Astronomy:Oort cloud

From HandWiki
Short description: Distant planetesimals in the Solar System
The distance from the Oort cloud to the interior of the Solar System, and two of the nearest stars, is measured in astronomical units. The scale is logarithmic: each indicated distance is ten times farther out than the previous distance. The red arrow indicates the location of the space probe Voyager 1 by 2012-2013, which will reach the Oort cloud in about 300 years.
An artist's impression of the Oort cloud and the Kuiper belt (inset); the sizes of objects are over-scaled for visibility.

The Oort cloud (/ɔːrt, ʊərt/),[1] sometimes called the Öpik–Oort cloud,[2] is a theoretical[3] concept of a cloud of predominantly icy planetesimals proposed to surround the Sun at distances ranging from 2,000 to 200,000 AU (0.03 to 3.2 light-years).[note 1][4] It is first described in 1950 by the Dutch astronomer Jan Oort.[5] It is divided into two regions: a disc-shaped inner Oort cloud (or Hills cloud) and a spherical outer Oort cloud. Both regions lie beyond the heliosphere and are in interstellar space.[4][6] The Kuiper belt, the scattered disc and the detached objects, the other three reservoirs of trans-Neptunian objects, are less than one thousandth as far from the Sun as the Oort cloud.

The outer limit of the Oort cloud defines the cosmographic boundary of the Solar System and the extent of the Sun's Hill sphere.[7] The outer Oort cloud is only loosely bound to the Solar System, and thus is easily affected by the gravitational pull both of passing stars and of the Milky Way itself. These forces occasionally dislodge comets from their orbits within the cloud and send them toward the inner Solar System.[4] Based on their orbits, most of the short-period comets may come from the scattered disc, but some short-period comets may have originated from the Oort cloud.[4][8]

Astronomers conjecture that the matter composing the Oort cloud formed closer to the Sun and was scattered far into space by the gravitational effects of the giant planets early in the Solar System's evolution.[4] Although no confirmed direct observations of the Oort cloud have been made, it may be the source that replenishes most long-period and Halley-type comets entering the inner Solar System, and many of the centaurs and Jupiter-family comets as well.[8]


There are two main classes of comet: short-period comets (also called ecliptic comets) and long-period comets (also called nearly isotropic comets). Ecliptic comets have relatively small orbits, below 10 au, and follow the ecliptic plane, the same plane in which the planets lie. All long-period comets have very large orbits, on the order of thousands of au, and appear from every direction in the sky.[9]

A. O. Leuschner in 1907 suggested that many comets believed to have parabolic orbits, and thus making single visits to the solar system, actually had elliptical orbits and would return after very long periods.[10] In 1932 Estonian astronomer Ernst Öpik postulated that long-period comets originated in an orbiting cloud at the outermost edge of the Solar System.[11] Dutch astronomer Jan Oort independently revived the idea in 1950 as a means to resolve a paradox:[12]

  • Over the course of the Solar System's existence the orbits of comets are unstable, and eventually dynamics dictate that a comet must either collide with the Sun or a planet or be ejected from the Solar System by planetary perturbations.
  • Moreover, their volatile composition means that as they repeatedly approach the Sun, radiation gradually boils the volatiles off until the comet splits or develops an insulating crust that prevents further outgassing.

Thus, Oort reasoned, a comet could not have formed while in its current orbit and must have been held in an outer reservoir for almost all of its existence.[12][13][9] He noted that there was a peak in numbers of long-period comets with aphelia (their farthest distance from the Sun) of roughly 20,000 au, which suggested a reservoir at that distance with a spherical, isotropic distribution. Those relatively rare comets with orbits of about 10,000 au have probably gone through one or more orbits through the Solar System and have had their orbits drawn inward by the gravity of the planets.[9]

Structure and composition

The presumed distance of the Oort cloud compared to the rest of the Solar System

The Oort cloud is thought to occupy a vast space from somewhere between 2,000 and 5,000 au (0.03 and 0.08 ly)[9] to as far as 50,000 au (0.79 ly)[4] from the Sun. Some estimates place the outer boundary at between 100,000 and 200,000 au (1.58 and 3.16 ly).[9] The region can be subdivided into a spherical outer Oort cloud of 20,000–50,000 au (0.32–0.79 ly), and a torus-shaped inner Oort cloud of 2,000–20,000 au (0.03–0.32 ly). The outer cloud is only weakly bound to the Sun and supplies the long-period (and possibly Halley-type) comets to inside the orbit of Neptune.[4] The inner Oort cloud is also known as the Hills cloud, named after Jack G. Hills, who proposed its existence in 1981.[14] Models predict that the inner cloud should have tens or hundreds of times as many cometary nuclei as the outer halo;[14][15][16] it is seen as a possible source of new comets to resupply the tenuous outer cloud as the latter's numbers are gradually depleted. The Hills cloud explains the continued existence of the Oort cloud after billions of years.[17]

The outer Oort cloud may have trillions of objects larger than 1 km (0.62 mi),[4] and billions with absolute magnitudes[18] brighter than 11 (corresponding to approximately 20-kilometre (12 mi) diameter), with neighboring objects tens of millions of kilometres apart.[8][19] Its total mass is not known, but, assuming that Halley's Comet is a suitable prototype for comets within the outer Oort cloud, roughly the combined mass is 3×1025 kilograms (6.6×1025 lb), or five times that of Earth.[4][20] Earlier it was thought to be more massive (up to 380 Earth masses),[21] but improved knowledge of the size distribution of long-period comets led to lower estimates. No known estimates of the mass of the inner Oort cloud have been published.

If analyses of comets are representative of the whole, the vast majority of Oort-cloud objects consist of ices such as water, methane, ethane, carbon monoxide and hydrogen cyanide.[22] However, the discovery of the object 1996 PW, an object whose appearance was consistent with a D-type asteroid[23][24] in an orbit typical of a long-period comet, prompted theoretical research that suggests that the Oort cloud population consists of roughly one to two percent asteroids.[25] Analysis of the carbon and nitrogen isotope ratios in both the long-period and Jupiter-family comets shows little difference between the two, despite their presumably vastly separate regions of origin. This suggests that both originated from the original protosolar cloud,[26] a conclusion also supported by studies of granular size in Oort-cloud comets[27] and by the recent impact study of Jupiter-family comet Tempel 1.[28]


The Oort cloud is thought to have developed after the formation of planets from the primordial protoplanetary disc approximately 4.6 billion years ago.[4] The most widely accepted hypothesis is that the Oort cloud's objects initially coalesced much closer to the Sun as part of the same process that formed the planets and minor planets. After formation, strong gravitational interactions with young gas giants, such as Jupiter, scattered the objects into extremely wide elliptical or parabolic orbits that were subsequently modified by perturbations from passing stars and giant molecular clouds into long-lived orbits detached from the gas giant region.[4][29]

Recent research has been cited by NASA hypothesizing that a large number of Oort cloud objects are the product of an exchange of materials between the Sun and its sibling stars as they formed and drifted apart and it is suggested that many—possibly the majority—of Oort cloud objects did not form in close proximity to the Sun.[30] Simulations of the evolution of the Oort cloud from the beginnings of the Solar System to the present suggest that the cloud's mass peaked around 800 million years after formation, as the pace of accretion and collision slowed and depletion began to overtake supply.[4]

Models by Julio Ángel Fernández suggest that the scattered disc, which is the main source for periodic comets in the Solar System, might also be the primary source for Oort cloud objects. According to the models, about half of the objects scattered travel outward toward the Oort cloud, whereas a quarter are shifted inward to Jupiter's orbit, and a quarter are ejected on hyperbolic orbits. The scattered disc might still be supplying the Oort cloud with material.[31] A third of the scattered disc's population is likely to end up in the Oort cloud after 2.5 billion years.[32]

Computer models suggest that collisions of cometary debris during the formation period play a far greater role than was previously thought. According to these models, the number of collisions early in the Solar System's history was so great that most comets were destroyed before they reached the Oort cloud. Therefore, the current cumulative mass of the Oort cloud is far less than was once suspected.[33] The estimated mass of the cloud is only a small part of the 50–100 Earth masses of ejected material.[4]

Gravitational interaction with nearby stars and galactic tides modified cometary orbits to make them more circular. This explains the nearly spherical shape of the outer Oort cloud.[4] On the other hand, the Hills cloud, which is bound more strongly to the Sun, has not acquired a spherical shape. Recent studies have shown that the formation of the Oort cloud is broadly compatible with the hypothesis that the Solar System formed as part of an embedded cluster of 200–400 stars. These early stars likely played a role in the cloud's formation, since the number of close stellar passages within the cluster was much higher than today, leading to far more frequent perturbations.[34]

In June 2010 Harold F. Levison and others suggested on the basis of enhanced computer simulations that the Sun "captured comets from other stars while it was in its birth cluster." Their results imply that "a substantial fraction of the Oort cloud comets, perhaps exceeding 90%, are from the protoplanetary discs of other stars."[35][36] In July 2020 Amir Siraj and Avi Loeb found that a captured origin for the Oort Cloud in the Sun's birth cluster could address the theoretical tension in explaining the observed ratio of outer Oort cloud to scattered disc objects, and in addition could increase the chances of a captured Planet Nine.[37][38][39]


Comets are thought to have two separate points of origin in the Solar System. Short-period comets (those with orbits of up to 200 years) are generally accepted to have emerged from either the Kuiper belt or the scattered disc, which are two linked flat discs of icy debris beyond Neptune's orbit at 30 au and jointly extending out beyond 100 au from the Sun. Very long-period comets, such as C/1999 F1 (Catalina), whose orbits last for millions of years, are thought to originate directly from the outer Oort cloud.[40] Other comets modeled to have come directly from the outer Oort cloud include C/2006 P1 (McNaught), C/2010 X1 (Elenin), Comet ISON, C/2013 A1 (Siding Spring), C/2017 K2, and C/2017 T2 (PANSTARRS). The orbits within the Kuiper belt are relatively stable, and so very few comets are thought to originate there. The scattered disc, however, is dynamically active, and is far more likely to be the place of origin for comets.[9] Comets pass from the scattered disc into the realm of the outer planets, becoming what are known as centaurs.[41] These centaurs are then sent farther inward to become the short-period comets.[42]

There are two main varieties of short-period comet: Jupiter-family comets (those with semi-major axes of less than 5 AU) and Halley-family comets. Halley-family comets, named for their prototype, Halley's Comet, are unusual in that although they are short-period comets, it is hypothesized that their ultimate origin lies in the Oort cloud, not in the scattered disc. Based on their orbits, it is suggested they were long-period comets that were captured by the gravity of the giant planets and sent into the inner Solar System.[13] This process may have also created the present orbits of a significant fraction of the Jupiter-family comets, although the majority of such comets are thought to have originated in the scattered disc.[8]

Oort noted that the number of returning comets was far less than his model predicted, and this issue, known as "cometary fading", has yet to be resolved. No dynamical process is known to explain the smaller number of observed comets than Oort estimated. Hypotheses for this discrepancy include the destruction of comets due to tidal stresses, impact or heating; the loss of all volatiles, rendering some comets invisible, or the formation of a non-volatile crust on the surface.[43] Dynamical studies of hypothetical Oort cloud comets have estimated that their occurrence in the outer-planet region would be several times higher than in the inner-planet region. This discrepancy may be due to the gravitational attraction of Jupiter, which acts as a kind of barrier, trapping incoming comets and causing them to collide with it, just as it did with Comet Shoemaker–Levy 9 in 1994.[44] An example of a typical dynamically old comet with an origin in the Oort cloud could be C/2018 F4.[45]

Tidal effects

Main page: Astronomy:Galactic tide

Most of the comets seen close to the Sun seem to have reached their current positions through gravitational perturbation of the Oort cloud by the tidal force exerted by the Milky Way. Just as the Moon's tidal force deforms Earth's oceans, causing the tides to rise and fall, the galactic tide also distorts the orbits of bodies in the outer Solar System. In the charted regions of the Solar System, these effects are negligible compared to the gravity of the Sun, but in the outer reaches of the system, the Sun's gravity is weaker and the gradient of the Milky Way's gravitational field has substantial effects. Galactic tidal forces stretch the cloud along an axis directed toward the galactic center and compress it along the other two axes; these small perturbations can shift orbits in the Oort cloud to bring objects close to the Sun.[46] The point at which the Sun's gravity concedes its influence to the galactic tide is called the tidal truncation radius. It lies at a radius of 100,000 to 200,000 au, and marks the outer boundary of the Oort cloud.[9]

Some scholars theorize that the galactic tide may have contributed to the formation of the Oort cloud by increasing the perihelia (smallest distances to the Sun) of planetesimals with large aphelia (largest distances to the Sun).[47] The effects of the galactic tide are quite complex, and depend heavily on the behaviour of individual objects within a planetary system. Cumulatively, however, the effect can be quite significant: up to 90% of all comets originating from the Oort cloud may be the result of the galactic tide.[48] Statistical models of the observed orbits of long-period comets argue that the galactic tide is the principal means by which their orbits are perturbed toward the inner Solar System.[49]

Stellar perturbations and stellar companion hypotheses

Besides the galactic tide, the main trigger for sending comets into the inner Solar System is thought to be interaction between the Sun's Oort cloud and the gravitational fields of nearby stars[4] or giant molecular clouds.[44] The orbit of the Sun through the plane of the Milky Way sometimes brings it in relatively close proximity to other stellar systems. For example, it is hypothesized that 70 thousand years ago, perhaps Scholz's Star passed through the outer Oort cloud (although its low mass and high relative velocity limited its effect).[50] During the next 10 million years the known star with the greatest possibility of perturbing the Oort cloud is Gliese 710.[51] This process could also scatter Oort cloud objects out of the ecliptic plane, potentially also explaining its spherical distribution.[51][52]

In 1984, physicist Richard A. Muller postulated that the Sun has an as-yet undetected companion, either a brown dwarf or a red dwarf, in an elliptical orbit within the Oort cloud. This object, known as Nemesis, was hypothesized to pass through a portion of the Oort cloud approximately every 26 million years, bombarding the inner Solar System with comets. However, to date no evidence of Nemesis has been found, and many lines of evidence (such as crater counts), have thrown its existence into doubt.[53][54] Recent scientific analysis no longer supports the idea that extinctions on Earth happen at regular, repeating intervals.[55] Thus, the Nemesis hypothesis is no longer needed to explain current assumptions.[55]

A somewhat similar hypothesis was advanced by astronomer John J. Matese of the University of Louisiana at Lafayette in 2002. He contends that more comets are arriving in the inner Solar System from a particular region of the postulated Oort cloud than can be explained by the galactic tide or stellar perturbations alone, and that the most likely cause would be a Jupiter-mass object in a distant orbit.[56] This hypothetical gas giant was nicknamed Tyche. The WISE mission, an all-sky survey using parallax measurements in order to clarify local star distances, was capable of proving or disproving the Tyche hypothesis.[55] In 2014, NASA announced that the WISE survey had ruled out any object as they had defined it.[57]

Future exploration

Artist's impression of the TAU spacecraft

In the 1980s, there was a concept for a probe that could reach 1,000 AU in 50 years, called TAU; among its missions would be to look for the Oort cloud.[58]

In the 2014 Announcement of Opportunity for the Discovery program, an observatory to detect the objects in the Oort cloud (and Kuiper belt) called the "Whipple Mission" was proposed.[59] It would monitor distant stars with a photometer, looking for transits up to 10,000 AU away.[59] The observatory was proposed for halo orbiting around L2 with a suggested 5-year mission.[59] It was also suggested that the Kepler observatory could have been capable of detecting objects in the Oort cloud.[60]

See also


  1. Oort (3rd ed.), Oxford University Press, September 2005,  (Subscription or UK public library membership required.)
  2. "A Review of Cometary Sciences". Philosophical Transactions of the Royal Society A 323 (1572): 339–347 [341]. 1987-09-30. doi:10.1098/rsta.1987.0090. Bibcode1987RSPTA.323..339W. 
  3. Williams, Matt (August 10, 2015). "What is the Oort Cloud?". 
  4. 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 4.13 4.14 Alessandro Morbidelli (2006). "Origin and dynamical evolution of comets and their reservoirs of water ammonia and methane". arXiv:astro-ph/0512256.
  5. Redd, Nola Taylor (October 4, 2018). "Oort Cloud: The Outer Solar System's Icy Shell". 
  6. Cite error: Invalid <ref> tag; no text was provided for refs named jpl.PIA17046
  7. "Kuiper Belt & Oort Cloud". NASA Solar System Exploration web site. NASA. 
  8. 8.0 8.1 8.2 8.3 V. V. Emelyanenko; D. J. Asher; M. E. Bailey (2007). "The fundamental role of the Oort Cloud in determining the flux of comets through the planetary system". Monthly Notices of the Royal Astronomical Society 381 (2): 779–789. doi:10.1111/j.1365-2966.2007.12269.x. Bibcode2007MNRAS.381..779E. 
  9. 9.0 9.1 9.2 9.3 9.4 9.5 9.6 Harold F. Levison; Luke Donnes (2007). "Comet Populations and Cometary Dynamics". in Lucy Ann Adams McFadden. Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 575–588. ISBN 978-0-12-088589-3. 
  10. Ley, Willy (April 1967). "The Orbits of the Comets". Galaxy Science Fiction 25 (4): 55–63. 
  11. Ernst Julius Öpik (1932). "Note on Stellar Perturbations of Nearby Parabolic Orbits". Proceedings of the American Academy of Arts and Sciences 67 (6): 169–182. doi:10.2307/20022899. Bibcode1932PAAAS..67..169O. 
  12. 12.0 12.1 Jan Oort (1950). "The structure of the cloud of comets surrounding the Solar System and a hypothesis concerning its origin". Bulletin of the Astronomical Institutes of the Netherlands 11: 91–110. Bibcode1950BAN....11...91O. 
  13. 13.0 13.1 David C. Jewitt (2001). "From Kuiper Belt to Cometary Nucleus: The Missing Ultrared Matter". Astronomical Journal 123 (2): 1039–1049. doi:10.1086/338692. Bibcode2002AJ....123.1039J. 
  14. 14.0 14.1 Jack G. Hills (1981). "Comet showers and the steady-state infall of comets from the Oort Cloud". Astronomical Journal 86: 1730–1740. doi:10.1086/113058. Bibcode1981AJ.....86.1730H. 
  15. Harold F. Levison; Luke Dones; Martin J. Duncan (2001). "The Origin of Halley-Type Comets: Probing the Inner Oort Cloud". Astronomical Journal 121 (4): 2253–2267. doi:10.1086/319943. Bibcode2001AJ....121.2253L. 
  16. Thomas M. Donahue, ed (1991). Planetary Sciences: American and Soviet Research, Proceedings from the U.S.–U.S.S.R. Workshop on Planetary Sciences. Kathleen Kearney Trivers, and David M. Abramson. National Academy Press. p. 251. doi:10.17226/1790. ISBN 978-0-309-04333-5. Retrieved 2008-03-18. 
  17. Julio A. Fernández (1997). "The Formation of the Oort Cloud and the Primitive Galactic Environment". Icarus 219 (1): 106–119. doi:10.1006/icar.1997.5754. Bibcode1997Icar..129..106F. Retrieved 2008-03-18. 
  18. Absolute magnitude is a measure of how bright an object would be if it were 1 au from the Sun and Earth; as opposed to apparent magnitude, which measures how bright an object appears from Earth. Because all measurements of absolute magnitude assume the same distance, absolute magnitude is in effect a measurement of an object's brightness. The lower an object's absolute magnitude, the brighter it is.
  19. Paul R. Weissman (1998). "The Oort Cloud". Scientific American. 
  20. Paul R. Weissman (1983). "The mass of the Oort Cloud". Astronomy and Astrophysics 118 (1): 90–94. Bibcode1983A&A...118...90W. 
  21. Sebastian Buhai. "On the Origin of the Long Period Comets: Competing theories". Utrecht University College. 
  22. E. L. Gibb; M. J. Mumma; N. Dello Russo; M. A. DiSanti; K. Magee-Sauer (2003). "Methane in Oort Cloud comets". Icarus 165 (2): 391–406. doi:10.1016/S0019-1035(03)00201-X. Bibcode2003Icar..165..391G. 
  23. Rabinowitz, D. L. (August 1996). "1996 PW". IAU Circular 6466: 2. Bibcode1996IAUC.6466....2R. 
  24. Davies, John K.; McBride, Neil; Green, Simon F.; Mottola, Stefano et al. (April 1998). "The Lightcurve and Colors of Unusual Minor Planet 1996 PW". Icarus 132 (2): 418–430. doi:10.1006/icar.1998.5888. Bibcode1998Icar..132..418D. 
  25. Paul R. Weissman; Harold F. Levison (1997). "Origin and Evolution of the Unusual Object 1996 PW: Asteroids from the Oort Cloud?". Astrophysical Journal 488 (2): L133–L136. doi:10.1086/310940. Bibcode1997ApJ...488L.133W. 
  26. D. Hutsemekers; J. Manfroid; E. Jehin; C. Arpigny; A. Cochran; R. Schulz; J.A. Stüwe; J.M. Zucconi (2005). "Isotopic abundances of carbon and nitrogen in Jupiter-family and Oort Cloud comets". Astronomy and Astrophysics 440 (2): L21–L24. doi:10.1051/0004-6361:200500160. Bibcode2005A&A...440L..21H. 
  27. Takafumi Ootsubo; Jun-ichi Watanabe; Hideyo Kawakita; Mitsuhiko Honda; Reiko Furusho (2007). "Grain properties of Oort Cloud comets: Modeling the mineralogical composition of cometary dust from mid-infrared emission features". Highlights in Planetary Science, 2nd General Assembly of Asia Oceania Geophysical Society 55 (9): 1044–1049. doi:10.1016/j.pss.2006.11.012. Bibcode2007P&SS...55.1044O. 
  28. Michael J. Mumma et al. (2005). "Parent Volatiles in Comet 9P/Tempel 1: Before and After Impact". Science Express 310 (5746): 270–274. doi:10.1126/science.1119337. PMID 16166477. Bibcode2005Sci...310..270M. Retrieved 2018-08-02. 
  29. "Oort Cloud & Sol b?". SolStation. 
  30. "The Sun Steals Comets from Other Stars". NASA. 2010. 
  31. Julio A. Fernández; Tabaré Gallardo; Adrián Brunini (2004). "The scattered disc population as a source of Oort Cloud comets: evaluation of its current and past role in populating the Oort Cloud". Icarus 172 (2): 372–381. doi:10.1016/j.icarus.2004.07.023. Bibcode2004Icar..172..372F. 
  32. Davies, J. K.; Barrera, L. H. (2004). The First Decadal Review of the Edgeworth-Kuiper Belt.. Kluwer Academic Publishers. ISBN 978-1-4020-1781-0. Retrieved 2020-10-11. 
  33. S. Alan Stern; Paul R. Weissman (2001). "Rapid collisional evolution of comets during the formation of the Oort Cloud". Nature 409 (6820): 589–591. doi:10.1038/35054508. PMID 11214311. Bibcode2001Natur.409..589S. 
  34. R. Brasser; M. J. Duncan; H.F. Levison (2006). "Embedded star clusters and the formation of the Oort Cloud". Icarus 184 (1): 59–82. doi:10.1016/j.icarus.2006.04.010. Bibcode2006Icar..184...59B. 
  35. Levison, Harold (10 June 2010). "Capture of the Sun's Oort Cloud from Stars in Its Birth Cluster". Science 329 (5988): 187–190. doi:10.1126/science.1187535. PMID 20538912. Bibcode2010Sci...329..187L. 
  36. "Many famous comets originally formed in other solar systems". Southwest Research Institute® (SwRI®) News. 10 June 2010. 
  37. Brasser, R.; Morbidelli, A. (2013-07-01). "Oort cloud and Scattered Disc formation during a late dynamical instability in the Solar System" (in en). Icarus 225 (1): 40–49. doi:10.1016/j.icarus.2013.03.012. ISSN 0019-1035. Bibcode2013Icar..225...40B. Retrieved 2020-11-16. 
  38. Siraj, Amir; Loeb, Abraham (2020-08-18). "The Case for an Early Solar Binary Companion" (in en). The Astrophysical Journal 899 (2): L24. doi:10.3847/2041-8213/abac66. ISSN 2041-8213. Bibcode2020ApJ...899L..24S. 
  39. "The Sun May Have Started Its Life with a Binary Companion" (in en). 2020-08-17. 
  40. Horizons output. "Barycentric Osculating Orbital Elements for Comet C/1999 F1 (Catalina)".  Solution using the Solar System Barycenter. Ephemeris Type:Elements and Center:@0 (To be outside planetary region, inbound epoch 1950 and outbound epoch 2050. For epoch 1950-Jan-01 orbit period is "PR= 1.6E+09 / 365.25 days" = ~4.3 million years)
  41. Harold E. Levison; Luke Dones (2007). Comet Populations and Cometary dynamics. 575–588. doi:10.1016/B978-012088589-3/50035-9. ISBN 978-0-12-088589-3. 
  42. J Horner; NW Evans; ME Bailey; DJ Asher (2003). "The Populations of Comet-like Bodies in the Solar System". Monthly Notices of the Royal Astronomical Society 343 (4): 1057–1066. doi:10.1046/j.1365-8711.2003.06714.x. Bibcode2003MNRAS.343.1057H. 
  43. Luke Dones; Paul R Weissman; Harold F Levison; Martin J Duncan (2004). "Oort Cloud Formation and Dynamics". in Michel C. Festou. Comets II. University of Arizona Press. pp. 153–173. Retrieved 2008-03-22. 
  44. 44.0 44.1 Julio A. Fernández (2000). "Long-Period Comets and the Oort Cloud". Earth, Moon, and Planets 89 (1–4): 325–343. doi:10.1023/A:1021571108658. Bibcode2002EM&P...89..325F. 
  45. Licandro, Javier; de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl; de Leon, Julia; Serra-Ricart, Miquel; Cabrera-Lavers, Antonio (28 May 2019). "Spectroscopic and dynamical properties of comet C/2018 F4, likely a true average former member of the Oort cloud". Astronomy and Astrophysics 625: A133 (6 pages). doi:10.1051/0004-6361/201834902. Bibcode2019A&A...625A.133L. 
  46. Marc Fouchard; Christiane Froeschlé; Giovanni Valsecchi; Hans Rickman (2006). "Long-term effects of the galactic tide on cometary dynamics". Celestial Mechanics and Dynamical Astronomy 95 (1–4): 299–326. doi:10.1007/s10569-006-9027-8. Bibcode2006CeMDA..95..299F. 
  47. Higuchi A.; Kokubo E.; Mukai, T. (2005). "Orbital Evolution of Planetesimals by the Galactic Tide". Bulletin of the American Astronomical Society 37: 521. Bibcode2005DDA....36.0205H. 
  48. Nurmi P.; Valtonen M.J.; Zheng J.Q. (2001). "Periodic variation of Oort Cloud flux and cometary impacts on the Earth and Jupiter". Monthly Notices of the Royal Astronomical Society 327 (4): 1367–1376. doi:10.1046/j.1365-8711.2001.04854.x. Bibcode2001MNRAS.327.1367N. 
  49. John J. Matese; Jack J. Lissauer (2004). "Perihelion evolution of observed new comets implies the dominance of the galactic tide in making Oort Cloud comets discernible". Icarus 170 (2): 508–513. doi:10.1016/j.icarus.2004.03.019. Bibcode2004Icar..170..508M. Retrieved 2018-08-02. 
  50. Mamajek, Eric E.; Barenfeld, Scott A.; Ivanov, Valentin D. (2015). "The Closest Known Flyby of a Star to the Solar System". The Astrophysical Journal 800 (1): L17. doi:10.1088/2041-8205/800/1/L17. Bibcode2015ApJ...800L..17M. Retrieved 2018-08-02. 
  51. 51.0 51.1 L. A. Molnar; R. L. Mutel (1997). "Close Approaches of Stars to the Oort Cloud: Algol and Gliese 710". American Astronomical Society 191st meeting. American Astronomical Society. Bibcode1997AAS...191.6906M. 
  52. A. Higuchi; E. Kokubo; T. Mukai (2006). "Scattering of Planetesimals by a Planet: Formation of Comet Cloud Candidates". Astronomical Journal 131 (2): 1119–1129. doi:10.1086/498892. Bibcode2006AJ....131.1119H. Retrieved 2019-08-25. 
  53. J. G. Hills (1984). "Dynamical constraints on the mass and perihelion distance of Nemesis and the stability of its orbit". Nature 311 (5987): 636–638. doi:10.1038/311636a0. Bibcode1984Natur.311..636H. 
  54. "Nemesis is a myth". Max Planck Institute. 2011. 
  55. 55.0 55.1 55.2 "Can WISE Find the Hypothetical 'Tyche'?". NASA/JPL. February 18, 2011. 
  56. John J. Matese; Jack J. Lissauer (2002-05-06). "Continuing Evidence of an Impulsive Component of Oort Cloud Cometary Flux". Proceedings of Asteroids, Comets, Meteors - ACM 2002. International Conference, 29 July - 2 August 2002, Berlin, Germany. 500. University of Louisiana at Lafayette, and NASA Ames Research Center. 309. Bibcode2002ESASP.500..309M. Retrieved 2008-03-21. 
  57. K. L., Luhman (7 March 2014). "A Search For A Distant Companion To The Sun With The Wide-field Infrared Survey Explorer". The Astrophysical Journal 781 (1): 4. doi:10.1088/0004-637X/781/1/4. Bibcode2014ApJ...781....4L. 
  58. Darling, David. "TAU (Thousand Astronomical Unit) mission". 
  59. 59.0 59.1 59.2 "The Whipple Mission: Exploring the Oort Cloud and the Kuiper Belt". 
  60. "Scientific American – Kepler Spacecraft May Be Able to Spot Elusive Oort Cloud Objects – 2010". 

Explanatory notes

  1. The Oort cloud's outer limit is difficult to define as it varies over the millennia as different stars pass the Sun and thus is subject to variation. Estimates of its distance range from 50,000 to 200,000 au.

External links