Misplaced Pages

Debris disk

Article snapshot taken from Wikipedia with creative commons attribution-sharealike license. Give it a read and then ask your questions in the chat. We can research this topic together.
(Redirected from Debris disc) Disk of dust and debris in orbit around a star
Hubble Space Telescope observation of the debris ring around Fomalhaut. The inner edge of the disk may have been shaped by the orbit of Fomalhaut b, at lower right.

A debris disk (American English), or debris disc (Commonwealth English), is a circumstellar disk of dust and debris in orbit around a star. Sometimes these disks contain prominent rings, as seen in the image of Fomalhaut on the right. Debris disks are found around stars with mature planetary systems, including at least one debris disk in orbit around an evolved neutron star. Debris disks can also be produced and maintained as the remnants of collisions between planetesimals, otherwise known as asteroids and comets.

As of 2001, more than 900 candidate stars had been found to possess a debris disk. They are usually discovered by examining the star system in infrared light and looking for an excess of radiation beyond that emitted by the star. This excess is inferred to be radiation from the star that has been absorbed by the dust in the disk, then re-radiated away as infrared energy.

Debris disks are often described as massive analogs to the debris in the Solar System. Most known debris disks have radii of 10–100 astronomical units (AU); they resemble the Kuiper belt in the Solar System, although the Kuiper belt does not have a high enough dust mass to be detected around even the nearest stars. Some debris disks contain a component of warmer dust located within 10 AU from the central star. This dust is sometimes called exozodiacal dust by analogy to zodiacal dust in the Solar System.

Observation history

VLT and Hubble images of the disc around AU Microscopii.

In 1984 a debris disk was detected around the star Vega using the IRAS satellite. Initially this was believed to be a protoplanetary disk, 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": Vega, Beta Pictoris, Fomalhaut, and Epsilon Eridani. Subsequently, direct images of the Beta Pictoris disk showed irregularities in the dust, which were attributed to gravitational perturbations by an unseen exoplanet. That explanation was confirmed with the 2008 discovery of the exoplanet Beta Pictoris b.

Other exoplanet-hosting stars, including the first discovered by direct imaging (HR 8799), are known to also host debris disks. The nearby star 55 Cancri, a system that is also known to contain five planets, also was reported to have a debris disk, but that detection could not be confirmed. Structures in the debris disk around Epsilon Eridani suggest perturbations by a planetary body in orbit around that star, which may be used to constrain the mass and orbit of the planet.

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 Hubble Space Telescope, by using newly improved imaging processes.

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. Two other stars, Epsilon Aurigae and TYC 2505-672-1, 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 Sagittarius.

Origin

Debris disks detected in HST archival images of young stars, HD 141943 and HD 191089, using improved imaging processes (24 April 2014).

During the formation of a Sun-like star, the object passes through the T-Tauri phase during which it is surrounded by a gas-rich, disk-shaped nebula. Out of this material are formed planetesimals, which can continue accreting other planetesimals and disk material to form planets. The nebula continues to orbit the pre-main-sequence star 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.

Typical debris disks contain small grains 1–100 μm in size. Collisions will grind down these grains to sub-micrometre sizes, which will be removed from the system by radiation pressure from the host star. In very tenuous disks such as the ones in the Solar System, the Poynting–Robertson effect can cause particles to spiral inward instead. Both processes limit the lifetime of the disk to 10 Myr 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.

For collisions to occur in a debris disk, the bodies must be gravitationally perturbed sufficiently to create relatively large collisional velocities. A planetary system around the star can cause such perturbations, as can a binary star companion or the close approach of another star. The presence of a debris disk may indicate a high likelihood of exoplanets orbiting the star. 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. The presence or absence of asymmetries in our own trans-Neptunian belt remains controversial although they might exist.

Extreme Debris disks

See also: List of extrasolar planetary collisions

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 Kelvin), that orbits the star within a few astronomical units. In other words the dust is present in a region where terrestrial planets form. EDDs are rare and around 24 are known as of 2024. Infrared spectra with Spitzer have shown that the dust is dominated by small particles made up of silicates that have a size between sub-μm and a few μm. EDDs are interpreted to have formed from one or more giant collisions between large planetesimals or planetary bodies. This is different to most debris disks, which are sustained by smaller collisions. EDDs are often transient events, with the dust produced in the event lasting years around the star before radiation pressure blows the small particles away. 2MASS J08090250-4858172 was one of the first such systems with observed infrared variability, showing two giant impact events in 2012 and 2014. In rare cases the dust cloud can orbit in front of the star, causing dips of brightness in the optical. One such system is HD 166191, which shows a star-sized dust cloud transiting in front of the star. Giant impacts are more common in young systems and after around 300 Myrs giant impacts become less common. A few relative old EDDs are also known, reaching up to 5.5 Gyrs. These old EDDs often have a wide, eccentric companion, which might help trigger such giant impact events. 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 boulders produced in the event. Simulations have shown that boulders are more important to classify disks as extreme.

Known belts

Belts of dust or debris have been detected around many stars, including the Sun, including the following:

Star Spectral
class 		Distance
(ly) 		Orbit
(AU) 		Notes
Epsilon Eridani K2V 10.5 35–75
Tau Ceti G8V 11.9 35–50
Vega A0V 25 86–200
Fomalhaut A3V 25 133–158
AU Microscopii M1Ve 33 50–150
HD 181327 F5.5V 51.8 89-110
HD 69830 K0V 41 <1
HD 207129 G0V 52 148–178
HD 139664 F5IV–V 57 60–109
Eta Corvi F2V 59 100–150
HD 53143 K1V 60 ?
Beta Pictoris A6V 63 25–550
Zeta Leporis A2Vann 70 2–8
HD 92945 K1V 72 45–175
HD 107146 G2V 88 130
Gamma Ophiuchi A0V 95 520
HR 8799 A5V 129 75
51 Ophiuchi B9 131 0.5–1200
HD 12039 G3–5V 137 5
HD 98800 K5e (?) 150 1
HD 15115 F2V 150 315–550
HR 4796 A A0V 220 200
HD 141569 B9.5e 320 400
HD 113766 A F4V 430 0.35–5.8
HD 141943
HD 191089

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 Earth has an average distance from the Sun of 1 AU.

See also

References

  1. 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.
  2. "Spitzer Sees Dusty Aftermath of Pluto-Sized Collision". NASA. 2005-01-10. Archived from the original on 2006-09-08. Retrieved 2007-01-03.
  3. "Debris Disk Database". Royal Observatory Edinburgh. Archived from the original on 2008-08-10. Retrieved 2007-01-03.
  4. "Mysterious Ripples Found Racing Through Planet-forming Disc". Retrieved 8 October 2015.
  5. 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.
  6. ^ 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.
  7. "University Of Arizona Scientists Are First To Discover Debris Disk Around Star Orbited By Planet". ScienceDaily. 1998-10-03. Retrieved 2006-05-24.
  8. 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.
  9. ^ 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.
  10. ^ 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. Retrieved 2014-04-25.
  11. Carpineti, Alfredo, Giant Star Obscured By Mysterious "Dark, Large, Elongated" Object Spotted By Astronomers, IFL Science, June 11, 2021
  12. Thomas, Paul J. (2006). Comets and the origin and evolution of life. Advances in astrobiology and biogeophysics (2nd ed.). Springer. p. 104. ISBN 3-540-33086-0.
  13. ^ Kenyon, Scott; Bromley, Benjamin (2007). "Stellar Flybys & Planetary Debris Disks". Smithsonian Astrophysical Observatory. Retrieved 2007-07-23.
  14. Raymond, Sean N.; Armitage, P. J.; et al. (2011). "Debris disks as signposts of terrestrial planet formation". Astronomy & Astrophysics. 530: A62. arXiv:1104.0007. Bibcode:2011A&A...530A..62R. doi:10.1051/0004-6361/201116456. S2CID 119220262.
  15. de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 May 2022). "Twisted extreme trans-Neptunian orbital parameter space: statistically significant asymmetries confirmed". Monthly Notices of the Royal Astronomical Society Letters. 512 (1): L6 – L10. arXiv:2202.01693. Bibcode:2022MNRAS.512L...6D. doi:10.1093/mnrasl/slac012.
  16. ^ Moór, Attila; Ábrahám, Péter; Su, Kate Y. L.; Henning, Thomas; Marino, Sebastian; Chen, Lei; Kóspál, Ágnes; Pawellek, Nicole; Varga, József; Vida, Krisztián (2024-03-01). "Abundant sub-micron grains revealed in newly discovered extreme debris discs". Monthly Notices of the Royal Astronomical Society. 528 (3): 4528–4546. arXiv:2402.15438. Bibcode:2024MNRAS.528.4528M. doi:10.1093/mnras/stae155. ISSN 0035-8711.
  17. Su, Kate Y. L.; Jackson, Alan P.; Gáspár, András; Rieke, George H.; Dong, Ruobing; Olofsson, Johan; Kennedy, G. M.; Leinhardt, Zoë M.; Malhotra, Renu; Hammer, Michael; Meng, Huan Y. A.; Rujopakarn, W.; Rodriguez, Joseph E.; Pepper, Joshua; Reichart, D. E. (2019-05-01). "Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation". The Astronomical Journal. 157 (5): 202. arXiv:1903.10627. Bibcode:2019AJ....157..202S. doi:10.3847/1538-3881/ab1260. ISSN 0004-6256.
  18. Su, Kate Y. L.; Kennedy, Grant M.; Schlawin, Everett; Jackson, Alan P.; Rieke, G. H. (2022-03-01). "A Star-sized Impact-produced Dust Clump in the Terrestrial Zone of the HD 166191 System". The Astrophysical Journal. 927 (2): 135. arXiv:2203.02366. Bibcode:2022ApJ...927..135S. doi:10.3847/1538-4357/ac4bbb. ISSN 0004-637X.
  19. Watt, Lewis; Leinhardt, Zoe; Su, Kate Y. L. (2021-04-01). "Planetary embryo collisions and the wiggly nature of extreme debris discs". Monthly Notices of the Royal Astronomical Society. 502 (2): 2984–3002. arXiv:2101.05106. Bibcode:2021MNRAS.502.2984W. doi:10.1093/mnras/stab106. ISSN 0035-8711.
  20. "SIMBAD: Query by identifiers". Centre de Données astronomiques de Strasbourg. Retrieved 2007-07-17.
  21. Greaves, J. S.; Wyatt, M. C.; Holland, W. S.; Dent, W. R. F. (2004). "The debris disc around tau Ceti: a massive analogue to the Kuiper Belt". Monthly Notices of the Royal Astronomical Society. 351 (3): L54 – L58. Bibcode:2004MNRAS.351L..54G. doi:10.1111/j.1365-2966.2004.07957.x.
  22. ^ "Astronomers discover possible new Solar Systems in formation around the nearby stars Vega and Fomalhaut" (Press release). Joint Astronomy Centre. 1998-04-21. Archived from the original on 2008-12-16. Retrieved 2006-04-24.
  23. ^ Backman, D. E. (1996). "Dust in beta PIC / VEGA Main Sequence Systems". Bulletin of the American Astronomical Society. 28: 1056. Bibcode:1996DPS....28.0122B.
  24. Sanders, Robert (2007-01-08). "Dust around nearby star like powder snow". UC Berkeley News. Retrieved 2007-01-11.
  25. Lebreton, J.; Augereau, J.-C.; Thi, W.-F.; Roberge, A.; et al. (2012). "An icy Kuiper belt around the young solar-type star HD 181327". Astronomy & Astrophysics. 539 (1): A17. arXiv:1112.3398. Bibcode:2012A&A...539A..17L. doi:10.1051/0004-6361/201117714. S2CID 12704582.
  26. Lisse, C. M.; Beichman, C. A.; Bryden, G.; Wyatt, M. C. (2007). "On the Nature of the Dust in the Debris Disk around HD 69830". The Astrophysical Journal. 658 (1): 584–592. arXiv:astro-ph/0611452. Bibcode:2007ApJ...658..584L. doi:10.1086/511001. S2CID 53460002.
  27. Krist, John E.; Stapelfeldt, Karl R.; et al. (October 2010). "HST and Spitzer Observations of the HD 207129 Debris Ring". The Astronomical Journal. 140 (4): 1051–1061. arXiv:1008.2793. Bibcode:2010AJ....140.1051K. doi:10.1088/0004-6256/140/4/1051. S2CID 43979052.
  28. ^ Kalas, Paul; Graham, James R.; Clampin, Mark C.; Fitzgerald, Michael P. (2006). "First Scattered Light Images of Debris Disks around HD 53143 and HD 139664". The Astrophysical Journal. 637 (1): L57 – L60. arXiv:astro-ph/0601488. Bibcode:2006ApJ...637L..57K. doi:10.1086/500305. S2CID 18293244.
  29. Wyatt, M. C.; Greaves, J. S.; Dent, W. R. F.; Coulson, I. M. (2005). "Submillimeter Images of a Dusty Kuiper Belt around Corvi". The Astrophysical Journal. 620 (1): 492–500. arXiv:astro-ph/0411061. Bibcode:2005ApJ...620..492W. doi:10.1086/426929. S2CID 14107485.
  30. Moerchen, M. M.; Telesco, C. M.; Packham, C.; Kehoe, T. J. J. (2006). "Mid-infrared resolution of a 3 AU-radius debris disk around Zeta Leporis". Astrophysical Journal Letters. 655 (2): L109. arXiv:astro-ph/0612550. Bibcode:2007ApJ...655L.109M. doi:10.1086/511955. S2CID 18073836.
  31. Golimowski, D.; et al. (2007). "Observations and Models of the Debris Disk around K Dwarf HD 92945" (PDF). University of California, Berkeley Astronomy Department. Retrieved 2007-07-17.
  32. Williams, Jonathan P., et al. (2004). "Detection of cool dust around the G2V star HD 107146". Astrophysical Journal. 604 (1): 414–419. arXiv:astro-ph/0311583. Bibcode:2004ApJ...604..414W. doi:10.1086/381721. S2CID 18799183.
  33. SU, K.Y.L.; et al. (2008). "The exceptionally large debris disk around γ Ophiuchi". Astrophysical Journal. 679 (2): L125 – L129. arXiv:0804.2924. Bibcode:2008ApJ...679L.125S. doi:10.1086/589508. S2CID 9634091.
  34. Marois, Christian; MacIntosh, B.; et al. (November 2008). "Direct Imaging of Multiple Planets Orbiting the Star HR 8799". Science. 322 (5906): 1348–52. arXiv:0811.2606. Bibcode:2008Sci...322.1348M. doi:10.1126/science.1166585. PMID 19008415. S2CID 206516630. (Preprint at exoplanet.eu Archived 2008-12-17 at the Wayback Machine)
  35. Stark, C.; et al. (2009). "51 Ophiuchus: A Possible Beta Pictoris Analog Measured with the Keck Interferometer Nuller". Astrophysical Journal. 703 (2): 1188–1197. arXiv:0909.1821. Bibcode:2009ApJ...703.1188S. doi:10.1088/0004-637X/703/2/1188. S2CID 17938884.
  36. Hines, Dean C., et al. (2006). "The Formation and Evolution of Planetary Systems (FEPS): Discovery of an Unusual Debris System Associated with HD 12039". The Astrophysical Journal. 638 (2): 1070–1079. arXiv:astro-ph/0510294. Bibcode:2006ApJ...638.1070H. doi:10.1086/498929. S2CID 14919914.
  37. Furlan, Elise; Sargent; Calvet; Forrest; D'Alessio; Hartmann; Watson; Green; et al. (2007-05-02). "HD 98800: A 10-Myr-Old Transition Disk". The Astrophysical Journal. 664 (2): 1176–1184. arXiv:0705.0380. Bibcode:2007ApJ...664.1176F. doi:10.1086/519301. S2CID 14027663.
  38. Kalas, Paul; Fitzgerald, Michael P.; Graham, James R. (2007). "Discovery of Extreme Asymmetry in the Debris Disk Surrounding HD 15115". The Astrophysical Journal. 661 (1): L85 – L88. arXiv:0704.0645. Bibcode:2007ApJ...661L..85K. doi:10.1086/518652. S2CID 16599464.
  39. Koerner, D. W.; Ressler, M. E.; Werner, M. W.; Backman, D. E. (1998). "Mid-Infrared Imaging of a Circumstellar Disk around HR 4796: Mapping the Debris of Planetary Formation". Astrophysical Journal Letters. 503 (1): L83. arXiv:astro-ph/9806268. Bibcode:1998ApJ...503L..83K. doi:10.1086/311525. S2CID 12715138.
  40. ^ Villard, Ray; Weinberger, Alycia; Smith, Brad (1999-01-08). "Hubble Views of Dust Disks and Rings Surrounding Young Stars Yield Clues". HubbleSite. Retrieved 2007-06-17.
  41. Meyer, M. R.; Backman, D. (2002-01-08). "Belt of Material Around Star May Be First Step in Terrestrial Planet Formation". University of Arizona, NASA. Archived from the original on 2011-06-07. Retrieved 2007-07-17.

External links

Category: