- Page 1: AbstractTitle of Dissertation:Formi
- Page 5 and 6: PrefaceMuch of the work in this dis
- Page 7 and 8: AcknowledgementsI would not have ma
- Page 9 and 10: 2.3 Results and Discussion . . . .
- Page 11 and 12: List of Tables1.1 Binary NEA proper
- Page 13 and 14: 4.8 Percentage of migrated binaries
- Page 15 and 16: of the system mass M by way of Kepl
- Page 17 and 18: the largest lightcurve amplitudes o
- Page 19 and 20: 1.1.3 Binary Main-Belt asteroidsRec
- Page 21 and 22: Lightcurve discoveriesA lightcurve
- Page 23 and 24: Figure 1.1: (Top) The primary rotat
- Page 25 and 26: 1.2.1 CaptureIn this scenario two a
- Page 27 and 28: ever, understanding the mechanism i
- Page 29 and 30: off the equator or off one end of a
- Page 31 and 32: 3 Denotes a secure result with no a
- Page 33 and 34: nostic.Recent results have demonstr
- Page 35 and 36: another intermediate source of NEAs
- Page 37 and 38: 1.5.2 Rubble pilesThe evidence for
- Page 39 and 40: Chapter 2Formation of Binary Astero
- Page 41 and 42: ∼ 60%, making a bulk density of
- Page 43 and 44: shedding mass and distorting prior
- Page 45 and 46: Figure 2.3: Snapshots of a tidal di
- Page 47 and 48: Figure 2.4: Normalized probability
- Page 49 and 50: Figure 2.5: Normalized probability
- Page 51 and 52: Figure 2.6: (a) Satellite eccentric
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various complications of measuring
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etween ω pri and L bin ), with clo
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prolate-like), the oblate-like bodi
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Figure 2.9: Plots comparing T-PROS
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Figure 2.10: Comparison of S-class
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2.3.5 Triples and hierarchical syst
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a/R pri based on a simple conversio
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Figure 2.13: The eccentricity dampi
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Main Belt. Work by Chauvineau & Far
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(1992), with a target range of slig
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The observations were made from the
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peaked period, with a lower signifi
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and suggests that it is possibly a
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fit for the period of the lightcurv
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Table 3.2.Orbital, physical and lig
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Figure 3.2: Asteroid lightcurves.70
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Figure 3.4: Asteroid lightcurves.72
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3.4.4 Spin and shape properties amo
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Figure 3.7: The lightcurve amplitud
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Typically observations of eclipse o
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Chapter 4Steady-State Model of the
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values between 0.2-0.6. There is on
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asteroids in the Main Belt is suffi
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Figure 4.2: Percent of surviving NE
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4.1.3 Binary evolutionBasic stabili
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Table 4.1.Lifetimes for binary NEAs
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which means it should have a critic
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Figure 4.4: The total number of bin
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the original eccentricity distribut
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Figure 4.6: Properties of the binar
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Figure 4.8: Binary percentage for m
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Figure 4.9: Effects of tidal evolut
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quickly altered, or involved in bin
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tidal disruption. However, the impl
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Chapter 5ConclusionsA general concl
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small additions to the angular mome
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cently this large pool of observers
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differences in results when a lower
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Table A.1.Number of binaries produc
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Thus the reaccumulated bodies in th
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of 2.2 h observed is significantly
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Benner, L. A. M., Nolan, M. C., Ost
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V7.0:LCREF TAB, 35, 4Harris, A. W.,
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Storrs, A. D., Close, L. M., & Mena
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122Pravec, P., Kušnirá, P., Hicks
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Shepard, M. K., Schlieder, J., Nola