Question: What Canadian astronomer born in 1963 studied minor planets of the solar system?

Context articles: Korado Korlević
List of exceptional asteroids
Asteroid
Lost minor planet
Asteroid belt
David J. Lane (astronomer)
Jumping-Jupiter scenario
Nice model
List of unnumbered minor planets
List of minor planets

Korado Korlević (born on 19 September 1958 in Poreč) is a Croatian teacher and prolific amateur astronomer, who ranks among the world's top 20 discoverers of minor planets.
 As of 2016, he is credited by the Minor Planet Center with the discovery of 1162 numbered minor planets he made at Višnjan Observatory during 1996–2001.
 In addition, he is credited with the co-discovery of another 132 minor planets.
 His discoveries include the slowly-rotating outer main-belt asteroid 10415 Mali Lošinj, and 10645 Brač, a member of the Eunomia family of asteroids.
 He has also discovered two comets, namely 183P/Korlević-Jurić and 203P/Korlević.
The following is a collection of lists of exceptional asteroids in the Solar System.
 For the purposes of this article "asteroid" means minor planet up to the orbit of Jupiter, which includes the dwarf planet Ceres.
 For a complete list of minor planets in numerical order, see List of minor planets.
Asteroids are minor planets, especially those of the inner Solar System.
 The larger ones have also been called planetoids.
 These terms have historically been applied to any astronomical object orbiting the Sun that did not show the disc of a planet and was not observed to have the characteristics of an active comet.
 As minor planets in the outer Solar System were discovered and found to have volatile-based surfaces that resemble those of comets, they were often distinguished from asteroids of the asteroid belt.
 In this article, the term "asteroid" refers to the minor planets of the inner Solar System including those co-orbital with Jupiter.
Lost minor planets are minor planets that observers lose track of due to too short an observation arc to accurately predict the future location of the minor planet.
 Many of the asteroids that were discovered early were lost and rediscovered in the 1980s and 1990s, but a number of minor planets continue to be lost.
 By some definitions, thousands, if not tens of thousands observed minor planets are lost—they cannot be found by pointing an appropriate telescope at their predicted location, because the uncertainty in their predicted orbit is too large or they are currently too faint to be detected.
The asteroid belt is the circumstellar disc in the Solar System located roughly between the orbits of the planets Mars and Jupiter.
 It is occupied by numerous irregularly shaped bodies called asteroids or minor planets.
 The asteroid belt is also termed the main asteroid belt or main belt to distinguish it from other asteroid populations in the Solar System such as near-Earth asteroids and trojan asteroids.
 About half the mass of the belt is contained in the four largest asteroids: Ceres, Vesta, Pallas, and Hygiea.
 The total mass of the asteroid belt is approximately 4% that of the Moon, or 22% that of Pluto, and roughly twice that of Pluto's moon Charon (whose diameter is 1200 km).
David J. Lane (born 1963) is a Canadian astronomer at Saint Mary's University, the past president of the Royal Astronomical Society of Canada, director of the Burke-Gaffney astronomical observatory, owner of the Abbey-Ridge Observatory, and creator of the planetarium software entitled the "Earth Centered Universe".
 Asteroid 117032 Davidlane is named in his honour, and the asteroid lies in the main asteroid belt between Mars and Jupiter.
The jumping-Jupiter scenario specifies an evolution of giant-planet migration described by the Nice model, in which an ice giant (Uranus, Neptune, or an additional Neptune-mass planet) is scattered inward by Saturn and outward by Jupiter, causing the step-wise separation of their orbits.
 The jumping-Jupiter scenario was proposed by Ramon Brasser, Alessandro Morbidelli, Rodney Gomes, Kleomenis Tsiganis, and Harold Levison after their studies revealed that the smooth divergent migration of Jupiter and Saturn resulted in an inner Solar System significantly different from the current Solar System.
 The sweeping of secular resonances through the inner Solar System during the migration excited the eccentricities of the terrestrial planets beyond current values and left an asteroid belt with an excessive ratio of high- to low-inclination objects.
 The step-wise separation of Jupiter and Saturn described in the jumping-Jupiter scenario can allow these resonances to quickly cross the inner Solar System without altering orbits excessively, although the terrestrial planets remain sensitive to its passage.
 The jumping-Jupiter scenario also results in a number of other differences with the original Nice model.
 The fraction of lunar impactors from the core of the asteroid belt during the Late Heavy Bombardment is significantly reduced, most of the Jupiter trojans are captured during Jupiter's encounters with the ice giant, as are Jupiter's irregular satellites.
 In the jumping-Jupiter scenario, the likelihood of preserving four giant planets on orbits resembling their current ones appears to increase if the early Solar System originally contained an additional ice giant, which was later ejected by Jupiter into interstellar space.
 However, this remains an atypical result, as is the preservation of the current orbits of the terrestrial planets.
The Nice ( ) model is a scenario for the dynamical evolution of the Solar System.
 It is named for the location of the Observatoire de la Côte d'Azur, where it was initially developed, in Nice, France.
 It proposes the migration of the giant planets from an initial compact configuration into their present positions, long after the dissipation of the initial protoplanetary gas disk.
 In this way, it differs from earlier models of the Solar System's formation.
 This planetary migration is used in dynamical simulations of the Solar System to explain historical events including the Late Heavy Bombardment of the inner Solar System, the formation of the Oort cloud, and the existence of populations of small Solar System bodies including the Kuiper belt, the Neptune and Jupiter trojans, and the numerous resonant trans-Neptunian objects dominated by Neptune.
 Its success at reproducing many of the observed features of the Solar System means that it is widely accepted as the current most realistic model of the Solar System's early evolution, although it is not universally favoured among planetary scientists.
 Later research revealed a number of differences between the original Nice model's predictions and observations of the current Solar System, for example the orbits of the terrestrial planets and the asteroids, leading to its modification.
This is a partial list of unnumbered minor planets, which are provisionally designated minor planets with a poorly determined orbit, not cataloged in the list of (numbered) minor planets "(see index)", due to insufficient observational data.
 This also include lost minor planets which have not been observed for many years, or even decades.
 As of July 2017, and according to the Minor Planet Center's statistic, there are 237,459 or 32.3% unnumbered minor planets (uMPs) of a total of 734,274.
 The displayed data for this and other partial lists, however, are sourced from JPL's data base on small Solar bodies, which may slightly differ.
This is a list of numbered minor planets in the Solar System, in numerical order.
 s of 2017 there are 496,815 numbered minor planets, and 237,441 unnumbered.
 Only 21,009 or approximately 4% of all numbered minor planets are currently named, mostly for people and figures from mythology and fiction.
 The Jupiter trojan is currently the lowest-numbered unnamed minor planet.
 Minor planets also include dwarf planets of which 5 have been officially recognized by the IAU with potentially hundreds more to follow in the future.