WorldCat Identities

Kavelaars, J. J. 1966-

Works: 8 works in 8 publications in 1 language and 13 library holdings
Roles: Author, Thesis advisor
Publication Timeline
Most widely held works by J. J Kavelaars
Ultra-wide Trans-Neptunian Binaries : tracers of the outer solar system's history by Alex Harrison Parker( )

1 edition published in 2011 in English and held by 4 WorldCat member libraries worldwide

Ultra-wide Trans-Neptunian Binaries (TNBs) are extremely sensitive to perturbation, and therefore make excellent probes of the past and present dynamical environment of the outer Solar System. Using data gathered from a host of facilities we have determined the mutual orbits for a sample of seven wide TNBs whose periods exceed one year. This characterized sample provides us with new information about the probable formation scenarios of TNBs, and has significant implications for the early dynamical and collisional history of the Kuiper Belt. We show that these wide binaries have short collisional lifetimes, and use them to produce a new estimate of the number of small (~1 km) objects in the Kuiper Belt. Additionally, these systems are susceptible to tidal disruption, and we show that it is unlikely that they were ever subjected to a period of close encounters with the giant planets. We find that the current properties of these ultra-wide Trans-Neptunian Binaries suggest that planetesimal growth in the Cold Classical Kuiper Belt did not occur through slow hierarchical accretion, but rather through rapid gravitational collapse
A photometric study of globular cluster NGC 6517 by J. J Kavelaars( Book )

1 edition published in 1993 in English and held by 2 WorldCat member libraries worldwide

On the population of the 5:1 Neptune resonance by Rosemary Ellen Pike( )

1 edition published in 2016 in English and held by 2 WorldCat member libraries worldwide

The recent discovery of objects near the 5:1 Neptune resonance prompts the study of the size, structure, and surface properties of this population to determine if these parameters are consistent with a ©Nice model' type evolution of the outer Solar System. Previous TNO discovery surveys have primarily targeted the ecliptic plane, where discovery of high inclination objects such as the 5:1 resonators is unlikely, and theoretical work on the evolution of the outer Solar System has focused on structure in and around the main Kuiper belt and largely ignored the distant resonant TNOs. I tracked these objects for several semesters, measured their positions accurately, and determined precise orbits. Integrating these orbits forward in time revealed that three objects are 5:1 resonators, and one object is not resonant but may have been resonant in the past. I constrained the structure of the 5:1 resonance population based on the three detections and determined that the minimum population in this resonance was much larger than expected, 1900(+3300,-1400) with H <8. I compared this large population with the orbital distribution of TNOs resulting from a Nice model evolution and determined that the population in the real 5:1 resonance is ~20-100 times larger than the model predicts. However, the structure of the 5:1 resonance in this model was consistent with the orbital distribution I determined based on the detections. The orbital distribution of the scattering population in the Nice model is consistent with other models and survey results, leading to the conclusion that the 5:1 resonance cannot be a steady state transient population produced via resonance sticking from the scattering objects. To test the origin of the 5:1 resonators, I measured the objects' surface colors in multiple wavelength ranges and compared their surface reflectance to TNOs from a large color survey, ColOSSOS. The 5:1 resonators have a consistent selection criteria to the TNOs from the ColOSSOS survey, so these samples have known selection biases and can be usefully compared to each other. The surfaces of the three 5:1 resonators showed three different spectral reflectance shapes, indicating that these three objects do not share a common formation location. The surface properties and orbital distribution of current 5:1 resonators are consistent with the remnant of a large captured population, partially resupplied by the scattering objects. However, the scattering event which produced this large 5:1 population remains unexplained
The Kuiper belt size distribution : constraints on accretion by Wesley Christopher Fraser( )

1 edition published in 2008 in English and held by 2 WorldCat member libraries worldwide

The Kuiper belt is a population of planetesimals outside the orbit of Neptune. The high inclinations and eccentricities exhibited by many belt members, and its very low mass (M 0.1M) present an enigma to planetesimal accretion scenarios: the high relative encounter velocities (vrei 1 km s-1), and infrequent collisions of the largest members make the growth of Pluto-sized bodies impossible over the age of the Solar system. Accretion in the early stages of planet-building must have been in a more dense environment allowing large objects to grow before growth was halted. The current Kuiper belt population is the left-over relic of accretion, which has undergone collisional re-shaping since the epoch of accretion. The shape of the size distribution can provide constraint on the accretion timescale, the primordial Kuiper belt mass, and the collisional processing the belt has undergone. Thus, a measure of the size distribution provides one of the primary constraint on models which attempt to explain the formation of the Kuiper belt. We have performed a large-scale ecliptic Kuiper belt survey, with an aerial coverage of 3.3 square degrees to a limiting magnitude m(R) 27. From these observations, we have discovered more than 100 new Kuiper belt objects. Using this survey we have provided the best measurement of the Kuiper belt luminosity function to-date, from which we have inferred the size distribution. We have found that the size distribution is well described by a power-law for large objects with a steep slope q1 = 4.8, that breaks, or rolls over to a shallower power-law with slope q2 = 2 at object diameter ~ 60 km. The steep large object slope is indicative of a short accretion phase, lasting no more than a few 100 Myr. The large break diameter demonstrates that the Kuiper belt has undergone substantial collisional processing. We have developed a collisional evolution model which we have used to study the effects of planetesimal bombardment and disruption on the size distribution. We have found that, in the current Kuiper belt, little to no evolution is occurring, or has occurred for the observable Kuiper belt. We conclude that the large break diameter cannot be produced in the current environment over the age of the Solar system. A period of intense collisional evolution in a much more dense, and hence, more massive belt is required. These findings are consistent with accretion models; the typical finding is that growth of the largest Kuiper belt objects over the age of the Solar system requires a much more massive belt than currently observed. These results point to a history in which an initially much more massive Kuiper belt underwent a short period of quiescent accretion producing Pluto size bodies. Some event then occurred, which dynamically excited the planetesimals, producing an erosive environment which effectively halted planet growth and rapidly depleted the majority of the primordial mass. The remnant of this depletion is the Kuiper belt we observe today
Globular clusters as dynamical probes of the SO galaxy NGC 3115 by J. J Kavelaars( Book )

1 edition published in 1997 in English and held by 1 WorldCat member library worldwide

Globular clusters as dynamical probes of the S0 galaxy NGC 3115 by J. J Kavelaars( Book )

1 edition published in 1999 in English and held by 1 WorldCat member library worldwide

A search for binary Kuiper belt objects in the CFEPS Samples by Shengwen Lin( Book )

1 edition published in 2008 in English and held by 1 WorldCat member library worldwide

Discovery of 12 satellites of saturn exhibiting orbital clustering by Brett J Gladman( )

1 edition published in 2001 in English and held by 0 WorldCat member libraries worldwide

Audience Level
Audience Level
  Kids General Special  
Audience level: 0.81 (from 0.73 for Globular c ... to 1.00 for Discovery ...)

Alternative Names
John J. Kavelaars born 1966; Canadian astronomer

John J. Kavelaars Canadees astronoom

John J. Kavelaars canadisk astronom

John J. Kavelaars kanadensisk astronom

John J. Kavelaars kanadischer Astronom

John J. Kavelaars kanadisk astronom

John Kavelaars astronomo canadese

Кавеларс, Джон

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