequence star</a> for a period of 1–20 million years until it is cleared out by radiation pressure and other processes. Second generation dust may then be generated about the star by collisions between the planetesimals, which forms a disk out of the resulting debris. At some point during their lifetime, at least 45% of these stars are surrounded by a debris disk, which then can be detected by the thermal emission of the dust using an infrared telescope. Repeated collisions may cause a disk to persist for much of the lifetime of a star.<a class="footnote-ref" id="fnref:11" href="#fn:11"><sup>11</sup></a> </p><p>Typical debris disks contain small grains 1–100 <a href="/facts/Micrometre/7eDFxD2L">μm</a> in size. Collisions will grind down these grains to sub-micrometre sizes, which will be removed from the system by <a href="/facts/Radiation/RwMocyeq">radiation</a> pressure from the host <a href="/facts/Star/PFbd6ICx">star</a>. In very tenuous disks such as the ones in the Solar System, the <a href="/facts/Poynting%E2%80%93Robertson_effect/aAl6CMVw">Poynting–Robertson effect</a> can cause particles to <a href="/facts/Spiral/4R331aba">spiral</a> inward instead. Both processes limit the lifetime of the disk to 10 <a href="/facts/Myr/DXcnXuAw">Myr</a> or less. Thus, for a disk to remain intact, a process is needed to continually replenish the disk. This can occur, for example, by means of collisions between larger bodies, followed by a cascade that grinds down the objects to the observed small grains.<a class="footnote-ref" id="fnref:12" href="#fn:12"><sup>12</sup></a> </p><p>For collisions to occur in a debris disk, the bodies must be gravitationally <a href="/facts/Perturbation_(astronomy)/og5hPpjQ">perturbed</a> sufficiently to create relatively large collisional velocities. A planetary system around the star can cause such perturbations, as can a <a href="/facts/Binary_star/TYlDe1bD">binary star</a> companion or the close approach of another star.<a class="footnote-ref" id="fnref:13" href="#fn:13"><sup>13</sup></a> The presence of a debris disk may indicate a high likelihood of <a href="/facts/Exoplanet/zjfmqfUf">exoplanets</a> orbiting the star.<a class="footnote-ref" id="fnref:14" href="#fn:14"><sup>14</sup></a> Furthermore, many debris disks also show structures within the dust (for example, clumps and warps or asymmetries) that point to the presence of one or more exoplanets within the disk.<a class="footnote-ref" id="fnref:15" href="#fn:15"><sup>15</sup></a> The presence or absence of asymmetries in our own trans-Neptunian belt remains controversial although they might exist.<a class="footnote-ref" id="fnref:16" href="#fn:16"><sup>16</sup></a> </p> <h2 id="extreme-debris-disks">Extreme Debris disks</h2> <p class="note">See also: <a href="/facts/List_of_extrasolar_planetary_collisions/ouDrcdBQ">List of extrasolar planetary collisions</a></p> <p>A sub-type of debris disk is the so-called "extreme debris disk" (EDD). This type is defined as exceeding 1% of the luminosity of the star in the infrared. An EDD is surrounded by warm dust (200-600 <a href="/facts/Kelvin/E3trzC4C">Kelvin</a>), that orbits the star within a few astronomical units. In other words the dust is present in a region where <a href="/facts/Terrestrial_planet/jpMC1ULt">terrestrial planets</a> form. EDDs are rare and around 24 are known as of 2024. Infrared spectra with <a href="/facts/Spitzer_Space_Telescope/Ic1xXIYb">Spitzer</a> have shown that the dust is dominated by small particles made up of <a href="/facts/Silicate_mineral/WclrQW2I">silicates</a> that have a size between sub-μm and a few <a href="/facts/Micrometre/7eDFxD2L">μm</a>. EDDs are interpreted to have formed from one or more giant <a href="/facts/Impact_event/fbWu9Q4p">collisions</a> between large planetesimals or planetary bodies. This is different to most debris disks, which are sustained by smaller collisions.<a class="footnote-ref" id="fnref:17" href="#fn:17"><sup>17</sup></a> EDDs are often transient events, with the dust produced in the event lasting years around the star before <a href="/facts/Radiation_pressure/xA6japY0">radiation pressure</a> blows the small particles away. <a href="/facts/2MASS_J08090250-4858172/FU3rIB6l">2MASS J08090250-4858172</a> was one of the first such systems with observed infrared variability, showing two giant impact events in 2012 and 2014.<a class="footnote-ref" id="fnref:18" href="#fn:18"><sup>18</sup></a> In rare cases the dust cloud can orbit in front of the star, causing dips of brightness in the optical. One such system is <a href="/facts/HD_166191/pjTXEayr">HD 166191</a>, which shows a star-sized dust cloud <a href="/facts/Astronomical_transit/4s6Mll1a">transiting</a> in front of the star.<a class="footnote-ref" id="fnref:19" href="#fn:19"><sup>19</sup></a> Giant impacts are more common in young systems and after around 300 <a href="/facts/Million_years_ago/DXcnXuAw">Myrs</a> giant impacts become less common. A few relative old EDDs are also known, reaching up to 5.5 <a href="/facts/Billion_years_ago/5E7foypY">Gyrs</a>. These old EDDs often have a wide, eccentric companion, which might help trigger such giant impact events.<a class="footnote-ref" id="fnref:20" href="#fn:20"><sup>20</sup></a> Giant impacts might not always be detectable as EDDs. Such disks are made up of two types of dust. The first type is vapor condensates that is produced immediately in the event. The second type is dust created by the grinding down of <a href="/facts/Boulder/zIYnMJ1g">boulders</a> produced in the event. Simulations have shown that boulders are more important to classify disks as extreme.<a class="footnote-ref" id="fnref:21" href="#fn:21"><sup>21</sup></a> </p> <h2 id="known-belts">Known belts</h2> <p>Belts of dust or debris have been detected around many stars, including the Sun, including the following: </p> <table><tbody><tr><th>Star</th><th><a href="/facts/Spectral_class/dYrIuK9H">Spectralclass</a><a class="footnote-ref" id="fnref:22" href="#fn:22"><sup>22</sup></a></th><th>Distance(<a href="/facts/Light_Year/IGc5NdQb">ly</a>)</th><th>Orbit(<a href="/facts/Astronomical_Unit/gjsbu5xU">AU</a>)</th><th>Notes</th></tr><tr><td><a href="/facts/Epsilon_Eridani/5LMmzaXl">Epsilon Eridani</a></td><td>K2V</td><td>10.5</td><td>35–75</td><td><a class="footnote-ref" id="fnref:23" href="#fn:23"><sup>23</sup></a></td></tr><tr><td><a href="/facts/Tau_Ceti/1tzg8cmQ">Tau Ceti</a></td><td>G8V</td><td>11.9</td><td>35–50</td><td><a class="footnote-ref" id="fnref:24" href="#fn:24"><sup>24</sup></a></td></tr><tr><td><a href="/facts/Vega/G3wJwhhl">Vega</a></td><td>A0V</td><td>25</td><td>86–200</td><td><a class="footnote-ref" id="fnref:25" href="#fn:25"><sup>25</sup></a><a class="footnote-ref" id="fnref:26" href="#fn:26"><sup>26</sup></a></td></tr><tr><td><a href="/facts/Fomalhaut/eQ4LC29E">Fomalhaut</a></td><td>A3V</td><td>25</td><td>133–158</td><td><a class="footnote-ref" id="fnref:27" href="#fn:27"><sup>27</sup></a></td></tr><tr><td><a href="/facts/AU_Microscopii/IPkKMJgs">AU Microscopii</a></td><td>M1Ve</td><td>33</td><td>50–150</td><td><a class="footnote-ref" id="fnref:28" href="#fn:28"><sup>28</sup></a></td></tr><tr><td>HD 181327</td><td>F5.5V</td><td>51.8</td><td>89-110</td><td><a class="footnote-ref" id="fnref:29" href="#fn:29"><sup>29</sup></a></td></tr><tr><td><a href="/facts/HD_69830/QSY6k3a6">HD 69830</a></td><td>K0V</td><td>41</td><td><1</td><td><a class="footnote-ref" id="fnref:30" href="#fn:30"><sup>30</sup></a></td></tr><tr><td><a href="/facts/HD_207129/rmfY15jq">HD 207129</a></td><td>G0V</td><td>52</td><td>148–178</td><td><a class="footnote-ref" id="fnref:31" href="#fn:31"><sup>31</sup></a></td></tr><tr><td><a href="/facts/HD_139664/fhIsNIYs">HD 139664</a></td><td>F5IV–V</td><td>57</td><td>60–109</td><td><a class="footnote-ref" id="fnref:32" href="#fn:32"><sup>32</sup></a></td></tr><tr><td><a href="/facts/Eta_Corvi/yJnKtyvD">Eta Corvi</a></td><td>F2V</td><td>59</td><td>100–150</td><td><a class="footnote-ref" id="fnref:33" href="#fn:33"><sup>33</sup></a></td></tr><tr><td><a href="/facts/HD_53143/BqWIreUw">HD 53143</a></td><td>K1V</td><td>60</td><td>?</td><td><a class="footnote-ref" id="fnref:34" href="#fn:34"><sup>34</sup></a></td></tr><tr><td><a href="/facts/Beta_Pictoris/QyTtCCHu">Beta Pictoris</a></td><td>A6V</td><td>63</td><td>25–550</td><td><a class="footnote-ref" id="fnref:35" href="#fn:35"><sup>35</sup></a></td></tr><tr><td><a href="/facts/Zeta_Leporis/upWpBMuh">Zeta Leporis</a></td><td>A2Vann</td><td>70</td><td>2–8</td><td><a class="footnote-ref" id="fnref:36" href="#fn:36"><sup>36</sup></a></td></tr><tr><td><a href="/facts/HD_92945/8agEMETu">HD 92945</a></td><td>K1V</td><td>72</td><td>45–175</td><td><a class="footnote-ref" id="fnref:37" href="#fn:37"><sup>37</sup></a></td></tr><tr><td><a href="/facts/HD_107146/LufUxDjm">HD 107146</a></td><td>G2V</td><td>88</td><td>130</td><td><a class="footnote-ref" id="fnref:38" href="#fn:38"><sup>38</sup></a></td></tr><tr><td><a href="/facts/Gamma_Ophiuchi/zuzuLrXm">Gamma Ophiuchi</a></td><td>A0V</td><td>95</td><td>520</td><td><a class="footnote-ref" id="fnref:39" href="#fn:39"><sup>39</sup></a></td></tr><tr><td><a href="/facts/HR_8799/kFBfC1WL">HR 8799</a></td><td>A5V</td><td>129</td><td>75</td><td><a class="footnote-ref" id="fnref:40" href="#fn:40"><sup>40</sup></a></td></tr><tr><td><a href="/facts/51_Ophiuchi/rcmNrYFb">51 Ophiuchi</a></td><td>B9</td><td>131</td><td>0.5–1200</td><td><a class="footnote-ref" id="fnref:41" href="#fn:41"><sup>41</sup></a></td></tr><tr><td><a href="/facts/HD_12039/9eIe5Ndw">HD 12039</a></td><td>G3–5V</td><td>137</td><td>5</td><td><a class="footnote-ref" id="fnref:42" href="#fn:42"><sup>42</sup></a></td></tr><tr><td><a href="/facts/HD_98800/gAaVAp6m">HD 98800</a></td><td>K5e (?)</td><td>150</td><td>1</td><td><a class="footnote-ref" id="fnref:43" href="#fn:43"><sup>43</sup></a></td></tr><tr><td><a href="/facts/HD_15115/zN09s2zk">HD 15115</a></td><td>F2V</td><td>150</td><td>315–550</td><td><a class="footnote-ref" id="fnref:44" href="#fn:44"><sup>44</sup></a></td></tr><tr><td><a href="/facts/HR_4796/21jkHd4w">HR 4796</a> A</td><td>A0V</td><td>220</td><td>200</td><td><a class="footnote-ref" id="fnref:45" href="#fn:45"><sup>45</sup></a><a class="footnote-ref" id="fnref:46" href="#fn:46"><sup>46</sup></a></td></tr><tr><td><a href="/facts/HD_141569/8PGbkXe8">HD 141569</a></td><td>B9.5e</td><td>320</td><td>400</td><td><a class="footnote-ref" id="fnref:47" href="#fn:47"><sup>47</sup></a></td></tr><tr><td><a href="/facts/HD_113766/CSdUc0qI">HD 113766</a> A</td><td>F4V</td><td>430</td><td>0.35–5.8</td><td><a class="footnote-ref" id="fnref:48" href="#fn:48"><sup>48</sup></a></td></tr><tr><td>HD 141943</td><td></td><td></td><td></td><td><a class="footnote-ref" id="fnref:49" href="#fn:49"><sup>49</sup></a></td></tr><tr><td>HD 191089</td><td></td><td></td><td></td><td><a class="footnote-ref" id="fnref:50" href="#fn:50"><sup>50</sup></a></td></tr></tbody></table> <p>The orbital distance of the belt is an estimated mean distance or range, based either on direct measurement from imaging or derived from the temperature of the belt. The <a href="/facts/Earth/HLLmDfj0">Earth</a> has an average distance from the Sun of 1 AU. </p> <h2 id="see-also">See also</h2> <ul><li><a href="/facts/Accretion_disk/8zJXshat">Accretion disk</a></li> <li><a href="/facts/Asteroid_belt/YHAq2Eh3">Asteroid belt</a></li> <li><a href="/facts/Circumplanetary_disk/dpsq9bdV">Circumplanetary disk</a> – Accumulation of matter around a planet</li> <li>Exoasteroid belt</li> <li><a href="/facts/Protoplanetary_disk/FtfSbP61">Protoplanetary disk</a></li></ul> <h2 id="external-links">External links</h2> Wikimedia Commons has media related to Debris disks. <ul><li>McCabe, Caer (2019-03-08). <a href="http://www.circumstellardisks.org/">"Catalog of Resolved Circumstellar Disks"</a>. NASA JPL. Retrieved 2019-03-08.</li></ul> <h2 id="references">References</h2> <ol> <li id="fn:1"><p>Wang, Z.; Chakrabarty, D.; Kaplan, D. L. (2006). "A debris disk around an isolated young neutron star". Nature. 440 (7085): 772–775. arXiv:astro-ph/0604076. Bibcode:2006Natur.440..772W. doi:10.1038/nature04669. PMID 16598251. S2CID 4372235. <a href="/wiki/ArXiv_(identifier)" target="_blank">/wiki/ArXiv_(identifier)</a> <a href="#fnref:1" class="footnote-back-ref">↩</a></p></li> <li id="fn:2"><p>"Spitzer Sees Dusty Aftermath of Pluto-Sized Collision". NASA. 2005-01-10. Archived from the original on 2006-09-08. Retrieved 2007-01-03. <a href="https://web.archive.org/web/20060908075059/http://www.spitzer.caltech.edu/Media/happenings/20051214/" target="_blank">https://web.archive.org/web/20060908075059/http://www.spitzer.caltech.edu/Media/happenings/20051214/</a> <a href="#fnref:2" class="footnote-back-ref">↩</a></p></li> <li id="fn:3"><p>"Debris Disk Database". Royal Observatory Edinburgh. Archived from the original on 2008-08-10. Retrieved 2007-01-03. <a href="https://web.archive.org/web/20080810004849/http://www.roe.ac.uk/ukatc/research/topics/dust/identification.html" target="_blank">https://web.archive.org/web/20080810004849/http://www.roe.ac.uk/ukatc/research/topics/dust/identification.html</a> <a href="#fnref:3" class="footnote-back-ref">↩</a></p></li> <li id="fn:4"><p>Heap, S (2000). "Space Telescope Imaging Spectrograph Coronagraphic Observations of Beta Pictoris". The Astrophysical Journal. 539 (1): 435–444. arXiv:astro-ph/9911363. Bibcode:2000ApJ...539..435H. doi:10.1086/309188. <a href="https://doi.org/10.1086%2F309188" target="_blank">https://doi.org/10.1086%2F309188</a> <a href="#fnref:4" class="footnote-back-ref">↩</a></p></li> <li id="fn:5"><p>Lagrange, A-M (2012). "The position of Beta Pictoris b position relative to the debris disk". Astronomy & Astrophysics. 542: A40. arXiv:1202.2578. Bibcode:2012A&A...542A..40L. doi:10.1051/0004-6361/201118274. S2CID 118046185. <a href="https://www.aanda.org/articles/aa/abs/2012/06/aa18274-11/aa18274-11.html" target="_blank">https://www.aanda.org/articles/aa/abs/2012/06/aa18274-11/aa18274-11.html</a> <a href="#fnref:5" class="footnote-back-ref">↩</a></p></li> <li id="fn:6"><p>"University Of Arizona Scientists Are First To Discover Debris Disk Around Star Orbited By Planet". ScienceDaily. 1998-10-03. Retrieved 2006-05-24. <a href="https://www.sciencedaily.com/releases/1998/10/981023073211.htm" target="_blank">https://www.sciencedaily.com/releases/1998/10/981023073211.htm</a> <a href="#fnref:6" class="footnote-back-ref">↩</a></p></li> <li id="fn:7"><p>Schneider, G.; Becklin, E. E.; Smith, B. A.; Weinberger, A. J.; Silverstone, M.; Hines, D. C. (2001). "NICMOS Coronagraphic Observations of 55 Cancri". The Astronomical Journal. 121 (1): 525–537. arXiv:astro-ph/0010175. Bibcode:2001AJ....121..525S. doi:10.1086/318050. S2CID 14503540. <a href="/wiki/The_Astronomical_Journal" target="_blank">/wiki/The_Astronomical_Journal</a> <a href="#fnref:7" class="footnote-back-ref">↩</a></p></li> <li id="fn:8"><p>Greaves, J. S.; Holland, W. S.; Wyatt, M. C.; Dent, W. R. F.; Robson, E. I.; Coulson, I. M.; Jenness, T.; Moriarty-Schieven, G. H.; Davis, G. R.; Butner, H. M.; Gear, W. K.; Dominik, C.; Walker, H. J. (2005). "Structure in the Epsilon Eridani Debris Disk". The Astrophysical Journal. 619 (2): L187 – L190. Bibcode:2005ApJ...619L.187G. doi:10.1086/428348. <a href="https://doi.org/10.1086%2F428348" target="_blank">https://doi.org/10.1086%2F428348</a> <a href="#fnref:8" class="footnote-back-ref">↩</a></p></li> <li id="fn:9"><p>Harrington, J.D.; Villard, Ray (24 April 2014). "RELEASE 14-114 Astronomical Forensics Uncover Planetary Disks in NASA's Hubble Archive". NASA. Archived from the original on 2014-04-25. 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