Forming Binary Near-Earth Asteroids From Tidal Disruptions

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A Parameter Tests 113A.1 Bulk Density of Progenitor . . . . . . . . . . . . . . . . . . . . . . . . . 113A.2 Resolution of Progenitor . . . . . . . . . . . . . . . . . . . . . . . . . . 115A.3 Packing Efficiency of Progenitor . . . . . . . . . . . . . . . . . . . . . . 116A.4 Conclusions on Parameter Tests . . . . . . . . . . . . . . . . . . . . . . 118Bibliography 121vii
List of Tables1.1 Binary NEA properties. . . . . . . . . . . . . . . . . . . . . . . . . . . . 51.2 Binary MBA properties. . . . . . . . . . . . . . . . . . . . . . . . . . . 112.1 Binary formation statistics. . . . . . . . . . . . . . . . . . . . . . . . . . 333.1 Diameter estimates from H. . . . . . . . . . . . . . . . . . . . . . . . . . 593.2 Orbital, physical and lightcurve parameters for all targets. . . . . . . . . . 684.1 Lifetimes for binary NEAs. . . . . . . . . . . . . . . . . . . . . . . . . 904.2 Binary fractions for all simulations. . . . . . . . . . . . . . . . . . . . . 103A.1 Number of binaries produced at varying resolutions. . . . . . . . . . . . 116viii
Page 1 and 2: AbstractTitle of Dissertation:Formi
Page 3 and 4: Forming Binary Near-Earth Asteroids
Page 5 and 6: PrefaceMuch of the work in this dis
Page 7 and 8: AcknowledgementsI would not have ma
Page 9: 2.3 Results and Discussion . . . .
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
Page 53 and 54: various complications of measuring
Page 55 and 56: etween ω pri and L bin ), with clo
Page 57 and 58: prolate-like), the oblate-like bodi
Page 59 and 60: Figure 2.9: Plots comparing T-PROS
Page 61 and 62:
Figure 2.10: Comparison of S-class
Page 63 and 64:
2.3.5 Triples and hierarchical syst
Page 65 and 66:
a/R pri based on a simple conversio
Page 67 and 68:
Figure 2.13: The eccentricity dampi
Page 69 and 70:
Main Belt. Work by Chauvineau & Far
Page 71 and 72:
(1992), with a target range of slig
Page 73 and 74:
The observations were made from the
Page 75 and 76:
peaked period, with a lower signifi
Page 77 and 78:
and suggests that it is possibly a
Page 79 and 80:
fit for the period of the lightcurv
Page 81 and 82:
Table 3.2.Orbital, physical and lig
Page 83 and 84:
Figure 3.2: Asteroid lightcurves.70
Page 85 and 86:
Figure 3.4: Asteroid lightcurves.72
Page 87 and 88:
3.4.4 Spin and shape properties amo
Page 89 and 90:
Figure 3.7: The lightcurve amplitud
Page 91 and 92:
Typically observations of eclipse o
Page 93 and 94:
Chapter 4Steady-State Model of the
Page 95 and 96:
values between 0.2-0.6. There is on
Page 97 and 98:
asteroids in the Main Belt is suffi
Page 99 and 100:
Figure 4.2: Percent of surviving NE
Page 101 and 102:
4.1.3 Binary evolutionBasic stabili
Page 103 and 104:
Table 4.1.Lifetimes for binary NEAs
Page 105 and 106:
which means it should have a critic
Page 107 and 108:
Figure 4.4: The total number of bin
Page 109 and 110:
the original eccentricity distribut
Page 111 and 112:
Figure 4.6: Properties of the binar
Page 113 and 114:
Figure 4.8: Binary percentage for m
Page 115 and 116:
Figure 4.9: Effects of tidal evolut
Page 117 and 118:
quickly altered, or involved in bin
Page 119 and 120:
tidal disruption. However, the impl
Page 121 and 122:
Chapter 5ConclusionsA general concl
Page 123 and 124:
small additions to the angular mome
Page 125 and 126:
cently this large pool of observers
Page 127 and 128:
differences in results when a lower
Page 129 and 130:
Table A.1.Number of binaries produc
Page 131 and 132:
Thus the reaccumulated bodies in th
Page 133 and 134:
of 2.2 h observed is significantly
Page 135 and 136:
Benner, L. A. M., Nolan, M. C., Ost
Page 137 and 138:
V7.0:LCREF TAB, 35, 4Harris, A. W.,
Page 139 and 140:
Storrs, A. D., Close, L. M., & Mena
Page 141 and 142:
122Pravec, P., Kušnirá, P., Hicks
Page 143 and 144:
Shepard, M. K., Schlieder, J., Nola
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Forming Binary Near-Earth Asteroids From Tidal Disruptions

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