Asteroid Family Associations of Active Asteroids

Hsieh, Henry H.; Novaković, Bojan; Kim, Yoonyoung; Brasser, R.

doi:10.3847/1538-3881/aaa5a2

Cited by 45 publications

(41 citation statements)

References 165 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Usui et al (2019) presented the spectrum of ( 24) Themis obtained by the Akari space telescope, where they identified two features: one at 2.7 µm associated with hydrated minerals, and another at around 3.071 µm related to water ice. Another indication of water ice as a constituent of the family composition is the presence of three MBCs, in which the cometary activity is suggested to be sublimation-driven (Hsieh et al 2018). As proposed by Castillo-Rogez & Schmidt (2010) and Marsset et al (2016), a possible explanation for the spectral diversity of Themis, which includes hydrated members, MBCs, and surface ice on two family members, is that the Themis parent body could be partially differentiated.…”

Section: Discussionmentioning

confidence: 97%

A comparative analysis of the outer-belt primitive families

Pra

Pinilla-Alonso

Carvano

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Asteroid families are witnesses to the intense collisional evolution that occurred on the asteroid belt. The study of the physical properties of family members can provide important information about the state of differentiation of the parent body and provide insights into how these objects were formed. Several of these asteroid families identified across the main belt are dominated by low-albedo, primitive asteroids. These objects are important for the study of Solar System formation because they were subject to weaker thermophysical processing and provide information about the early conditions of our planetary system. Aims. We aim to study the diversity of physical properties among the Themis, Hygiea, Ursula, Veritas, and Lixiaohua families. Methods. We present new spectroscopic data, combined with a comprehensive analysis using a variety of data available in the literature, such as albedo and rotational properties. Results. Our results show that Themis and Hygiea families, the largest families in the region, present similar levels of hydration. Ursula and Lixiaohua families are redder in comparison to the others and present no sign of hydrated members based on the analysis of visible spectra. Conversely, Veritas presents the highest fraction of hydrated members. Conclusions. This work demonstrates a diverse scenario in terms of the physical properties of primitive outer-belt families, which could be associated with dynamical mixing of asteroid populations and the level of differentiation of the parental body.

show abstract

Section: Discussionmentioning

confidence: 97%

A comparative analysis of the outer-belt primitive families

Pra

Pinilla-Alonso

Carvano

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…Many MBCs may be much younger, being apparent members of asteroid families formed in catastrophic disruption events of larger parent bodies in the relatively recent past (cf. Hsieh et al, ). Recent formation of MBCs is also supported by the fact that they exhibit comet‐like activity, implying the presence of ice in near‐surface layers and not only in their deep interiors.…”

Section: Model Of Ice Retreatmentioning

confidence: 99%

Ice Loss From the Interior of Small Airless Bodies According to an Idealized Model

Schörghofer

Hsieh

2018

JGR Planets

Self Cite

View full text Add to dashboard Cite

Ice in main belt asteroids and near‐Earth objects is of scientific and resource exploration interest, but small airless bodies gradually lose their ice to space by outward diffusion. Here we quantitatively estimate the time it takes a porous airless body to lose all of its interior ice, based on an analytic solution for the interior temperature field of bodies in stable orbits. Without latent heat, the average surface temperature, which is lower than the classic effective temperature, is representative of the body interior and hence an appropriate temperature to evaluate desiccation timescales. In a spherically averaged model, an explicit analytic solution is obtained for the depth to ice as a function of time and the time to complete desiccation. Half of the ice volume is lost after 11% of this time. A bilobate structure emerges from the strong latitude dependence of desiccation rates. Cold polar regions can harbor subsurface ice, even when the body center does not. Latent heat retards ice loss, and we obtain a succinct expression for the temperature difference between the surface and the ice. In the outer main belt, nearly all bodies 10 km in size or larger should have been able to retain ice in their interiors over the age of the solar system. Each of the following factors favors the presence of ice inside near‐Earth objects: a semimajor axis in the outer belt or beyond, a mantle of very low thermal inertia, a young age, or a small and stable axis tilt.

show abstract

“…Still, several questions regarding their structure, composition, and origin are yet to be answered. For instance, the MBCs are found to be associated with collisional asteroid families of primitive taxonomic classifications (Hsieh, et al 2018;Novaković 2018). The low thermal conductivity of porous cometary material suggests that ice may be retained in the interior of main-belt asteroids, despite continual solar heating.…”

Section: Future Prospectsmentioning

confidence: 99%

Analysis of the Karma asteroid family

Pavela

Novaković

Carruba

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The Karma asteroid family is a group of primitive asteroids in the middle part of the main belt, just at the outer edge of the 3J:1A mean-motion resonance. We obtained the list of the family members with 317 asteroids, and estimated that it was formed by the catastrophic disruption of a parent body that was between 34 and 41 km in diameter. Based on the V-shape method, age of the Karma family is estimated to be about 137 Myr. A detailed dynamical map of the region combined with numerical simulations allowed us to reconstruct the long-term dynamical evolution of the family, and to identify the mechanisms responsible for this evolution. The numerical simulations successfully reproduced the main features in the orbital distribution of the family members but also showed that some regions of the Karma family could be missing. A more detailed analysis revealed that these regions likely consist of very dark objects, fainter than absolute magnitude H=17, that have not yet been detected. Based on the obtained results, we concluded that magnitude-frequency distribution of family members up to H=16 mag is neither affected by dynamical erosion nor observational incompleteness, and therefore represents the result of collisional grinding of the original family population. Finally, we found that the Karma family have been supplying some asteroids to the near-Earth region via the 3J:1A resonance. Currently there should about 10 family members larger than 1 km in diameter, orbiting in the near-Earth space.

show abstract

Asteroid Family Associations of Active Asteroids

Cited by 45 publications

References 165 publications

A comparative analysis of the outer-belt primitive families

A comparative analysis of the outer-belt primitive families

Ice Loss From the Interior of Small Airless Bodies According to an Idealized Model

Analysis of the Karma asteroid family

Contact Info

Product

Resources

About