Angular momentum of binary asteroids: Implications for their possible origin

Descamps, P.; Marchis, Franck

doi:10.1016/j.icarus.2007.07.024

Cited by 44 publications

(67 citation statements)

References 44 publications

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“…In fact, the high value of the specific angular momentum and the scaled spin rate of this system do not fall into the "high size ratio binaries" region indicated in Fig. 9 of Descamps & Marchis (2008) and is far from the Jacobi or MacLaurin sequences. Accordingly, we can probably discard a possible rotational fission origin for this binary.…”

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 75%

“…One argument in favor of a rotational fission scenario for some cases is the specific angular momentum of a binary and multiple system. The specific angular momentum (SAM), computed according to Descamps & Marchis (2008) is…”

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

“…The scaled spin rate and specific angular momentum are dimensionless values. Based on a binary asteroid population study, Descamps & Marchis (2008) concluded that binary systems near the MacLaurin/Jacobi transition are most likely formed by rotational fission or mass shedding. In Fig.…”

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

“…We indicate the MacLaurin and the Jacobi sequences. The "high size ratio binaries", as indicated in Descamps & Marchis (2008), are located near the MacLaurin/Jacobi transition. The legend is as follows: the black triangle denotes Salacia-Actaea, the gray diamond HaumeaNamaka, the black diamond Haumea-Hi'iaka, the gray triangle VardaIlmarë, the gray square Quaoar-Weywot, the black circle Orcus-Vanth assuming a secondary-to-primary mass ratio of 0.03, the gray circle Orcus-Vanth assuming a secondary-to-primary mass ratio of 0.09, and black square for Typhon-Echidna.…”

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

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Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

Thirouin

Noll

Ortiz

et al. 2014

A&A

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We present results for the short-term variability of binary trans-Neptunian objects (BTNOs). We performed CCD photometric observations using the 3.58 m Telescopio Nazionale Galileo (TNG), the 1.5 m Sierra Nevada Observatory (OSN) telescope, and the 1.23 m Centro Astronómico Hispano Alemán (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the short-term variability of six BTNOs. Our sample contains three classical objects: (174567) We also derived some physical properties from their light curves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast light curve database for TNOs including centaurs to determine the light-curve amplitude and spin frequency distributions for the binary and non-binary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63 ± 0.52 h for the entire sample, 8.37 ± 0.58 h for the sample without the binary population, and 10.11 ± 1.19 h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86 ± 0.58 h for the sample without the centaur population, and of 8.64 ± 0.67 h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.

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Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 75%

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

Section: Formation Of Binary and Multiple Systemsmentioning

confidence: 99%

See 2 more Smart Citations

Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

Thirouin

Noll

Ortiz

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…The internal density of asteroids inferred from their orbital dynamics is in the range 1 − 5 g/cm 3 (Margot et al 2002;Marchis et al 2006;Descamps & Marchis 2008). We assume that differentiation and fragmentation may have occurred among relatively large planetesimals, whereas small planetesimals may be considered to be pristine rubble piles.…”

Section: Methodsmentioning

confidence: 99%

Planetesimal Clearing and Size-dependent Asteroid Retention by Secular Resonance Sweeping during the Depletion of the Solar Nebula

Zheng

Lin

Kouwenhoven

2017

ApJ

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The distribution of heavy elements is anomalously low in the asteroid main belt region compared with elsewhere in the solar system. Observational surveys also indicate a deficit in the number of small ( 50 km size) asteroids that is two orders of magnitude lower than what is expected from the single power-law distribution that results from a collisional coagulation and fragmentation equilibrium. Here, we consider the possibility that a major fraction of the original asteroid population may have been cleared out by Jupiter's secular resonance, as it swept through the main asteroid belt during the depletion of the solar nebula. This effect leads to the excitation of the asteroids' orbital eccentricities. Concurrently, hydrodynamic drag and planet-disk tidal interaction effectively damp the eccentricities of sub-100 km-size and of super-lunar-size planetesimals, respectively. These combined effects lead to the asteroids' orbital decay and clearing from the present-day main belt region (∼ 2.1 − 3.3 AU). Eccentricity damping for the intermediate-size (50 to several hundreds of kilometers) planetesimals is less efficient than for small or large planetesimals. These objects therefore preferentially remain as main belt asteroids near their birthplaces, with modest asymptotic eccentricities. The smaller asteroids are the fragments of subsequent disruptive collisions at later times as suggested by the present-day asteroid families. This scenario provides a natural explanation for both the observed low surface density and the size distribution of asteroids in the main belt, without the need to invoke special planetesimal formation mechanisms. It also offers an explanation for the confined spatial extent of the terrestrial planet building blocks without the requirement of extensive migration of Jupiter, which is required in the grand-tack scenario.

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Tidal evolution of close binary asteroid systems

Taylor

Margot

2010

Celest Mech Dyn Astr

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We provide a generalized discussion of tidal evolution to arbitrary order in the expansion of the gravitational potential between two spherical bodies of any mass ratio. To accurately reproduce the tidal evolution of a system at separations less than 5 times the radius of the larger primary component, the tidal potential due to the presence of a smaller secondary component is expanded in terms of Legendre polynomials to arbitrary order rather than truncated at leading order as is typically done in studies of well-separated system like the Earth and Moon. The equations of tidal evolution including tidal torques, the changes in spin rates of the components, and the change in semimajor axis (orbital separation) are then derived for binary asteroid systems with circular and equatorial mutual orbits. Accounting for higher-order terms in the tidal potential serves to speed up the tidal evolution of the system leading to underestimates in the time rates of change of the spin rates, semimajor axis, and mean motion in the mutual orbit if such corrections are ignored. Special attention is given to the effect of close orbits on the calculation of material properties of the components, in terms of the rigidity and tidal dissipation function, based on the tidal evolution of the system. It is found that accurate determinations of the physical parameters of the system, e.g., densities, sizes, and current separation, are typically more important than accounting for higher-order terms in the potential when calculating material properties. In the scope of the long-term tidal evolution of the semimajor axis and the component spin rates, correcting for close orbits is a small effect, but for an instantaneous rate of change in spin rate, semimajor axis, or mean motion, the close-orbit correction can be on the order of tens of percent. This work has possible implications for the determination of the Roche limit and for spin-state alteration during close flybys.

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Angular momentum of binary asteroids: Implications for their possible origin

Cited by 44 publications

References 44 publications

Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

Rotational properties of the binary and non-binary populations in the trans-Neptunian belt

Planetesimal Clearing and Size-dependent Asteroid Retention by Secular Resonance Sweeping during the Depletion of the Solar Nebula

Tidal evolution of close binary asteroid systems

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