Forming Binary Near-Earth Asteroids From Tidal Disruptions

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List of Figures1.1 Binary NEA and MBA properties. . . . . . . . . . . . . . . . . . . . . . 102.1 Initial spin and shape parameters. . . . . . . . . . . . . . . . . . . . . . . 292.2 Distribution of v ∞ for NEA close encounters. . . . . . . . . . . . . . . . 312.3 Snapshots of a tidal disruption. . . . . . . . . . . . . . . . . . . . . . . . 322.4 Probability of binary formation for each parameter. . . . . . . . . . . . . 342.5 Binaries formed compared to mass of the largest remnant. . . . . . . . . . 362.6 Binary orbital properties. . . . . . . . . . . . . . . . . . . . . . . . . . . 382.7 Binary size ratio, obliquity and spin period. . . . . . . . . . . . . . . . . 412.8 Primary body shape statistics. . . . . . . . . . . . . . . . . . . . . . . . . 432.9 T-PROS and T-EEBs . . . . . . . . . . . . . . . . . . . . . . . . . . . . 462.10 Comparison of S-, B-, and M-class disruptions. . . . . . . . . . . . . . . 482.11 Spin periods of 3 h spin subset. . . . . . . . . . . . . . . . . . . . . . . . 492.12 Tidal evolution of semi-major axis. . . . . . . . . . . . . . . . . . . . . . 532.13 Eccentricity damping timescales. . . . . . . . . . . . . . . . . . . . . . . 543.1 Lightcurve plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 693.2 Lightcurve plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 703.3 Lightcurve plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 713.4 Lightcurve plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 723.5 Lightcurve plots . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 733.6 Shape and spin distributions for different sized MBAs . . . . . . . . . . . 753.7 NEA and SMBA lightcurve distribution comparison . . . . . . . . . . . . 763.8 NEA and SMBA lightcurve distribution comparison, H < 17 . . . . . . . 774.1 Lightcurves periods and amplitudes for NEAs, MBAs and SMBAs . . . . 854.2 NEA lifetimes . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 864.3 Test of 3-body simulations . . . . . . . . . . . . . . . . . . . . . . . . . 914.4 MBA binary properties . . . . . . . . . . . . . . . . . . . . . . . . . . . 944.5 Number of binaries in nominal simulation . . . . . . . . . . . . . . . . . 974.6 Properties of binaries in nominal simulation . . . . . . . . . . . . . . . . 984.7 Lifetimes of binaries in nominal simulation . . . . . . . . . . . . . . . . 99ix
4.8 Percentage of migrated binaries . . . . . . . . . . . . . . . . . . . . . . . 1004.9 Influence of tidal evolution on simulations . . . . . . . . . . . . . . . . . 1025.1 Preliminary YORP spinup results . . . . . . . . . . . . . . . . . . . . . . 111A.1 Results from simulations with varying resolution. . . . . . . . . . . . . . 117x
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 and 10: 2.3 Results and Discussion . . . .
Page 11: List of Tables1.1 Binary NEA proper
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
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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
Page 71 and 72:
(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
Page 85 and 86:
Figure 3.4: Asteroid lightcurves.72
Page 87 and 88:
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
Page 135 and 136:
Benner, L. A. M., Nolan, M. C., Ost
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V7.0:LCREF TAB, 35, 4Harris, A. W.,
Page 139 and 140:
Storrs, A. D., Close, L. M., & Mena
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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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