INITIAL PLANETESIMAL SIZES AND THE SIZE DISTRIBUTION OF SMALL KUIPER BELT OBJECTS

We show, by comparing observations with theoretical models, that the observed Kuiper Belt size distribution is well matched by coagulation models, which start with an initial planetesimal population with radii of about 1 km, and subsequent collisional evolution. We find that the observed size distri...

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Bibliographic Details
Published in:The Astronomical journal 2013-08, Vol.146 (2), p.1-7
Main Authors: Schlichting, Hilke E, Fuentes, Cesar I, Trilling, David E
Format: Article
Language:English
Subjects:
Astronomical instruments
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
COLLISIONS
COMETS
DISTRIBUTION
ECLIPSE
EQUILIBRIUM
Evolution
GROWTH
Kuiper belt
LAWS
LEAVES
LIMITING VALUES
MASS
Occultation
Planet formation
PLANETS
PROTOPLANETS
SATELLITES
Size distribution
Slopes
SOLAR SYSTEM
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Summary:We show, by comparing observations with theoretical models, that the observed Kuiper Belt size distribution is well matched by coagulation models, which start with an initial planetesimal population with radii of about 1 km, and subsequent collisional evolution. We find that the observed size distribution above R ~ 30 km is primordial, i.e., it has not been modified by collisional evolution over the age of the solar system, and that the size distribution below R ~ 30 km has been modified by collisions and that its slope is well matched by collisional evolution models that use published strength laws. We find that results from recent KBO occultation surveys and the observed KBO size distribution can be best matched by an initial planetesimal population that contained about equal mass per logarithmic mass bin in bodies ranging from 0.4 km to 4 km in radius.
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.1088/0004-6256/146/2/36