Recent collisional jet from a primitive asteroid

Novaković, Bojan; Dell’Oro, A.; Cellino, A.; Knežević, Ž.

doi:10.1111/j.1365-2966.2012.21468.x

Cited by 18 publications

(17 citation statements)

References 78 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…; Nesvorný et al, 2008b), and (300163) P/2006 VW139 and P/2012 F5 (Gibbs) can be linked to small families that probably formed within the past 10 m.y. (Novaković et al, 2012a. If this relationship is confirmed by future studies, this can help us to understand how the MBCs are "activated".…”

Section: Detection Of Recent Breakupsmentioning

confidence: 79%

Identification and Dynamical Properties of Asteroid Families

Nesvorný¹,

Brož²,

Carruba³

2015

Asteroids IV

199

535

View full text Add to dashboard Cite

Asteroids formed in a dynamically quiescent disk but their orbits became gravitationally stirred enough by Jupiter to lead to high-speed collisions. As a result, many dozen large asteroids have been disrupted by impacts over the age of the Solar System, producing groups of fragments known as asteroid families. Here we explain how the asteroid families are identified, review their current inventory, and discuss how they can be used to get insights into long-term dynamics of main belt asteroids. Electronic tables of the membership for 122 notable families are reported on the Planetary Data System node.Comment: Asteroids IV chapte

show abstract

Section: Detection Of Recent Breakupsmentioning

confidence: 79%

Identification and Dynamical Properties of Asteroid Families

Nesvorný¹,

Brož²,

Carruba³

2015

Asteroids IV

199

535

View full text Add to dashboard Cite

show abstract

“…(Nesvorný and Bottke, 2004), Lorre (1.9 ± 0.3) m.y. (Novaković et al, 2012), P/2012 F5 (Gibbs) (1.5 ± 0.1) m.y. (Novaković et al, 2014), etc.…”

Section: Asteroid Familiesmentioning

confidence: 99%

The Collisional Evolution of the Main Asteroid Belt

Bottke¹,

Brož²,

O’Brien³

et al. 2015

Asteroids IV

View full text Add to dashboard Cite

Collisional and dynamical models of the main asteroid belt allow us to glean insights into planetesimal-and planet-formation scenarios as well as how the main belt reached its current state. Here we discuss many of the processes affecting asteroidal evolution and the constraints that can be used to test collisional model results. We argue the main belt's wavy size-frequency distribution for diameter D < 100-km asteroids is increasingly a byproduct of comminution as one goes to smaller sizes, with its shape a fossil-like remnant of a violent early epoch. Most D > 100-km asteroids, however, are primordial, with their physical properties set by planetesimal formation and accretion processes. The main-belt size distribution as a whole has evolved into a collisional steady state, and it has possibly been in that state for billions of years. Asteroid families provide a critical historical record of main-belt collisions. The heavily depleted and largely dispersed "ghost families," however, may hold the key to understanding what happened in the primordial days of the main belt. New asteroidal fragments are steadily created by both collisions and mass shedding events via YORP spinup processes. A fraction of this population, in the form of D < 30 km fragments, go on to escape the main belt via the Yarkovsky/YORP effects and gravitational resonances, thereby creating a quasi-steady-state population of planetcrossing and near-Earth asteroids. These populations go on to bombard all inner solar system worlds. By carefully interpreting the cratering records they produce, it is possible to constrain how portions of the main-belt population have evolved with time.

show abstract

“…The average reported albedo of ten cluster members for which albedos have been measured is p V = 0.044±0.013, though, consistent with these other members also being C-type objects. No MBCs have yet been identified among the members of the cluster, although due to the cluster's young age and spectral type of its largest member, Novaković et al (2012a) hypothesized that it could be a potential MBC reservoir.…”

Section: Other Asteroid Families and Clustersmentioning

confidence: 99%

“…Another interesting group of asteroids is the Lorre cluster, named for (5438) Lorre, which was determined to be 1.9±0.3 Myr old by Novaković et al (2012a). Lorre has been classified as a C-type asteroid, and is the only object in the 19-member cluster to have had its spectral class determined.…”

Section: Other Asteroid Families and Clustersmentioning

confidence: 99%

Asteroid Family Associations of Active Asteroids

Hsieh

Novaković

Kim

et al. 2018

Self Cite

View full text Add to dashboard Cite

We report on the results of a systematic search for associated asteroid families for all active asteroids known to date. We find that 10 out of 12 main-belt comets (MBCs) and 5 out of 7 disrupted asteroids are linked with known or candidate families, rates that have ∼0.1% and ∼6% probabilities, respectively, of occurring by chance, given an overall family association rate of 37% for asteroids in the inner solar system. We find previously unidentified family associations between 238P/Read and the candidate Gorchakov family, 311P/PANSTARRS and the candidate Behrens family, 324P/La Sagra and the Alauda family, 354P/LINEAR and the Baptistina family, P/2013 R3-B (Catalina-PANSTARRS) and the Mandragora family, P/2015 X6 (PANSTARRS) and the Aeolia family, P/2016 G1 (PANSTARRS) and the Adeona family, and P/2016 J1-A/B (PANSTARRS) and the Theobalda family. All MBCs with family associations belong to families that contain asteroids with primitive taxonomic classifications and low average reported albedos (p V 0.10), while disrupted asteroids with family associations belong to families that contain asteroids that span wider ranges of taxonomic types and average reported albedos (0.06 < p V < 0.25). These findings are consistent with MBC activity being closely correlated to composition (i.e., whether an object is likely to contain ice), while disrupted asteroid activity is not as sensitive to composition. Given our results, we describe a sequence of processes by which the formation of young asteroid families could lead to the production of present-day MBCs.

show abstract

Recent collisional jet from a primitive asteroid

Cited by 18 publications

References 78 publications

Identification and Dynamical Properties of Asteroid Families

Identification and Dynamical Properties of Asteroid Families

The Collisional Evolution of the Main Asteroid Belt

Asteroid Family Associations of Active Asteroids

Contact Info

Product

Resources

About