Dynamical evolution and chronology of the Hygiea asteroid family

Carruba, V.; Domingos, R. C.; Huaman, M.; Santos, Carla Rodrigues dos; Souami, D.

doi:10.1093/mnras/stt2040

Cited by 25 publications

(32 citation statements)

References 35 publications

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“…We observed Hygiea with sub-Earth latitudes near 50°S (first epoch) and 24°S (second epoch) so that the visible surface extended from 66°N through 90°S, leading to ~95% surface coverage. Surprisingly, none of our images and their associated contours (supplementary figure 3) revealed the large impact basin expected from the large size of the Hygiea family 3,12 (volume-equivalent diameter (D eq ) of the family members ~ 100 km; see Methods). In comparison, Vesta possesses a large impact basin that is clearly observable from the ground 13,7 (Fig.…”

Section: By Comparing Hygiea's Sphericity With That Of Other Solar Symentioning

confidence: 93%

A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea

et al. 2019

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Section: By Comparing Hygiea's Sphericity With That Of Other Solar Symentioning

confidence: 93%

A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea

et al. 2019

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“…No physical data on these interlopers were found, thus it is difficult to know whether they are also physical interlopers. In order to refine the family age estimation previously obtained, we followed the work of Carruba et al (2014a), Carruba, Aljbaae & Souami (2014b) and Carruba et al (2015), analysing the semimajor axis evolution of a fictitious distribution of asteroids, evolved for different values of the ejection velocity parameter (V EJ ) under the influence of Yarkovsky diurnal and seasonal effects. We used the Monte Carlo method of Vokrouhlický et al (2006a,b,c).…”

Section: H Ro N O L O G Ymentioning

confidence: 99%

The Maria asteroid family

Aljbaae

Carruba

Masiero

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The Maria asteroid family is a group of S-type asteroids. Its location adjacent to the left side of the 3J:-1A mean-motion resonances could be the reason for the absence of the left side of the 'V' shape in the (a, 1/D) domain. This family can be considered as a likely source of ordinary chondrite-like material. In this work, we make use of the time dependence of the asymmetric coefficient A S describing the degree of asymmetry of the C distribution of a fictitious Maria family generated with the value of the ejection velocity parameter V EJ = 35 m s −1 to obtain an age estimate of 1750 −231 +537 Myr, in good agreement with the family age found in the literature. Analysing the contribution to the near-Earth object (NEO) population, we found that about 7.6 per cent of presently known near-Earth asteroids (NEAs) have orbits similar to asteroids from the Maria family. Only ∼1.7 per cent of our simulated family can stay in NEO space for more than 10 Myr, while only five asteroids become NEOs in the last 500 Myr of the simulation.

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“…In particular, if a secular resonance is effective in a layer in proper element space which has a large width in proper a, a Yarkovsky driven transport is possible 10 . Indeed, Carruba et al (2014a) show the results of a large-scale numerical experiment on transport due to the Yarkovsky effect inside and near secular resonances, and in particular the z 1 resonance; see their Fig. 9, in the top-left corner, which refers to a portion of the Eos family more or less corresponding to the one shown in Fig.…”

Section: Family Of (179) Klytaemnestramentioning

confidence: 99%

Asteroid cratering families: recognition and collisional interpretation

Milani

Knežević

Spoto

et al. 2019

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Aims. We continue our investigation of the bulk properties of asteroid dynamical families identified using only asteroid proper elements to provide plausible collisional interpretations. We focus on cratering families consisting of a substantial parent body and many small fragments. Methods. We propose a quantitative definition of cratering families based on the fraction in volume of the fragments with respect to the parent body; fragmentation families are above this empirical boundary. We assess the compositional homogeneity of the families and their shape in proper element space by computing the differences of the proper elements of the fragments with respect to the ones of the major body, looking for anomalous asymmetries produced either by post-formation dynamical evolution, or by multiple collisional/cratering events, or by a failure of the hierarchical clustering method (HCM) for family identification. Results. We identified a total of 25 dynamical families with more than 100 members ranging from moderate to heavy cratering. For three families (4, 15 and 283) we confirm the occurrence of two separate cratering events, while family (569) Misa is a mixed case, with one cratering event and one fragmentation event. The case of family 3 remains dubious, in that there could be either one or two collisions. For family 20, we propose a double collision origin, not previously identified. In four cases (31, 480, 163 and 179) we performed a dedicated search for dynamical resonant transport mechanisms that could have substantially changed the shape of the family. By using a new synthetic method for computation of secular frequencies, we found possible solutions for families 31, 480, and 163, but not for family 179, for which we propose a new interpretation, based on a secular resonance contaminating this family: the family of 179 should be split into two separate clusters, one containing (179) itself and the other, family (9506) Telramund, of fragmentation type, for which we have computed an age.

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Dynamical evolution and chronology of the Hygiea asteroid family

Cited by 25 publications

References 35 publications

A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea

A basin-free spherical shape as an outcome of a giant impact on asteroid Hygiea

The Maria asteroid family

Asteroid cratering families: recognition and collisional interpretation

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