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Journal articles on the topic 'Edgeworth Kuiper belt'

Author: Grafiati

Published: 4 June 2021

Last updated: 13 February 2022

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1

Ipatov, S. I. "Evolution of the Edgeworth-Kuiper Belt." Highlights of Astronomy 12 (2002): 247–48. http://dx.doi.org/10.1017/s153929960001340x.

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AbstractDue to gravitational interactions with large trans-neptunian objects (TNOs) several percent of TNOs can change their semimajor axes by more that 1 AU during last 4 Gyr. Now about 30000 1-km former TNOs can be Jupiter crossers and about 20% of Earth-crossing objects can be former TNOs which now move in Jupiter-crossing orbits.

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2

Yamamoto, T. "Are Edgeworth-Kuiper Belt Objects Pristine?" Science 273, no. 5277 (August 16, 1996): 921–0. http://dx.doi.org/10.1126/science.273.5277.921.

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3

Hughes, David W. "Quaoar and the Edgeworth-Kuiper belt." Astronomy and Geophysics 44, no. 3 (June 2003): 3.21–3.22. http://dx.doi.org/10.1046/j.1468-4004.2003.44321.x.

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4

Collander-Brown, S. "The plane of the Edgeworth–Kuiper belt." Icarus 162, no. 1 (March 2003): 22–26. http://dx.doi.org/10.1016/s0019-1035(02)00061-1.

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5

DAVIS, D., and P. FARINELLA. "Collisional Evolution of Edgeworth–Kuiper Belt Objects☆." Icarus 125, no. 1 (January 1997): 50–60. http://dx.doi.org/10.1006/icar.1996.5595.

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6

Barucci, M. "Spectrophotometric Observations of Edgeworth–Kuiper Belt Objects." Icarus 142, no. 2 (December 1999): 476–81. http://dx.doi.org/10.1006/icar.1999.6212.

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7

Doressoundiram, A., N. Peixinho, C. de Bergh, S. Fornasier, P. Thébault, M. A. Barucci, and C. Veillet. "The Color Distribution in the Edgeworth-Kuiper Belt." Astronomical Journal 124, no. 4 (October 2002): 2279–96. http://dx.doi.org/10.1086/342447.

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8

Fulchignoni, Marcello, and Audrey C. Delsanti. "A statistical insight into the Edgeworth-Kuiper belt." Comptes Rendus Physique 4, no. 7 (September 2003): 767–74. http://dx.doi.org/10.1016/j.crhy.2003.09.013.

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9

Taidakova, Tanya, Leonid M. Ozernoy, and Nick N. Gorkavyi. "Resonant Gaps in the Scattered Cometary Population of the Trans-Neptunian Region." Highlights of Astronomy 12 (2002): 251–52. http://dx.doi.org/10.1017/s1539299600013423.

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AbstractOur numerical simulations of the Edgeworth-Kuiper Belt objects gravitationally scattered by the four giant planets accounting for mean motion resonances reveal numerous resonant gaps in the distribution of the scattered population.

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10

Davis, Donald R., and Paolo Farinella. "Collisional Evolution of the Edgeworth-Kuiper Belt: Implications for the Origin and Evolution of Small Body Populations." Highlights of Astronomy 12 (2002): 219–22. http://dx.doi.org/10.1017/s1539299600013307.

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AbstractCollisions have been a major process that shaped the Kuiper Belt that we see today. Collisional grinding likely played a significant role in removing mass from the trans-neptunian region and collisions are a mechanism for injecting fragments into resonances to start their journey to become short period comets. The Kuiper Belt preserves the accretional size distribution in bodies ≳ 100 km while the size distribution of smaller bodies is the result of collisional evolution. Observational confirmation of the transition size between these different regimes will constrain our understanding of the origin and evolution of the Kuiper Belt.

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11

Yamamoto, S., and T. Mukai. "Thermal radiation from dust grains in Edgeworth-Kuiper Belt." Earth, Planets and Space 50, no. 6-7 (June 1998): 531–37. http://dx.doi.org/10.1186/bf03352145.

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12

De Sanctis, M. C., M. T. Capria, and A. Coradini. "Thermal Evolution and Differentiation of Edgeworth–Kuiper Belt Objects." Astronomical Journal 121, no. 5 (May 2001): 2792–99. http://dx.doi.org/10.1086/320385.

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13

Vitense, Christian, Alexander V. Krivov, and Torsten Löhne. "WILLNEW HORIZONSSEE DUST CLUMPS IN THE EDGEWORTH-KUIPER BELT?" Astronomical Journal 147, no. 6 (May 9, 2014): 154. http://dx.doi.org/10.1088/0004-6256/147/6/154.

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14

Brunini, A. "Dynamics of the Edgeworth-Kuiper Belt beyond 50 AU." Astronomy & Astrophysics 394, no. 3 (October 21, 2002): 1129–34. http://dx.doi.org/10.1051/0004-6361:20021198.

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15

Moody, Rachel, Brian Schmidt, Charles Alcock, Jeffrey Goldader, Tim Axelrod, Kem H. Cook, and Stuart Marshall. "Initial Results from the Southern Edgeworth-Kuiper belt Survey." Earth, Moon, and Planets 92, no. 1-4 (June 2003): 125–30. http://dx.doi.org/10.1023/b:moon.0000031931.12546.7f.

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16

Abedin, Abedin Y., J. J. Kavelaars, Sarah Greenstreet, Jean-Marc Petit, Brett Gladman, Samantha Lawler, Michele Bannister, et al. "OSSOS. XXI. Collision Probabilities in the Edgeworth–Kuiper Belt." Astronomical Journal 161, no. 4 (March 25, 2021): 195. http://dx.doi.org/10.3847/1538-3881/abe418.

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17

Ipatov, Sergei I. "Migration of Trans-Neptunian Objects to The Earth." International Astronomical Union Colloquium 172 (1999): 107–16. http://dx.doi.org/10.1017/s0252921100072468.

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AbstractMigration of trans–Neptunian objects under their mutual gravitation influence and the influence of the giant planets is investigated. These investigations are based on computer simulation results and on some formulas. We estimated that about 20 % of near–Earth objects with diameter d ≥ 1 km may have come from the Edgeworth–Kuiper belt.

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18

Ryan, E. "A Laboratory Impact Study of Simulated Edgeworth–Kuiper Belt Objects." Icarus 142, no. 1 (November 1999): 56–62. http://dx.doi.org/10.1006/icar.1999.6209.

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19

Klačka, J., and M. Kocifaj. "Orbital evolution of dust in the Edgeworth–Kuiper belt zone." Monthly Notices of the Royal Astronomical Society 450, no. 1 (April 17, 2015): 523–32. http://dx.doi.org/10.1093/mnras/stv583.

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20

Jones, Daniel C., Iwan P. Williams, and Mario D. Melita. "The Dynamics of Objects in the Inner Edgeworth–Kuiper Belt." Earth, Moon, and Planets 97, no. 3-4 (April 20, 2006): 435–58. http://dx.doi.org/10.1007/s11038-006-9069-7.

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21

Hsu, Hui-Chun, and Wing-Huen Ip. "The True Colors of KBOs." International Astronomical Union Colloquium 183 (2001): 263–64. http://dx.doi.org/10.1017/s0252921100079021.

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AbstractThe existence of a population of large planetoids outside the orbit of Neptune predicted by GP Kuiper, KE Edgeworth and JA Fernandez has been confirmed by ground-based observations.The physical properties of these Kuiper Belt Objects (KBOs) remain elusive. Photometric measurements have indicated that they have diverse color variations. A theoretical model is formulated to simulate the evolution of the surface materials of the KBOs under the influence of cosmic ray irradiation and meteoroid impacts. The long-term goal is to couple this theoretical model to observations and laboratory experiments such as LARA (Laboratory Astrochemistry and Astrophysics).

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22

Malhotra, R. "A Brief Summary of Kuiper Belt Research." Highlights of Astronomy 11, no. 1 (1998): 223–28. http://dx.doi.org/10.1017/s1539299600020621.

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Ideas about the contents of the Solar System beyond Neptune and Pluto can be traced back to at least Edgeworth (1943, 1949) and Kuiper (1951), who speculated on the existence of pre-planetary small bodies in the outer Solar System beyond the orbit of Neptune - remnants of the accretion process in the primordial Solar Nebula. The basis for the speculation was primarily the argument that the Solar Nebula was unlikely to have been abruptly truncated at the orbit of Neptune, and that in the trans-Neptunian accretion timescales were too long for bodies larger than about ˜ 1000 km in radius to have formed in the 4.5 billion year age of the Solar System. Another important theoretical argument relevant to this region of the Solar System is related to the origin of short period comets. Fernández (1980) suggested that the short period comets may have an origin in a disk of small bodies beyond Neptune, rather than being “captured” from the population of long period comets originating in the Oort Cloud, the latter scenario having considerable difficulty reconciling the observed flux of short period comets with the exceedingly low efficiency of transfer of long period comet orbits to short period ones by means of the gravitational perturbations of the giant planets. The new scenario received further strength in the numerical work of Duncan et al. (1988) and Quinn et al. (1990) which showed that the relatively small orbital inclinations of the Jupiter-family short period comets were not consistent with a source in the isotropic Oort Cloud of comets but could be reproduced with a source in a low-inclination reservoir beyond Neptune’s orbit. Duncan et al. named this hypothetical source the Kuiper Belt, and the name has come into common use in the last decade (although other names are also in use, e.g. Edgeworth-Kuiper Belt, and trans-Neptunian objects). A recent theoretical milestone was the work by Holman and Wisdom (1993) and Levison and Duncan (1993) on the long term stability of test particle orbits in the trans-Neptunian Solar System. This work showed that low-eccentricity, low-inclination orbits with semimajor axes in excess of about 43 AU are stable on billion year timescales, but that in the region between 35 AU and 43 AU orbital stability times range from 107 yr to more than 109 yr [see, for example, figure 1 in Holman (1995)]. Orbital instability in this intermediate region typically leads to a close encounter with Neptune which causes dramatic orbital changes, with the potential for subsequent transfer to the inner Solar System. Thus, this region could in principle serve as the reservoir of short period comets at the present epoch. However, the idea of a kinematically cold — i.e. low-eccentricity, low-inclination — population in this region is at odds with recent observations, and the question of the origin of short period comets remains unsettled at the present time.

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23

Marboeuf, Ulysse, Jean-Marc Petit, and Olivier Mousis. "Can collisional activity produce a crystallization of Edgeworth-Kuiper Belt comets?" Monthly Notices of the Royal Astronomical Society: Letters 397, no. 1 (July 21, 2009): L74—L78. http://dx.doi.org/10.1111/j.1745-3933.2009.00687.x.

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24

Kobayashi, Hiroshi, Shigeru Ida, and Hidekazu Tanaka. "The evidence of an early stellar encounter in Edgeworth–Kuiper belt." Icarus 177, no. 1 (September 2005): 246–55. http://dx.doi.org/10.1016/j.icarus.2005.02.017.

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25

Morbidelli, Alessandro, and Giovanni B. Valsecchi. "Neptune Scattered Planetesimals Could Have Sculpted the Primordial Edgeworth–Kuiper Belt." Icarus 128, no. 2 (August 1997): 464–68. http://dx.doi.org/10.1006/icar.1997.5745.

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26

Moore, M. H., R. L. Hudson, and R. F. Ferrante. "Radiation Products in Processed Ices Relevant to Edgeworth-Kuiper-Belt Objects." Earth, Moon, and Planets 92, no. 1-4 (June 2003): 291–306. http://dx.doi.org/10.1023/b:moon.0000031946.53696.f6.

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27

Osip, David J., S. D. Kern, and J. L. Elliot. "Physical Characterization of the Binary Edgeworth–Kuiper Belt Object 2001 QT297." Earth, Moon, and Planets 92, no. 1-4 (June 2003): 409–21. http://dx.doi.org/10.1023/b:moon.0000031955.57130.91.

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28

McFarland, John. "Kenneth Essex Edgeworth—Victorian polymath and founder of the Kuiper belt?" Vistas in Astronomy 40, no. 2 (January 1996): 343–54. http://dx.doi.org/10.1016/0083-6656(96)00014-1.

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29

Kennedy, Grant M., and Mark C. Wyatt. "Two-temperature Debris Disks: Signposts for Directly Imaged Planets?" Proceedings of the International Astronomical Union 10, S314 (November 2015): 163–66. http://dx.doi.org/10.1017/s1743921315006201.

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AbstractThis work considers debris disks whose spectra can be modelled by dust emission at two different temperatures. These disks are typically assumed to be a sign of multiple belts, but only a few cases have been confirmed via high resolution observations. We derive the properties of a sample of two-temperature disks, and explore whether this emission can arise from dust in a single narrow belt. While some two-temperature disks arise from single belts, it is probable that most have multiple spatial components. These disks are plausibly similar to the outer Solar System's configuration of Asteroid and Edgeworth-Kuiper belts separated by giant planets. Alternatively, the inner component could arise from inward scattering of material from the outer belt, again due to intervening planets. For either scenario, the ratio of warm/cool component temperatures is indicative of the scale of outer planetary systems, which typically span a factor of about ten in radius.

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30

MELITA, M., J. LARWOOD, and I. WILLIAMS. "Sculpting the outer Edgeworth?Kuiper belt: stellar encounter followed by planetary perturbations." Icarus 173, no. 2 (February 2005): 559–73. http://dx.doi.org/10.1016/j.icarus.2004.08.020.

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31

Stern, S. Alan, and Joshua E. Colwell. "Collisional Erosion in the Primordial Edgeworth‐Kuiper Belt and the Generation of the 30–50 AU Kuiper Gap." Astrophysical Journal 490, no. 2 (December 1997): 879–82. http://dx.doi.org/10.1086/304912.

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32

Orosei, R., A. Coradini, M. C. De Sanctis, and C. Federico. "Collision-induced thermal evolution of a comet nucleus in the Edgeworth-Kuiper Belt." Advances in Space Research 28, no. 10 (January 2001): 1563–69. http://dx.doi.org/10.1016/s0273-1177(01)00362-3.

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33

Liou, Jer-Chyi, and Herbert A. Zook. "Signatures of the Giant Planets Imprinted on the Edgeworth-Kuiper Belt Dust Disk." Astronomical Journal 118, no. 1 (July 1999): 580–90. http://dx.doi.org/10.1086/300938.

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34

Collander-Brown, S., M. Maran, and I. P. Williams. "The effect on the Edgeworth-Kuiper Belt of a large distant tenth planet." Monthly Notices of the Royal Astronomical Society 318, no. 1 (October 11, 2000): 101–8. http://dx.doi.org/10.1046/j.1365-8711.2000.03640.x.

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35

Ichikawa, Kazuhide, and Masataka Fukugita. "MICROWAVE EMISSION FROM THE EDGEWORTH-KUIPER BELT AND THE ASTEROID BELT CONSTRAINED FROM THEWILKINSON MICROWAVE ANISOTROPY PROBE." Astrophysical Journal 736, no. 2 (July 15, 2011): 122. http://dx.doi.org/10.1088/0004-637x/736/2/122.

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36

Ida, Shigeru, John Larwood, and Andreas Burkert. "Evidence for Early Stellar Encounters in the Orbital Distribution of Edgeworth–Kuiper Belt Objects." Astrophysical Journal 528, no. 1 (January 2000): 351–56. http://dx.doi.org/10.1086/308179.

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37

Poppe, A. R. "The contribution of Centaur-emitted dust to the interplanetary dust distribution." Monthly Notices of the Royal Astronomical Society 490, no. 2 (October 9, 2019): 2421–29. http://dx.doi.org/10.1093/mnras/stz2800.

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ABSTRACT Interplanetary dust grains originate from a variety of source bodies, including comets, asteroids, and Edgeworth–Kuiper belt objects. Centaurs, generally defined as those objects with orbits that cross the outer planets, have occasionally been observed to exhibit cometary-like outgassing at distances beyond Jupiter, implying that they may be an important source of dust grains in the outer Solar system. Here, we use an interplanetary dust grain dynamics model to study the behaviour and equilibrium distribution of Centaur-emitted interplanetary dust grains. We focus on the five Centaurs with the highest current mass-loss rates: 29P/Schwassmann-Wachmann 1, 166P/2001 T4, 174P/Echeclus, C/2001 M10, and P/2004 A1, which together comprise 98 per cent of the current mass loss from all Centaurs. Our simulations show that Centaur-emitted dust grains with radii s < 2 μm have median lifetimes consistent with Poynting–Robertson (P–R) drag lifetimes, while grains with radii s > 2 μm have median lifetimes much shorter than their P–R drag lifetimes, suggesting that dynamical interactions with the outer planets are effective in scattering larger grains, in analogy to the relatively short lifetimes of Centaurs themselves. Equilibrium density distributions of grains emitted from specific Centaurs show a variety of structure including local maxima in the outer Solar system and azimuthal asymmetries, depending on the orbital elements of the parent Centaur. Finally, we compare the total Centaur interplanetary dust density to dust produced from Edgeworth–Kuiper belt objects, Jupiter-family comets, and Oort cloud comets, and conclude that Centaur-emitted dust may be an important component between 5 and 15 au, contributing approximately 25 per cent of the local interplanetary dust density at Saturn.

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38

Yamamoto, Naotaka, Daisuke Kinoshita, Tetsuharu Fuse, Jun-ichi Watanabe, and Kiyoshi Kawabata. "A Deep Sky Survey of Edgeworth Kuiper Belt Objects with an Improved Shift-and-Add Method." Publications of the Astronomical Society of Japan 60, no. 2 (April 25, 2008): 285–91. http://dx.doi.org/10.1093/pasj/60.2.285.

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39

Han, Dong, Andrew R. Poppe, Marcus Piquette, Eberhard Grün, and Mihály Horányi. "Constraints on dust production in the Edgeworth-Kuiper Belt from Pioneer 10 and New Horizons measurements." Geophysical Research Letters 38, no. 24 (December 28, 2011): n/a. http://dx.doi.org/10.1029/2011gl050136.

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40

ENCRENAZ, THÉRÈSE. "The formation and evolution of the Solar System." European Review 10, no. 2 (May 2002): 171–84. http://dx.doi.org/10.1017/s1062798702000133.

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Astronomers have built the main components of a scenario for the formation of the Solar System. Small planetary bodies accreted others by collisions within a rotating protoplanetary disk that formed at the same time as the Sun. While terrestrial planets near the warming Sun could accumulate only solid metallic and silicate material, the giant planets formed from ice and gas at lower temperatures. Each planet and satellite then followed its own specific evolution, depending upon the properties of its atmosphere and/or surface. Information about the origin and evolution of the Solar System is also provided by the comets, which can be considered as frozen fossils of the Solar System's early stages. On the borders of the outer Solar System, beyond the orbit of Neptune, the newly discovered Edgeworth–Kuiper belt is probably the reservoir where short-period comets are formed.

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41

Poppe, A. R., C. M. Lisse, M. Piquette, M. Zemcov, M. Horányi, D. James, J. R. Szalay, E. Bernardoni, and S. A. Stern. "Constraining the Solar System's Debris Disk with In Situ New Horizons Measurements from the Edgeworth–Kuiper Belt." Astrophysical Journal 881, no. 1 (August 7, 2019): L12. http://dx.doi.org/10.3847/2041-8213/ab322a.

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42

Stern, S. Alan, and Joshua E. Colwell. "Accretion in the Edgeworth-Kuiper Belt: Forming 100-1000 KM Radius Bodies at 30 AU and Beyond." Astronomical Journal 114 (August 1997): 841. http://dx.doi.org/10.1086/118518.

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43

Marov, Mikhail, and Sergei Ipatov. "Migration Processes and Volatiles Delivery." Symposium - International Astronomical Union 213 (2004): 295–98. http://dx.doi.org/10.1017/s007418090019343x.

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Migration processes of comets and asteroids from the outer regions of the solar system, including the Edgeworth–Kuiper belt, are regarded as important mechanisms for the formation and evolution of the inner planets. These minor bodies may be responsible for the delivery of volatile matter to the inner planets and thus be responsible for the origin of life. We estimate that the cumulative mass of icy comets impacting on the Earth during the formation of the giant planets is similar to the mass of water in the Earth oceans, and that Mars acquired more water per unit planet mass than Earth. We find that these cometary objects mostly evolved from typical near-Earth orbits and Encke-type orbits with aphelia located inside the orbit of Jupiter, and played a greater role than those with Jupiter-crossing orbits. The relative importance of comets and chondrites in the delivery of volatiles is constrained by the observed fractionation patterns of atmospheric noble gas abundance.

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44

Brunini, A. "The Existence of a Planet beyond 50 AU and the Orbital Distribution of the Classical Edgeworth–Kuiper-Belt Objects." Icarus 160, no. 1 (November 2002): 32–43. http://dx.doi.org/10.1006/icar.2002.6935.

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45

Krivov, Alexander V., Miodrag Sremčević, and Frank Spahn. "Evolution of a Keplerian disk of colliding and fragmenting particles: a kinetic model with application to the Edgeworth–Kuiper belt." Icarus 174, no. 1 (March 2005): 105–34. http://dx.doi.org/10.1016/j.icarus.2004.10.003.

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46

Toth, I. "On the Detectability of Satellites of Small Bodies Orbiting the Sun in the Inner Region of the Edgeworth–Kuiper Belt." Icarus 141, no. 2 (October 1999): 420–25. http://dx.doi.org/10.1006/icar.1999.6189.

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47

Poppe, A. R., C. M. Lisse, M. Piquette, M. Zemcov, M. Horányi, D. James, J. R. Szalay, E. Bernardoni, and S. A. Stern. "Erratum: “Constraining the Solar System's Debris Disk with In Situ New Horizons Measurements from the Edgeworth-Kuiper Belt” (2019, ApJL, 881, L12)." Astrophysical Journal 882, no. 1 (September 3, 2019): L14. http://dx.doi.org/10.3847/2041-8213/ab3c6f.

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48

Palumbo, M. E., and G. Strazzulla. "Nitrogen condensation on water ice." Canadian Journal of Physics 81, no. 1-2 (January 1, 2003): 217–24. http://dx.doi.org/10.1139/p03-037.

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We studied, by infrared absorption spectroscopy, icy samples (16 K) of pure water, a mixture N2:H2O=100:1, and a sample made of N2 condensed on water ice and diffused in it after warm up to 30 K. We concentrated our efforts in two spectral regions around 3700 cm1 where the feature due to the OH dangling bonds in porous amorphous water falls and around 5000 cm1 where a broad water band is present. We found that in the N2:H2=100:1 mixture the profile of the broad water feature at about 5000 cm1 dramatically changed to a very narrow band at about 5300 cm1. When N2 diffuses in water ice a feature at about 5300 cm1 appears along with the broad 5000 cm1 band. We also studied some of the effects of ion irradiation (Ar++, 60 keV ions) on these icy samples. We found that after processing the feature due to the OH dangling bonds it reduced in intensity and eventually disappeared. Here we present the experimental results, discuss their astrophysical relevance and suggest that a band at about 5300 cm1 (1.88 µm) should be searched for on icy surfaces in the outer Solar System, namely Pluto, Triton, EdgeworthKuiper Belt Objects, and Centaurs. PACS No.: 68.43Pg

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49

Doressoundiram, A., N. Peixinho, C. de Bergh, S. Fornasier, P. Thébault, M. A. Barucci, and C. Veillet. "Erratum: “The Color Distribution in the Edgeworth-Kuiper Belt” [[URL ADDRESS="/cgi-bin/resolve?2002AJ....124.2279D" STATUS="OKAY"]Astron. J. [BF]124[/BF], 2279 (2002)[/URL]]." Astronomical Journal 125, no. 3 (March 2003): 1629–30. http://dx.doi.org/10.1086/375497.

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50

Horner, J., and B. W. Jones. "Jupiter – friend or foe? II: the Centaurs." International Journal of Astrobiology 8, no. 2 (December 24, 2008): 75–80. http://dx.doi.org/10.1017/s1473550408004357.

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AbstractIt has long been assumed that the planet Jupiter acts as a giant shield, significantly lowering the impact rate of minor bodies upon the Earth, and thus enabling the development and evolution of life in a collisional environment which is not overly hostile. In other words, it is thought that, thanks to Jupiter, mass extinctions have been sufficiently infrequent that the biosphere has been able to diversify and prosper. However, in the past, little work has been carried out to examine the validity of this idea. In the second of a series of papers, we examine the degree to which the impact risk resulting from objects on Centaur-like orbits is affected by the presence of a giant planet, in an attempt to fully understand the impact regime under which life on Earth has developed. The Centaurs are a population of ice-rich bodies which move on dynamically unstable orbits in the outer Solar system. The largest Centaurs known are several hundred kilometres in diameter, and it is certain that a great number of kilometre or sub-kilometre sized Centaurs still await discovery. These objects move on orbits which bring them closer to the Sun than Neptune, although they remain beyond the orbit of Jupiter at all times, and have their origins in the vast reservoir of debris known as the Edgeworth–Kuiper belt that extends beyond Neptune. Over time, the giant planets perturb the Centaurs, sending a significant fraction into the inner Solar System where they become visible as short-period comets. In this work, we obtain results which show that the presence of a giant planet can act to significantly change the impact rate of short-period comets on the Earth, and that such planets often actually increase the impact flux greatly over that which would be expected were a giant planet not present.

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