Forming Binary Near-Earth Asteroids From Tidal Disruptions

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and its axis orientation and therefore should operate at different timescales on the NEAand MBA populations. The scenario for successfully losing mass while retaining somein a stable orbit is unknown, but small separations and fast spinning primaries are likelyresulting properties, making this the most likely mechanism to supply the large percentageof observed binaries.107
Chapter 5ConclusionsA general conclusion to this entire work is that tidal disruption is not a sufficient formationmechanism to create the observed binary NEAs. More specifically, in Section 1.6 threequestions were posed to be answered in this dissertation, and each in turn was answeredin the following chapters.What are the properties of tidal-disruption-formed binaries and how do they compareto the observed NEA and MBA binaries? The semi-major axis distribution is stronglypeaked below 10 R pri , with about half of the binaries with larger separations. The simulationsdo produce systems similar to the observed binaries, as all observed NEA binarieshave semi-major axes less than 10 R pri , with the majority below 5 R pri . The size ratios arepeaked between R sec /R pri = 0.1–0.2. Similar to the observed population, few systems aremade with equal sized components. The simulations produced a tight bracket of primaryrotation rates between 4–6 h. The observed NEA binaries are similarly bracketed, but ata more rapid rotation rate between 2.2–3.5 h.What is the spin and shape distribution for small MBAs? Small MBAs appear to havea distribution of shape and spin most similar to that of MBAs with D < 20 km. NEAsgenerally have an excess of rapid rotators not observed among the small MBAs.108
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AbstractTitle of Dissertation:Formi
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Forming Binary Near-Earth Asteroids
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PrefaceMuch of the work in this dis
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AcknowledgementsI would not have ma
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2.3 Results and Discussion . . . .
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List of Tables1.1 Binary NEA proper
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4.8 Percentage of migrated binaries
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of the system mass M by way of Kepl
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the largest lightcurve amplitudes o
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1.1.3 Binary Main-Belt asteroidsRec
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Lightcurve discoveriesA lightcurve
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Figure 1.1: (Top) The primary rotat
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1.2.1 CaptureIn this scenario two a
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ever, understanding the mechanism i
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off the equator or off one end of a
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3 Denotes a secure result with no a
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nostic.Recent results have demonstr
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another intermediate source of NEAs
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1.5.2 Rubble pilesThe evidence for
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Chapter 2Formation of Binary Astero
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∼ 60%, making a bulk density of
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shedding mass and distorting prior
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Figure 2.3: Snapshots of a tidal di
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Figure 2.4: Normalized probability
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Figure 2.5: Normalized probability
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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
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
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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: tidal disruption. However, the impl
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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