Secular resonances with Ceres and Vesta

Tsirvoulis, Georgios; Novaković, Bojan

doi:10.1016/j.icarus.2016.06.024

Cited by 17 publications

(16 citation statements)

References 22 publications

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“…3. The dynamical model included gravitational forces including the Sun and eight planets (using the JPL DE405 planetary ephemeris), perturbations from Ceres, Pallas, Vesta, and Hygiea (Carruba et al 2007;Tsirvoulis & Novaković 2016) indicate that the close encounters or secular resonances with Vesta could influence orbital evolution of bodies in the inner main belt) and the thermal Yarkovsky force (we refer to it as using CPVH model further in the text). We used SWIFT_RMVSY software package as the main tool of numerical integration and calculations of mean and proper elements.…”

Section: Dynamical Modelmentioning

confidence: 99%

“…We also analyzed resonances with Vesta, focusing on nodal precession and precession of line of apsides. Tsirvoulis & Novaković (2016) indicates their potential impact on asteroids in the vicinity of the Spartacus region (in particular the nodal resonance). We found no significant secular resonances.…”

Section: Dynamical Modelmentioning

confidence: 99%

“…Two large craters were discovered and mapped on the surface of Vesta (Thomas et al 1997;Schenk et al 2012) consistent with this scenario. Some of those ejected asteroids formed the Vesta family while others were scattered and drifted away though the Yarkovsky effect, encounters with other bodies and dynamical resonances (Scholl & Froeschlé 1991;Vokrouhlicky 1998;Vokrouhlický & Farinella 1999;Nesvorný et al 2008;Carruba et al 2007;Tsirvoulis & Novaković 2016) and are known as Vesta fugitives. Some were perturbed into near-Earth orbits, some of which later struck the Earth and were collected as meteorites.…”

Section: Introductionmentioning

confidence: 99%

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Physical and dynamical properties of the unusual V-type asteroid (2579) Spartacus

Oszkiewicz

Kryszczyńska

Kankiewicz

et al. 2019

A&A

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Context. Asteroid (2579) Spartacus is a small V-type object located in the inner main belt. This object shows spectral characteristics unusual for typical Vestoids, which may indicate an origin deeper than average within Vesta or an origin from an altogether different parent body. Aims. Our main goal is to study the origin of Spartacus. We derive the spin of Spartacus and a convex shape model of Spartacus in order to increase the knowledge of the body’s physical properties. The rotational parameters are then used to investigate dynamical evolution of the object as well as to distinguish regions sampled by spectral observations to determine whether its surface displays heterogeneity. Methods. We collected lightcurves available from the literature (oppositions of 2009, 2012) and obtained additional photometric observations at various telescopes in 2016, 2017, and 2018. We used the lightcurve inversion method to derive a spin and convex shape model. We have collected spectral observations over two rotational periods of Spartacus and determined its spectral parameters using the modified Gaussian model (MGM). We then dynamically integrated the orbital elements of Spartacus, taking into account existing information, including its thermal properties, size and the derived spin axis orientation. Results. We find two models for (2579) Spartacus: (a) λ = 312° ± 5°, β = −57° ± 5° and (b) λ = 113° ± 5°, β = −60° ± 5° both retrograde. We find that the drift direction for Spartacus is consistent with separation from Vesta, and after a backward integration of 1 Gyr the asteroid reaches the boundary of the family. We did not observe spectral variations with rotation, thus the body most likely has a homogeneous surface. Additionally, new spectral analysis indicates that the 1.0 and 2.0 μm band centers are within ranges that are typical for Vestoids while the area ratio of these bands is about half that of typical Vestoids. Conclusions. The asteroid (2579) Spartacus is in retrograde rotation and has a drift direction consistent with an origin from Vesta. The revised spectral band centers are within ranges typical for Vestoids, while band area ratio (BAR) is unusually low compared to that of other V-types. The dynamical model shows that the asteroid could have migrated to its current location from the edges of the Vesta family within 1 Gyr, but an origin from an earlier impact on Vesta could also be plausible.

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Section: Dynamical Modelmentioning

confidence: 99%

Section: Dynamical Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Physical and dynamical properties of the unusual V-type asteroid (2579) Spartacus

Oszkiewicz

Kryszczyńska

Kankiewicz

et al. 2019

A&A

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“…Still, it should be noted that a smaller fraction of the Eos family, with H > 15 mag and a > 3.156 au, overlaps the Veritas family, suggesting that the latter may be contaminated by some members of the former group. Also, as noted by Tsirvoulis et al (2017), members of the Eos family could be found at a < 2.95 au, but a too high cutoff is needed to jump across the 7/3 resonance with Jupiter that limited the family at the inner edge.…”

Section: Other Familiesmentioning

confidence: 84%

An automatic approach to exclude interlopers from asteroid families

Radović

Novaković

Carruba

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Asteroid families are valuable source of information to many asteroid-related researches, assuming a reliable list of their members could be obtained. However, as the number of known asteroids increases fast it becomes more and more difficult to obtain robust list of members of an asteroid family. Here we are proposing a new approach to deal with the problem, based on the well known Hierarchical Clustering Method (HCM). An additional step in the whole procedure is introduced in order to reduce a so-called chaining effect. The main idea is to prevent chaining through an already identified interloper. We show that in this way a number of potential interlopers among family members is significantly reduced. Moreover, we developed an automatic on-line based portal to apply this procedure, i.e to generate a list of family members as well as a list of potential interlopers. The Asteroid Families Portal (AFP) is freely available to all interested researchers.

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“…Since the pioneering work of Hirayama (1918), a century ago, the study of asteroid families has been a very active field, and the primary source of our knowledge on the collisional history of the Main Belt (Bottke et al, 2005;Cellino et al, 2009). However, since asteroid families evolve over time due to various phenomena such as chaotic evolution of their orbits Nesvorný et al, 2002a), the semimajor drift induced by the Yarkovsky effect (Farinella & Vokrouhlický, 1999;Vokrouhlický et al, 2006b), further collisional evolution (Marzari et al, 1999;Dell'Oro et al, 2002), close encounters (Carruba et al, 2003;Novaković et al, 2010) and secular resonances with massive asteroids (Novaković et al, 2015;Tsirvoulis & Novaković, 2016), the older a family is, the less likely it is for us to reconstruct its collisional birth. Therefore, young asteroid families which have not evolved significantly allow us to extract information on the physical processes of colliding asteroids in a more direct manner.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a young subfamily of the (221) Eos asteroid family

Tsirvoulis

2018

Monthly Notices of the Royal Astronomical Society

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In this work we report the discovery of a young cluster of asteroids that originated by the breakup of an asteroid member of the (221) Eos family. By applying the Hierarchical clustering method to the catalog of proper elements we have identified 26 members of this new small group of asteroids. We have established that the statistical significance of this cluster is > 99%, therefore it corresponds to a real asteroid family, named the (633) Zelima cluster, after its lowest numbered member. The orbits of its members are dynamically stable, a fact that enabled us to use the backward integration method, in two variants to identify potential interlopers and estimate its age. Applying it first on the orbits of the nominal family members we identified three asteroids as interlopers. Then we applied it on a set of statistically equivalent clones of each member to determine the age of the cluster, with a result of 2.9 ± 0.2 Myrs. *

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Secular resonances with Ceres and Vesta

Cited by 17 publications

References 22 publications

Physical and dynamical properties of the unusual V-type asteroid (2579) Spartacus

Physical and dynamical properties of the unusual V-type asteroid (2579) Spartacus

An automatic approach to exclude interlopers from asteroid families

Discovery of a young subfamily of the (221) Eos asteroid family

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