Forming Binary Near-Earth Asteroids From Tidal Disruptions

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Table 1.1.Binary NEA properties.Binary a e D pri P pri a D sec P orb Disc. ref(AU) (km) (h) km (km) (d)(66391) 1999 KW 4 0.64 0.68 1.2 2.77 2.5 0.4 0.73 R [1,2]1998 ST 27 0.81 0.53 0.8 3.0 4.0 0.12 R [3,4]1999 HF 1 0.81 0.46 3.5 2.32 7.0 0.8 0.58 L [2,5](5381) Sekhmet 0.94 0.29 1.0 2.7 1.5 0.3 0.52 R [6,7](66063) 1998 RO 1 0.99 0.72 0.8 2.49 1.4 0.38 0.60 L [2,8]1996 FG 3 1.05 0.35 1.5 3.59 2.6 0.47 0.67 L [2,9,10](88710) 2001 SL 9 1.06 0.27 0.8 2.40 1.4 0.22 0.68 L [2,11]1994 AW 1 1.10 0.07 1.0 2.52 2.1 0.5 0.93 L [2,12]2003 YT 1 1.10 0.29 1.0 2.34 2.7 0.18 1.25 L/R [2,13](35107) 1991 VH 1.13 0.14 1.2 2.62 3.2 0.44 1.36 L [2,14]2000 DP 107 1.36 0.37 0.8 2.77 2.6 0.3 1.76 R [2,15,16,17](1862) Apollo 1.47 0.56 1.6 3.06 3.0 0.08 R [33](65803) Didymos 1.64 0.38 0.8 2.26 1.1 0.17 0.49 L/R [2,18](69230) Hermes 1.65 0.62 0.6 13.89 0.54 R [2,19]1990 OS 1.67 0.46 0.3 0.6 0.05 0.88 R [20](5407) 1992 AX 1.83 0.27 3.9 2.55 6.8 0.78 0.56 L [2,21]2002 BM 26 1.83 0.44 0.6 2.7 0.1 R [22](85938) 1999 DJ 4 1.85 0.48 0.4 2.51 1.5 0.17 0.74 L [2,23,24]2000 UG 11 1.92 0.57 0.2 4.44 0.4 0.08 0.77 R [2,25]2003 SS 84 1.93 0.57 0.1 0.06 R [26]2002 KK 8 1.95 0.46 0.5 0.1 R [27](31345) 1998 PG 2.01 0.39 0.9 2.52 1.5 0.3 L [2,28](3671) Dionysus 2.19 0.54 1.5 2.71 3.8 0.3 1.16 L [2,29]2002 CE 26 2.23 0.55 3.0 3.29 5.1 0.21 0.67 R [2,30]1994 XD 2.35 0.73 0.6 1.0 0.15 0.67 R [32]2005 AB 3.21 0.65 3.33 0.75 L [31]Note. — Orbital and physical properties for well-observed or suspected NEA binaries. Thediscovery techniques are (L) lightcurve and (R) radar. References: [1] Benner et al. (2001b); [2]Pravec et al. (2006); [3] Benner et al. (2001a); [4] Benner et al. (2003); [5] Pravec et al. (2002); [6]Nolan et al. (2003b); [7] Neish et al. (2003); [8] Pravec et al. (2003b); [9] Pravec et al. (2000b);[10] Mottola & Lahulla (2000); [11] Pravec et al. (2001); [12] Pravec & Hahn (1997); [13] Nolanet al. (2004); [14] Pravec et al. (1998); [15] Ostro et al. (2000); [16] Pravec et al. (2000a); [17]Margot et al. (2002); [18] Pravec et al. (2003a); [19] Margot et al. (2003); [20] Ostro et al. (2003);[21] Pravec et al. (2000b); [22] Nolan et al. (2002a); [23] Pravec et al. (2004a); [24] Benner et al.(2004); [25] Nolan et al. (2000); [26] Nolan et al. (2003a); [27] Nolan et al. (2002b); [28] Pravecet al. (2000b); [29] Mottola et al. (1997); [30] Shepard et al. (2004); [31] Reddy et al. (2005);[32] Benner et al. (2005); [33] Ostro et al. (2005),5
1.1.3 Binary Main-Belt asteroidsRecent discoveries among small Main-Belt asteroids (MBAs) using lightcurve observationshave started to remove the observational biases that previously obscured any similaritiesbetween binary MBAs and NEAs (Pravec & Harris 2006). At first they were discoveredprimarily using two distinct techniques, lightcurves for NEAs and high-resolutiondirect imaging for MBAs. These two techniques preferentially discover entirely differentkinds of binaries, with lightcurves only sensitive to binaries with small separation andmoderate (1.0-0.2) size ratios, whereas direct imaging is primarily sensitive to binarieswith a large separation and can cover a wider range of size ratios.A limiting factor, which plagues both discovery methods, is primary size. This isa complication regardless of observing technique, as a 1 km body in the Main Belt issubstantially more difficult to study than one in the near-Earth population. Despite recentlightcurve discoveries among MBAs with D < 5km, sub-kilometer discoveries of any kindwould require substantial time on very large telescopes. Discoveries with both methodspoint to two seemingly different groups within the binary MBA population, each formedfrom different mechanisms. Hence, we describe the binaries discovered by each methodseparately.High-resolution imaging discoveriesThe binary MBAs discovered via direct imaging always have relatively distant companionsthat must be observed outside of the point spread function of the brighter primary.However, these observations are sensitive to large brightness differences, for example(45) Eugenia’s moon Petit Prince was 7 magnitudes dimmer at discovery than its primary(Merline et al. 2002c). These two effects demand that the observed MBA binaries havelarge separations but allow a wide range of size ratios. Even the smallest binaries discov-6
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 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: the largest lightcurve amplitudes o
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
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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
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Forming Binary Near-Earth Asteroids From Tidal Disruptions

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