Oort cloud

An artist's rendering of the Oort cloud and the Kuiper belt (inset)
TNOs and similar bodies
*Trans-Neptunian dwarf planets are "plutoids"

The Oort cloud (pronounced /ˈɔrt/ ort, alternatively the Öpik-Oort cloud IPA: [ˈøpik]) is a hypothesized spherical cloud of comets which may lie roughly 50,000 AU, or nearly a light-year, from the Sun.[1] This places the cloud at nearly a quarter of the distance to Proxima Centauri, the nearest extrasolar star. The Kuiper belt and scattered disc, the other two known reservoirs of trans-Neptunian objects, are less than one thousandth the Oort cloud's distance. The outer extent of the Oort cloud defines the gravitational boundary of our Solar System.[2]

The Oort cloud is thought to comprise two separate regions: a spherical outer Oort cloud and a disc-shaped inner Oort cloud, or Hills cloud. Objects in the Oort cloud are largely composed of ices, such as water, ammonia, and methane. Astronomers believe that the matter comprising the Oort cloud formed closer to the Sun and was scattered far out into space by the gravitational effects of the giant planets early in the Solar System's evolution.[1]

Although no confirmed direct observations of the Oort cloud have been made, astronomers believe that it is the source of all long-period and Halley-type comets entering the inner Solar System and many of the Centaurs and Jupiter-family comets as well.[3] 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 Galaxy itself. These forces occasionally dislodge comets from their orbits within the cloud and send them towards the inner Solar System.[1] Based on their orbits, most of the short-period comets may come from the scattered disc, but some may still have originated from the Oort cloud.[1][3] Although the Kuiper belt and the farther scattered disc have been observed and mapped, only four currently known trans-Neptunian objects—90377 Sedna, 2000 CR105, 2006 SQ372 and 2008 KV42—are considered possible members of the inner Oort cloud.[4][5]

Contents

Hypothesis

In 1932, Estonian astronomer Ernst Öpik postulated that long-period comets originated in an orbiting cloud at the outermost edge of the Solar System.[6] In 1950, the idea was independently revived by Dutch astronomer Jan Hendrik Oort as a means to resolve a paradox:[7] over the course of the Solar System's existence, the orbits of comets are unstable; eventually, dynamics dictate that a comet must either collide with the Sun or a planet, or else 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, reasoned Oort, a comet could not have formed on its current orbit, and must have been held in an outer reservoir for almost all of its existence.[7][8][9]

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 short orbits, below 10 AU, and follow the ecliptic plane, the same plane in which the planets lie. Nearly all isotropic comets have very long orbits, on the order of thousands of AU, and appear from every corner of the sky.[9] Oort noted that there was a peak in numbers of nearly isotropic 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.[9] 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[9] to as far as 50,000 AU[1] from the Sun. Some estimates place the outer edge at between 100,000 and 200,000 AU.[9] The region can be subdivided into a spherical outer Oort cloud (20,000–50,000 AU), and a doughnut-shaped inner Oort cloud (2,000–20,000 AU). 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.[1] The inner Oort cloud is also known as the Hills cloud, named after J. G. Hills, who proposed its existence in 1981.[10] Models predict that the inner cloud should have tens or hundreds of times as many cometary nuclei as the outer halo;[10][11][12] it is seen as a possible source of new comets to resupply the relatively 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.[13]

The outer Oort cloud is believed to contain several trillion individual objects larger than approximately 1 km[1] (with many billions with absolute magnitudes[14] brighter than 11 - corresponding to ~20 km diameter), with neighboring objects typically tens of millions of kilometres apart.[3][15] Its total mass is not known with certainty, but, assuming that Halley's comet is a suitable prototype for all comets within the outer Oort cloud, the estimated combined mass is 3 × 1025 kilograms, or roughly five times the mass of the Earth.[1][16] Earlier it was thought to be more massive (up to 380 Earth masses),[17] but improved knowledge of the size distribution of long-period comets has led to much lower estimates. The mass of the inner Oort Cloud is not currently known.

If analyses of comets are representative of the whole, the vast majority of Oort-cloud objects consist of various ices such as water, methane, ethane, carbon monoxide and hydrogen cyanide.[18] However, the discovery of the object 1996 PW, an asteroid in an orbit more typical of a long-period comet, suggests that the cloud may also be home to rocky objects.[19] Analysis of the carbon and nitrogen isotope ratios in both the Oort cloud and Jupiter-family comets shows little difference between the two, despite their vastly separate regions of origin. This suggests that both originated from the original protosolar cloud,[20] a conclusion also supported by studies of granular size in Oort cloud comets[21] and by the recent impact study of Jupiter-family comet Tempel 1.[22]

Origin

The Oort cloud is thought to be a remnant of the original protoplanetary disc that formed around the Sun approximately 4.6 billion years ago.[1] 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 asteroids, but that gravitational interaction with young gas giant planets such as Jupiter ejected the objects into extremely long elliptic or parabolic orbits.[1][23] 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.[1]

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 towards the Oort cloud, while 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.[24] A third of the scattered disc's population is likely to end up in the Oort cloud after 2.5 billion years.[25]

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.[26] The estimated mass of the cloud is only a small part of the 50–100 Earth masses of ejected material.[1]

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.[1] On the other hand, the Hills cloud, which is bound more strongly to the Sun, has yet to acquire 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.[27]

In June 2010 Harold F. Levison and others have 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 disks of other stars." [28]

Comets

Comet Hale-Bopp, an archetypal Oort cloud comet

Comets are believed 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 the Kuiper belt or scattered disc, two linked flat discs of icy debris beyond Neptune's orbit at 30 AU and jointly extending out beyond 100 AU from the Sun. Long-period comets, such as comet Hale-Bopp, whose orbits last for thousands of years, are thought to originate in the Oort cloud. The orbits within the Kuiper belt are relatively stable, and so very few comets are believed 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.[29] These centaurs are then sent farther inward to become the short-period comets.[30]

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 while they are short-period comets, their ultimate origin lies in the Oort cloud, not in the scattered disc. Based on their orbits, it is believed they were long-period comets that were captured by the gravity of the giant planets and sent into the inner Solar System.[8] 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.[3]

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 known dynamical process can explain this undercount of observed comets. 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.[31] Dynamical studies of Oort Cloud comets have shown that their occurrence in the outer planet region is 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.[32]

Tidal effects

Most of the comets seen close to the Sun are believed to have reached their current positions through gravitational distortion of the Oort cloud by the tidal force exerted by the Milky Way galaxy. Just as the Moon's tidal force bends and deforms the Earth's oceans, causing the tides to rise and fall, so the galactic tide also bends and distorts the orbits of bodies in the outer Solar System, pulling them towards the galactic centre. In the charted regions of the Solar System, these effects are negligible compared to the gravity of the Sun. At the outer reaches of the system, however, the Sun's gravity is weaker and the gradient of the Milky Way's gravitational field plays a far more noticeable role. Because of this gradient, galactic tides can deform an otherwise spherical Oort cloud, stretching the cloud in the direction of the galactic centre and compressing it along the other two axes. These small galactic perturbations may be enough to dislodge members of the Oort cloud from their orbits, sending them towards the Sun.[33] 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 theorise that the galactic tide may have contributed to the formation of the Oort cloud by increasing the perihelia—closest distances to the Sun—of planetesimals with large aphelia.[34] 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.[35] 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.[36]

Star perturbations and stellar companion hypotheses

Besides the galactic tide, the main trigger for sending comets into the inner Solar System is believed to be interaction between the Sun's Oort cloud and the gravitational fields of near-by stars[1] or giant molecular clouds.[32] 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, during the next 10 million years the known star with the greatest possibility of perturbing the Oort cloud is Gliese 710.[37] This process also serves to scatter the objects out of the ecliptic plane, potentially also explaining the cloud's spherical distribution.[37][38]

In 1984, Physicist Richard A. Muller postulated that the Sun has a heretofore undetected companion, either a brown dwarf star, a dim red dwarf star or a gaseous giant planet, in an elliptical orbit within the Oort cloud. This object, known as Nemesis, is 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 direct evidence of Nemesis has been found.[39] One star survey using parallax measurements in order to clarify local star distances, the WISE mission, is currently underway with part of its mission being to help with either proving or disproving the Nemesis hypothesis.[40] The analysis of this survey is expected to be completed by 2013. Two other planned astronomical missions, the Pan-STARRS and the LSST astronomical surveys may also be able to aid in resolving the debate over the existence or non-existence of a Nemesis companion star to our Sun.[41]

A somewhat similar hypothesis was advanced by astronomer John J. Matese of the University of Louisiana in 2002. He contends that more comets are arriving in the inner Solar System from a particular region of the Oort Cloud than can be explained by the galactic tide or stellar perturbations alone, and that the most likely cause is a Jupiter-mass object in a distant orbit.[42]

Oort cloud objects (OCOs)

Main article: Detached object
Sedna, a possible inner Oort cloud object discovered in 2003

Apart from long-period comets, only four known objects have orbits which suggest that they may belong to the Oort cloud: 90377 Sedna, 2000 CR105, 2006 SQ372 and 2008 KV42. The first two, unlike scattered disc objects, have perihelia outside the gravitational reach of Neptune, and thus their orbits cannot be explained by perturbations from the gas giant planets.[43] If they formed in their current locations, their orbits must originally have been circular; otherwise accretion (the coalescence of smaller bodies into larger ones) would not have been possible because the large relative velocities between planetesimals would have been too disruptive.[44] Their present-day elliptical orbits can be explained by a number of hypotheses:

  1. These objects could have had their orbits and perihelion distances "lifted" by the passage of a nearby star when the Sun was still embedded in its birth star cluster.[4]
  2. Their orbits could have been disrupted by an as-yet-unknown planet-sized body within the Oort cloud.[45]
  3. They could have been scattered by Neptune during a period of particularly high eccentricity or by the gravity of a far larger primordial trans-Neptunian disc.
  4. They could have been captured from around smaller passing stars.

Of these, the stellar disruption and "lift" hypothesis appears to agree most closely with observations.[4] Some astronomers prefer to refer to Sedna and 2000 CR105 as belonging to the "extended scattered disc" rather than to the inner Oort cloud.[44]

Oort cloud object candidates
Number Name Equatorial diameter
(km)		 Perihelion (AU) Aphelion (AU) Year discovered Discoverer Diameter method
90377 Sedna 1,180–1,800 km 76.1 892 2003 Brown, Trujillo, Rabinowitz thermal[46]
148209 2000 CR105 ~250 km 44.3 397 2000 Lowell Observatory assumed[47]
- 2006 SQ372 50–100 km 24.17 2,005.38 2006 SDSS assumed[48]
- 2008 KV42 58.9 km[49] 20.217 71.760 2008 Canada-France-Hawaii Telescope assumed[5]

See also


References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 Alessandro Morbidelli (2008-02-03). "Origin and dynamical evolution of comets and their reservoirs" (PDF). arxiv. http://arxiv.org/abs/astro-ph/0512256. Retrieved 2007-05-26. 
  2. ↑ "NASA Solar System Exploration". "Oort Cloud". http://solarsystem.nasa.gov/planets/profile.cfm?Object=OortCloud&Display=OverviewLong. Retrieved 2008-12-02. 
  3. ↑ 3.0 3.1 3.2 3.3 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 (Royal Astronomical Society) 381 (2): 779–789. doi:10.1111/j.1365-2966.2007.12269.x. http://www.blackwell-synergy.com/doi/abs/10.1111/j.1365-2966.2007.12269.x. Retrieved 2008-03-31. 
  4. ↑ 4.0 4.1 4.2 Alessandro Morbidelli; Harold Levison (2004). "Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna)". The Astronomical Journal (University of Chicago Press) 128 (5): 2564–2576. doi:10.1086/424617. http://adsabs.harvard.edu/abs/2004AJ....128.2564M. 
  5. ↑ 5.0 5.1 "International Team of Astronomers Finds Missing Link". NRC Herzberg Institute of Astrophysics. 2008. http://www.nrc-cnrc.gc.ca/eng/news/hia/2008/09/04/asteroid-2008kv42.html. Retrieved 2008-09-05. 
  6. ↑ Ernst Julius Öpik (1932). "Note on Stellar Perturbations of Nearby Parabolic Orbits". Proceedings of the American Academy of Arts and Sciences 67: 169–182. 
  7. ↑ 7.0 7.1 Jan Oort (1950). "The structure of the cloud of comets surrounding the Solar System and a hypothesis concerning its origin" (PDF). Bull. Astron. Inst. Neth. 11: 91–110. http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1950BAN....11...91O&data_type=PDF_HIGH&type=PRINTER&filetype=.pdf. 
  8. ↑ 8.0 8.1 David C. Jewitt (2001). "From Kuiper Belt to Cometary Nucleus: The Missing Ultrared Matter". University of Chicago. http://www.journals.uchicago.edu/doi/full/10.1086/338692. Retrieved 2007-06-26. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 9.6 9.7 Harold F. Levison, Luke Donnes (2007). "Comet Populations and Cometary Dynamics". In Lucy Ann Adams McFadden, Lucy-Ann Adams, Paul Robert Weissman, Torrence V. Johnson. Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 575–588. ISBN 0120885891. 
  10. ↑ 10.0 10.1 Jack G. Hills (November 1981). "Comet showers and the steady-state infall of comets from the Oort Cloud". The Astronomical Journal 86: 1730–1740. doi:10.1086/113058. http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1981AJ.....86.1730H&db_key=AST&data_type=HTML&format=&high=44b52c369025824. 
  11. ↑ Harold F. Levison, Luke Dones, Martin J. Duncan (April 2001). "The Origin of Halley-Type Comets: Probing the Inner Oort Cloud". The Astronomical Journal, Vol. 121. The American Astronomical Society.. pp. 2253–2267. http://adsabs.harvard.edu/abs/2001AJ....121.2253L. Retrieved 2007-06-27. 
  12. ↑ 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. pp. 251. ISBN 0-309-04333-6. 
  13. ↑ Julio A. Fernéndez (1997-04-07). "The Formation of the Oort Cloud and the Primitive Galactic Environment" (PDF). Icarus (Elsevier) (219): 106–119. http://www.gps.caltech.edu/classes/ge133/reading/oort.pdf. Retrieved 2008-03-18. 
  14. ↑ Absolute magnitude is a measure of how bright an object would be if it were exactly 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 true brightness. The lower an object's absolute magnitude, the brighter it is.
  15. ↑ Paul R. Weissman (1998). "The Oort Cloud". Scientific American. Scientific American, Inc.. http://www.sciamdigital.com/index.cfm?fa=Products.ViewIssuePreview&ISSUEID_CHAR=8DB2FB44-6B4B-47AF-B46B-791A911764D&ARTICLEID_CHAR=B294C211-98B8-4374-92AB-158C4866AB1. Retrieved 2007-05-26. 
  16. ↑ Paul R. Weissman (1983-02-01). "The mass of the Oort Cloud". Astronomy and Astrophysics (American Astronomical Society) 118 (1): 90–94. http://adsabs.harvard.edu/abs/1983A&A...118...90W. Retrieved 2008-03-31. 
  17. ↑ Sebastian Buhai. "On the Origin of the Long Period Comets: Competing theories". Utrecht University College. http://66.102.1.104/scholar?hl=en&lr=&safe=off&q=cache:oco9aJ2k6UoJ:www.tinbergen.nl/~buhai/pictures/UCU/Physics_AppliedMathematics/Astrophysics/long_period_comets.pdf+380+mass+earth+oort-cloud. Retrieved 2008-03-29. 
  18. ↑ E. L. Gibb, M. J. Mumma, N. Dello Russo, M. A. DiSanti and K. Magee-Sauer (October 2003). "Methane in Oort Cloud comets". Icarus (Elselvier) 165 (2): 391–406. doi:10.1016/S0019-1035(03)00201-X. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-49H6Y7T-1&_user=10&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=15835488b797048e6387a553b257695b. Retrieved 2008-03-31. 
  19. ↑ Paul R. Weissman, Harold F. Levison (1997). "Origin and Evolution of the Unusual Object 1996 PW: Asteroids from the Oort Cloud?". Earth and Space Sciences Division, Jet Propulsion Laboratory, Space Sciences Department, Southwest Research Institute. University of Chicago Press. http://www.journals.uchicago.edu/doi/full/10.1086/310940. Retrieved 2007-05-26. 
  20. ↑ D. Hutsemekers, J. Manfroid, E. Jehin, C. Arpigny, A. Cochran, R. Schulz, J.A. St¨uwe, and J.M. Zucconi (2005). "Isotopic abundances of carbon and nitrogen in Jupiter-family and Oort Cloud comets". Astronomy and Astrophysics (American Astronomical Society) 440: L21–L24. doi:10.1051/0004-6361:200500160. http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2005/35/aahf085/aahf085.html. Retrieved 2008-03-31. 
  21. ↑ Takafumi Ootsubo, Jun-ichi Watanabe, Hideyo Kawakita, Mitsuhiko Honda and Reiko Furusho (June 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 (Elselvier) 55 (9): 1044–1049. doi:10.1016/j.pss.2006.11.012. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6V6T-4MW95KK-2&_user=10&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=c34afe76f6d7a2617bd502724b9fcd35. Retrieved 2008-03-31. 
  22. ↑ Michael J. Mumma, Michael A. DiSanti, Karen Magee-Sauer et al. (2005-09-15). "Parent Volatiles in Comet 9P/Tempel 1: Before and After Impact". Science Express (Nature Publishing Group) 310 (5746): 270–274. doi:10.1126/science.1119337. PMID 16166477. http://www.sciencemag.org/cgi/content/abstract/310/5746/270. Retrieved 2008-03-22. 
  23. ↑ "Oort Cloud & Sol b?". SolStation. http://www.solstation.com/stars/oort.htm. Retrieved 2007-05-26. 
  24. ↑ Julio A. Fernández, Tabaré Gallardo and Adrián Brunini (December 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 (Elsevier) 172 (2): 372–381. doi:10.1016/j.icarus.2004.07.023. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-4DGW3Y9-1&_user=10&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=43509a25b71b753a2046b1928019aaee. Retrieved 2008-03-31. 
  25. ↑ Davies, J. K.; Barrera, L. H. (2004). The First Decadal Review of the Edgeworth-Kuiper Belt.. Kluwer Academic Publishers. ISBN 9781402017810. http://books.google.com/?id=WuDdVbJf_d8C&pg=PA43&dq=+oort+cloud. 
  26. ↑ S. Alan Stern, Paul R. Weissman (2001-02-01). "Rapid collisional evolution of comets during the formation of the Oort Cloud". Nature (Nature Publishing Group) 409 (6820): 589–591. doi:10.1038/35054508. PMID 11214311. http://adsabs.harvard.edu/abs/2001Natur.409..589S. Retrieved 2008-03-31. 
  27. ↑ R. Brasser, M. J. Duncan, H.F. Levison (2006). "Embedded star clusters and the formation of the Oort Cloud". Icarus (Elsevier) 184 (1): 59–82. doi:10.1016/j.icarus.2006.04.010. http://adsabs.harvard.edu/abs/2006Icar..184...59B. Retrieved 2007-05-26. 
  28. ↑ Harold F. Levison (2010), "Capture of the Sun's Oort Cloud from Stars in Its Birth Cluster" (Science June 10, 2010)
  29. ↑ Harold E. Levison and Luke Dones (2007). "Comet Populations and Cometary dynamics". Encyclopedia of the Solar System: 575–588. 
  30. ↑ J Horner, NW Evans, ME Bailey, DJ Asher (2003). "The Populations of Comet-like Bodies in the Solar System" (PDF). http://star.arm.ac.uk/preprints/396.pdf. Retrieved 2007-06-29. 
  31. ↑ Luke Dones, Paul R Weissman, Harold F Levison, Martin J Duncan (2004). "Oort Cloud Formation and Dynamics". In Michel C. Festou; H. Uwe Keller; Harold A. Weaver. Comets II. The University of Arizona Press. pp. 153–173. http://www.lpi.usra.edu/books/CometsII/7031.pdf. Retrieved 2008-03-22. 
  32. ↑ 32.0 32.1 Julio A. Fernández (October 2000). "Long-Period Comets and the Oort Cloud". Earth, Moon, and Planets (Springer Netherlands) 89 (1–4): 325–343. doi:10.1023/A:1021571108658. http://www.springerlink.com/content/t45273004183469h/. Retrieved 2008-03-25. 
  33. ↑ Marc Fouchard, Christiane Froeschlé, Giovanni Valsecchi, Hans Rickman (2006). "Long-term effects of the galactic tide on cometary dynamics". Celestial Mechanics and Dynamical Astronomy (Springer) 95 (1–4): 299–326. doi:10.1007/s10569-006-9027-8. http://adsabs.harvard.edu/abs/2006CeMDA..95..299F. 
  34. ↑ Higuchi A., Kokubo E. & Mukai, T. (2005). "Orbital Evolution of Planetesimals by the Galactic Tide". Bulletin of the American Astronomical Society (American Astronomical Society) 37: 521. http://adsabs.harvard.edu/abs/2005DDA....36.0205H. 
  35. ↑ 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 (Blackwell) 327: 1367–1376. doi:10.1046/j.1365-8711.2001.04854.x. http://adsabs.harvard.edu/abs/2001MNRAS.327.1367N. 
  36. ↑ John J. Matese and Jack J. Lissauer (August 2004). "Perihelion evolution of observed new comets implies the dominance of the galactic tide in making Oort Cloud comets discernible". Icarus (Elselvier) 170 (2): 508–513. doi:10.1016/j.icarus.2004.03.019. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-4CHRXV5-3&_user=10&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=ffd9ac2ea18895488f80d5255be2b448. Retrieved 2008-03-21. 
  37. ↑ 37.0 37.1 L. A. Molnar, R. L. Mutel (1998-01-09). "Close Approaches of Stars to the Oort Cloud: Algol and Gliese 710". American Astronomcial Society 191st meeting. The American Astronomcial Society. http://www.aas.org/publications/baas/v29n5/aas191/abs/S069006.html. Retrieved 2008-03-31. 
  38. ↑ A. Higuchi, E. Kokubo and T. Mukai (February 2006). "Scattering of Planetesimals bya a Planet: Formation of Comet Cloud Candidates". The Astronomical Journal (The American Astronomical Society) 131: 1119–1129. http://www.iop.org/EJ/article/1538-3881/131/2/1119/204756.text.html. Retrieved 2007-05-27. 
  39. ↑ J. G. Hills (1984-10-18). "Dynamical constraints on the mass and perihelion distance of Nemesis and the stability of its orbit". Nature (Nature Publishing Group) 311: 636–638. doi:10.1038/311636a0. http://www.nature.com/nature/journal/v311/n5987/abs/311636a0.html. Retrieved 2008-03-25. 
  40. ↑ "Getting WISE About Nemesis". Discover magazine. 2010. http://www.astrobio.net/exclusive/3427/getting-wise-about-nemesis. Retrieved 2010-03-26. 
  41. ↑ "Nemesis". Universe Today. http://www.universetoday.com/tag/binary-star/. Retrieved 2010-04-01. 
  42. ↑ John J. Matese and Jack J. Lissauer (2002-05-06). "Continuing Evidence of an Impulsive Component of Oort Cloud Cometary Flux" (PDF). 1University of Louisiana at Lafayette, and NASA Ames Research Center. http://www.ucs.louisiana.edu/~jjm9638/acm2002/acm2002_05_06.pdf. Retrieved 2008-03-21. 
  43. ↑ Michael E. Brown, Chadwick Trujillo, David Rabinowitz (December 10, 2004). "Discovery Of A Candidate Inner Oort Cloud Planetoid". The Astrophysical Journal 617: 645–649. doi:10.1086/422095. http://64.233.179.104/scholar?hl=en&lr=&safe=off&q=cache:VGo9PER564YJ:www.gps.caltech.edu/classes/ge133/reading/sedna.pdf+. Retrieved 2008-04-02. 
  44. ↑ 44.0 44.1 Scott S. Sheppard; D. Jewitt (2005). "Small Bodies in the Outer Solar System" (PDF). Frank N. Bash Symposium. The University of Texas at Austin. http://www.dtm.ciw.edu/users/sheppard/pub/Sheppard06smallbodies.pdf. Retrieved 2008-03-25. 
  45. ↑ Rodney S. Gomes; John J. Matese, Jack J. Lissauer (2006). "A distant planetary-mass solar companion may have produced distant detached objects". Icarus (Elsevier) 184 (2): 589–601. doi:10.1016/j.icarus.2006.05.026. http://adsabs.harvard.edu/abs/2006Icar..184..589G. 
  46. ↑ W.M. Grundy, K.S. Noll and D.C. Stephens (July 2005). "Diverse albedos of small trans-Neptunian objects". Icarus (Elsevier) 176 (1): 184–191. doi:10.1016/j.icarus.2005.01.007. http://www.sciencedirect.com/science?_ob=ArticleURL&_udi=B6WGF-4FR4BS3-3&_user=10&_rdoc=1&_fmt=&_orig=search&_sort=d&view=c&_acct=C000050221&_version=1&_urlVersion=0&_userid=10&md5=086bf515703846247c0819bb30f5b5f1. Retrieved 2008-03-22.  (arxiv.org)
  47. ↑ E. L. Schaller and M. E. Brown (2007). "Volatile loss and retention on Kuiper belt objects". Astrophysical Journal 659: I.61–I.64. doi:10.1086/516709. http://64.233.183.104/search?q=cache:YBGHuSlg6a0J:www.gps.caltech.edu/~mbrown/papers/ps/volatiles.pdf+VOLATILE+LOSS+AND+RETENTION+ON+KUIPER+BELT+OBJECTS&hl=en&ct=clnk&cd=1&gl=uk&lr=lang_en. Retrieved 2008-04-02.  (PDF)
  48. ↑ "Solar System's newest member points to inner Oort Cloud". Astronomy Now. 2008. http://www.astronomynow.com/080818NewObjectPointsToInnerOortCloud.html. Retrieved 2008-08-19. 
  49. ↑ http://www.hohmanntransfer.com/mn/08/08198_0716.htm

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