Do Slivan states exist in the Flora family?

Kryszczyńska, A.

doi:10.1051/0004-6361/201220490

Cited by 26 publications

(33 citation statements)

References 29 publications

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“…Also, observational evidence showed that the spin orientation in the collisional asteroid family Koronis (Slivan 2002) and Flora (Kryszczyńska 2013) are indeed not following a Maxwellian distribution, as collisional origin would produce, but rather distributed bi-modal, with 42°to 50°for prograde, and 154°to 169°for retrograde rotators in the Koronis family (Slivan et al 2003). This gives indirect evidence for evolution due to YORP after the family creating event, and first hand evidence for the importance of the effect in the evolution of the asteroid belt.…”

Section: Introductionmentioning

confidence: 95%

Hyper-Velocity Impacts on Rubble Pile Asteroids

Deller¹

2017

Springer Theses

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SummaryMost asteroids in the size range of approximately 100 m to 100 km are rubble piles, aggregates of rocky material held together mainly by gravitational forces, and only weak cohesion. They contain high macroporosities, indicating a large amount of void space in their interiors. How these voids are distributed is not yet known, as in-situ measurements are still outstanding.In this work, a model to create rubble pile asteroid simulants for use in SPH impact simulations is presented. Rubble pile asteroids are modelled as gravitational re-aggregating remnant fragments of a catastrophically disrupted parent body, which are represented by spherical pebbles. It is shown that this approach allows to explicitly follow the internal restructuring of rubble pile asteroids during impact events, while preserving the expected properties of the bulk asteroid as known from observations and experiments. The bulk behaviour of asteroid simulants, as characterized by the stability against disruption and fragment size distribution, follows the expected behaviour and is not sensitive to the exact distribution of voids in the interior structure, but rather to the void fraction as the amount of consolidated void space in between the constituent fragment pebbles. No exact a priory knowledge of the fragment size distribution inside the body is therefore needed to use this model in impact simulations.Modelling the behaviour of the large-scale rubble pile constituents during impact events is used as a tool to infer the internal structure of asteroids by linking surface features like hills or pits to the creation of sub-catastrophic craters.In this work, the small rubble pile asteroid (2867) Šteins is analysed. The flyby of the Rosetta spacecraft at Šteins has revealed several interesting features: the large crater Diamond close to the southern pole, a hill like feature almost opposite to the crater, and a catena of crater pits extending radially from the rim of the crater.A possible link between these two structures and the cratering event is investigated in a series of impact simulations varying the interior of a plausible shape of Šteins prior to the event that formed crater Diamond. A connection between the cratering event and the hill is shown to be highly unlikely. Therefore, the hill is most likely a remnant of the formation of Šteins. Its size therefore helps to infer the initial size distribution of fragments forming the asteroid.The formation of a fracture radially from the crater can be observed for rubble pile simulants with highly collimated voids. This fracture could plausibly form the catena of pits observed on Šteins. This can therefore serve as a link between observable surface features and Šteins internal structure. The interior of Šteins is most likely an aggregate of fragments that themselves are only lightly fractured, and large void spaces might be found inside the asteroid. As Šteins seems to be a good example of a YORPoid, an asteroid that has been evolved to a top-like shape by radiative forces due to the YORP ...

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Section: Introductionmentioning

confidence: 95%

Hyper-Velocity Impacts on Rubble Pile Asteroids

Deller¹

2017

Springer Theses

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“…The high-resolution camera revealed the unique six comet-like dust tails of asteroid P/2013 P5 (Figure 1). Jewitt et al (2013) observed the object on both September 10, 2013 andSeptember 23, 2013. In this two-week time span between observations, P/2013 P5 displayed many differences in the appearance of its six tails.…”

Section: Introductionmentioning

confidence: 97%

Rotational Properties of the Extraordinary Multi-tailed Asteroid P/2013 P5

Gustafsson¹

2015

OURJ

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Observations made with the Hubble Space Telescope in September 2013 revealed that the asteroid known as P/2013 P5 appeared to have six comet-like tails. Jewitt et al. (2013) concluded that this extraordinary structure and activity could not be explained by traditional near-surface ice sublimation or collision events ejecting particles from the asteroid's surface. Instead, the most likely explanation is that this unusual object has been spun-up by solar radiation forces to a critical limit which has resulted in the rotational disruption of the asteroid causing the unique six-tail structure. This interpretation predicts that the nucleus of this comet-like asteroid should be in rapid rotation. In November 2013, broadband photometry of P/2013 P5 was obtained with Lowell Observatory's 4.3-meter Discovery Channel Telescope using the Large Monolithic Imager to investigate the possibility of rapid rotation. While the variation in the rotational light curve from these data was too small to be justifiable, morphological changes in the nucleus-coma system were observed.

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“…Additionally, Vokrouhlický et al (2003) showed that this situation is a natural end-state of a billion-year evolution driven by the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. Recently, Kryszczyńska (2013) suggested that similar Slivan states might also exist among the Flora-family members at a much smaller heliocentric distance. However, Vraštil & Vokrouhlický (2015) showed that their stability is much lower than in the Koronis-family zone, and proposed instead that asteroids in the Massalia family are better situated to have their axes captured in the stable Slivan states.…”

Section: Introductionmentioning

confidence: 99%

Low-frequency Slivan states in the outer main belt?

Vraštil

Vokrouhlický

2016

A&A

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Context. Spin states of several main belt asteroids have been recently found to reside in what is called the Slivan state, namely a secular spin-orbit resonance with the s 6 mode of their orbital precession in space. Aims. We examine a possibility of the Slivan states of asteroids with other than orbital s 6 precession frequency. Methods. The asteroids' orbital and spin states are numerically propagated using well-tested computer codes. We select parameter space favorable for the Slivan-state capture with the s 7 frequency mode of the orbital precession. The stability of these states is numerically verified. Results. We find that asteroid (184) Dejopeja has a spin state captured in (or very nearly) the Slivan state with the s 7 orbital frequency. In general, such a situation may favorably occur for low-inclination orbits in the outermost part of the main asteroid belt. We expect these states to be common among the Themis family members.

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Do Slivan states exist in the Flora family?

Cited by 26 publications

References 29 publications

Hyper-Velocity Impacts on Rubble Pile Asteroids

Hyper-Velocity Impacts on Rubble Pile Asteroids

Rotational Properties of the Extraordinary Multi-tailed Asteroid P/2013 P5

Low-frequency Slivan states in the outer main belt?

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