The resonant population of asteroids in librating states of the ν6 linear secular resonance

Huaman, M.; Roig, F.; Carruba, V.; Domingos, R. C.; Aljbaae, S.

doi:10.1093/mnras/sty2381

Cited by 7 publications

(9 citation statements)

References 29 publications

(49 reference statements)

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“…with the ν 6 secular resonance 2 and the family members are located in the anti-aligned states (Machuca & Carruba 2012;Carruba et al 2014;Huaman et al 2018;Milani et al 2019). For objects that are temporarily captured in the ν 6 resonance, their e p can be pumped up significantly and subsequently be implanted into Jupiter-crossing, Mars-crossing, and even near-Earth orbits (Masiero et al 2015).…”

Section: Evolution and Age Of The Familymentioning

confidence: 99%

Physical and dynamical characterization of the Euphrosyne asteroid family

Yang

Hanuš

Brož

et al. 2020

A&A

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Aims. The Euphrosyne asteroid family occupies a unique zone in orbital element space around 3.15 au and may be an important source of the low-albedo near-Earth objects. The parent body of this family may have been one of the planetesimals that delivered water and organic materials onto the growing terrestrial planets. We aim to characterize the compositional properties as well as the dynamical properties of the family. Methods. We performed a systematic study to characterize the physical properties of the Euphrosyne family members via low-resolution spectroscopy using the NASA Infrared Telescope Facility. In addition, we performed smoothed-particle hydrodynamics (SPH) simulations and N-body simulations to investigate the collisional origin, determine a realistic velocity field, study the orbital evolution, and constrain the age of the Euphrosyne family. Results. Our spectroscopy survey shows that the family members exhibit a tight taxonomic distribution, suggesting a homogeneous composition of the parent body. Our SPH simulations are consistent with the Euphrosyne family having formed via a reaccumulation process instead of a cratering event. Finally, our N-body simulations indicate that the age of the family is 280−80+180 Myr, which is younger than previous estimates.

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Section: Evolution and Age Of The Familymentioning

confidence: 99%

Physical and dynamical characterization of the Euphrosyne asteroid family

Yang

Hanuš

Brož

et al. 2020

A&A

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“…After the next 200 Myr of evolution, the family dynamically spreads due to combined effects of the Yarkovsky drift and resonant perturbations. Strong diffusion is observed close to the family center where the mean-motion resonances overlap with the ν 6 secular resonance 2 and the family members are located in the anti-aligned states (Machuca & Carruba 2012;Carruba et al 2014;Huaman et al 2018;Milani et al 2019). For objects that are temporarily captured in the ν 6 resonance, their e p can be pumped up significantly and subsequently be implanted into Jupiter-crossing, Mars-crossing, and even near-Earth orbits (Masiero et al 2015).…”

Section: Evolution and Age Of The Familymentioning

confidence: 99%

Physical and dynamical characterization of the Euphrosyne asteroid Family

Yang,

Hanus,

Broz

et al. 2020

Preprint

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Aims. The Euphrosyne asteroid family occupies a unique zone in orbital element space around 3.15 au and may be an important source of the low-albedo near-Earth objects. The parent body of this family may have been one of the planetesimals that delivered water and organic materials onto the growing terrestrial planets. We aim to characterize the compositional properties as well as the dynamical properties of the family. Methods. We performed a systematic study to characterize the physical properties of the Euphrosyne family members via lowresolution spectroscopy using the IRTF telescope. In addition, we performed smoothed-particle hydrodynamics (SPH) simulations and N-body simulations to investigate the collisional origin, determine a realistic velocity field, study the orbital evolution, and constrain the age of the Euphrosyne family. Results. Our spectroscopy survey shows that the family members exhibit a tight taxonomic distribution, suggesting a homogenous composition of the parent body. Our SPH simulations are consistent with the Euphrosyne family having formed via a reaccumulation process instead of a cratering event. Finally, our N-body simulations indicate that the age of the family is 280 +180 −80 Myr, which is younger than a previous estimate.

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“…To identify the population of ν6 resonators, first, we need to select the asteroids most likely to be affected by this resonance. For this purpose, we use the criterion described in (Huaman et al 2018): we compute the value of σ = ̟ − ̟6 for all asteroids of interest, and select those for which:…”

Section: Selecting the Population Of Likely ν6 Resonatorsmentioning

confidence: 99%

“…As discussed in (Huaman et al 2018), these are the bodies that are more likely to be in aligned or anti-aligned librating states of the resonance, according to the analytical model revised in (Huaman et al 2018). We applied this criterion to all the numbered asteroids for which proper elements and frequencies are available at the Asteroid Families Portal AF P ("http://asteroids.matf.bg.ac.rs/fam/index.php", Radović et al ( 2017)), i.e., those with an identification up to 523584, which yielded a sample of 4875 asteroids likely to be affected.…”

Section: Selecting the Population Of Likely ν6 Resonatorsmentioning

confidence: 99%

“…(Carruba et al 2014) later identified the case of the Euphrosyne family, with the second-largest population of asteroids in such states. Finally, (Huaman et al 2018) extended this analysis to the whole main-belt, and, apart from identifying the case of the 329 Svea family, the third asteroid family in terms of population of asteroids in ν6 anti-aligned states, found the first seven asteroids in aligned states of the same resonance.…”

Section: Introductionmentioning

confidence: 99%

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Identifying the population of stable $ν_6$ resonant asteroids using large databases

Carruba,

Aljbaae,

Domingos

et al. 2022

Preprint

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Large observational surveys, like those that will be conducted at the Vera C. Rubin Observatory, are expected to discover up to one million new asteroids in the first year of operation. This will more than double the database of known asteroids in a very short time. New methods and techniques will be needed to handle the large influx of data.Here we tested some of these new methods by studying the population of asteroids on stable orbits inside the ν 6 secular resonance. This resonance is one of the strongest mechanisms for destabilizing the orbits of main-belt bodies and producing Near-Earth Asteroids (NEAs). Yet, stable orbital configurations where the asteroid pericenter is either aligned or anti-aligned with that of Saturn exist inside the resonance. The population of stable ν 6 resonators, first discovered in the early 2010s, is now the largest population of asteroids in stable orbits inside a secular resonance.Here we obtained the largest sample of asteroids' proper elements for numbered and multi-opposition objects most likely to be affected by the resonance. Artificial Neural Networks (ANN) were then used to identify the images of resonant angles of asteroids in stable orbits, more than doubling their number. Clustering methods and the use of machine learning algorithms allowed the identification of the known asteroid families crossed by the ν 6 resonance, the Tina, Euphrosyne, and Svea clusters, and of two entirely new groups: the Tiffanykapler and the 138605 QW177 families.

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The resonant population of asteroids in librating states of the ν6 linear secular resonance

Cited by 7 publications

References 29 publications

Physical and dynamical characterization of the Euphrosyne asteroid family

Physical and dynamical characterization of the Euphrosyne asteroid family

Physical and dynamical characterization of the Euphrosyne asteroid Family

Identifying the population of stable $ν_6$ resonant asteroids using large databases

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