Asteroid families: evidence of ageing of the proper elements

Icarus ◽  
2004 ◽  
Vol 169 (2) ◽  
pp. 341-356 ◽  
Author(s):  
A. Dell'Oro ◽  
G. Bigongiari ◽  
P. Paolicchi ◽  
A. Cellino
Keyword(s):  
Proper Elements ◽  
Asteroid Families

scholarly journals Asteroid Proper Elements: The Big Picture

1994 ◽  
Vol 160 ◽  
pp. 143-158 ◽  
Author(s):  
Zoran Knežević ◽  
Andrea Milani
Keyword(s):  
Point Of View ◽  
Dynamical Structure ◽  
Main Belt ◽  
Secular Resonances ◽  
Mean Motion Resonances ◽  
Mean Motion ◽  
Proper Elements ◽  
Big Picture ◽  
Linear And Nonlinear ◽  
Asteroid Families

Four perturbation theories presently used to compute asteroid proper elements are reviewed, and their results are briefly discussed (Milani and Knežević, 1990, 1992, 1994, for low to moderate eccentricity/inclination main belt objects; Lemaitre and Morbidelli, 1994, for high e, I objects; Milani, 1993, for Trojans; Schubart, 1982, 1991 for Hildas). The most important recent improvements are described, in particular those pertaining to the upgrades of the previous analytic and semianalytic solutions. The dynamical structure of the asteroid main belt, as defined by the low order mean motion resonances and by linear and nonlinear secular resonances, is considered from the point of view of the effects of these resonances on the accuracy and/or reliability of the computation of proper elements and on the reliability of the identification of asteroid families.

Families among the Hildas and Trojans

2018 ◽  
Vol 14 (A30) ◽  
pp. 24-25
Author(s):  
Tamara A. Vinogradova
Keyword(s):  
Empirical Method ◽  
Proper Elements ◽  
Asteroid Families

AbstractA search for asteroid families among the Hildas and Jupiter Trojans was performed with the use of a new set of proper elements. The proper elements were calculated by the empirical method. Besides well known families, several new probable families were found in addition.

scholarly journals 10. A Statistical Investigation of Asteroid Families: Preliminary Results

1977 ◽  
Vol 39 ◽  
pp. 327-332
Author(s):  
A. Carusi ◽  
E. Massaro
Keyword(s):  
Orbital Evolution ◽  
Statistical Investigation ◽  
Correct Identification ◽  
Physical Origin ◽  
Preliminary Results ◽  
Clustering Technique ◽  
Proper Elements ◽  
Statistical Relevance ◽  
Asteroid Families

The correct identification of asteroid families is a prerequisite for understanding their nature, their orbital evolution and their physical origin. For this reason, a statistical investigation of asteroid families has been carried out, using a new clustering technique developed by A. I. Gavrishin. Proper elements for 2764 asteroids (1810 numbered and 954 Palomar-Leiden-Survey (PLS) asteroids) have been computed. Using these data, the Gavrishin method gives only ten significant classes. Five of them are coincident with the Hirayama families 1, 2, 3, 5, and the Flora group, that cannot be univocally subdivided. The PLS families are recognized. Furthermore many small-sized families reported by several authors lose their statistical relevance.

scholarly journals Numerical mean elements for asteroid orbits

1996 ◽  
Vol 172 ◽  
pp. 165-170 ◽  
Author(s):  
Anne Lemaitre
Keyword(s):  
Body Problem ◽  
Minor Planets ◽  
Proper Elements ◽  
N Body Problem ◽  
Double Averaging ◽  
The Mean ◽  
Osculating Elements ◽  
Mean Elements ◽  
Asteroid Families

In the context of the search of asteroid families (i.e. identification of minor planets as potential fragments of an old bigger body), the calculation of proper elements plays an important role. They are quasi-invariants of the motion, obtained by a double averaging process of the restricted N-body problem; firstly the osculating elements are averaged over the short periodic terms (namely the longitudes of the asteroid and of the perturbing planets) so to get the mean elements, and secondly, the mean elements are averaged over the long periodic terms (longitudes of the pericenters and of the nodes of the asteroid and of the perturbing planets) to obtain the proper elements.

scholarly journals Asteroid Family Identification: History and State of the Art

2015 ◽  
Vol 10 (S318) ◽  
pp. 16-27 ◽  
Author(s):  
Zoran Knežević
Keyword(s):  
State Of The Art ◽  
The State ◽  
Classification Methods ◽  
Data Set ◽  
The Third ◽  
Proper Elements ◽  
The Future ◽  
History Of ◽  
Asteroid Families ◽  
Collisional Evolution

AbstractThe history of asteroid families, from their discovery back in 1918, until the present time, is briefly reviewed. Two threads have been followed: on the development of the theories of asteroid motion and the computation of proper elements, and on the methods of classification themselves. Three distinct periods can be distinguished: the first one until mid-1930s, devoted to discovery and first attempts towards understanding of the properties of families; the second one, until early 1980s, characterized by a growing understanding of their importance as key evidence of the collisional evolution; the third one, characterized by an explosion of work and results, comprises the contemporary era. An assessment is given of the state-of-the-art and possible directions for the future effort, focusing on the dynamical studies, and on improvements of classification methods to cope with ever increasing data set.

scholarly journals Secular evolution of asteroid families: the role of Ceres

2015 ◽  
Vol 10 (S318) ◽  
pp. 46-54 ◽  
Author(s):  
Bojan Novaković ◽  
Georgios Tsirvoulis ◽  
Stefano Marò ◽  
Vladimir Đošović ◽  
Clara Maurel
Keyword(s):  
Numerical Simulations ◽  
Main Belt ◽  
Secular Resonance ◽  
Secular Evolution ◽  
Secular Dynamics ◽  
Proper Elements ◽  
Post Impact ◽  
Actual Shape ◽  
Asteroid Families

AbstractWe consider the role of the dwarf planet Ceres on the secular dynamics of the asteroid main belt. Specifically, we examine the post impact evolution of asteroid families due to the interaction of their members with the linear nodal secular resonance with Ceres. First, we find the location of this resonance and identify which asteroid families are crossed by its path. Next, we summarize our results for three asteroid families, namely (1726) Hoffmeister, (1128) Astrid and (1521) Seinajoki which have irregular distributions of their members in the proper elements space, indicative of the effect of the resonance. We confirm this by performing a set of numerical simulations, showcasing that the perturbing action of Ceres through its linear nodal secular resonance is essential to reproduce the actual shape of the families.

scholarly journals What we know about Families of Asteroids

1989 ◽  
Vol 8 ◽  
pp. 273-279
Author(s):  
V. Zappala’
Keyword(s):  
Family Members ◽  
Parent Body ◽  
Classification Methods ◽  
Hypervelocity Impacts ◽  
Mass Distributions ◽  
Proper Elements ◽  
The Family ◽  
Families Of Asteroids ◽  
Asteroid Families ◽  
Degree Of Fragmentation

AbstractAsteroid families are considered for the most to represent fragments of collisional breakup of precursor bodies. If true, this offers the unique possibility to examine the interiors of large bodies and to study the processes of collision on a scale much larger than can be done in laboratory. Indeed, the general features of the mass distributions and of the ejection velocities of the family members can be interpreted in terms of collisional disruption of a parent body followed by self-gravitational reaccumulation on the largest remnant. However, several problems remain open: a) the degree of fragmentation in real families is generally lower than that observed for experimental targets; b) the relative velocities computed including also proper eccentricity and inclination differences are higher by about a factor 4 than those derived from semiaxes differences only; c) only very few of the presently proposed families have distributions of inferred mineralogies consistent with cosmochemistry. Further studies are needed, including better proper elements computation, classification methods, and new investigations on the physics of hypervelocity impacts.

scholarly journals Reconnecting groups of space debris to their parent body through proper elements

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Alessandra Celletti ◽  
Giuseppe Pucacco ◽  
Tudor Vartolomei
Keyword(s):  
Space Debris ◽  
Parent Body ◽  
Statistical Data Analysis ◽  
Proper Elements ◽  
Dynamical Features ◽  
Break Up ◽  
Osculating Elements ◽  
Original Configuration ◽  
Over Time ◽  
Asteroid Families

AbstractSatellite collisions or fragmentations generate a huge number of space debris; over time, the fragments might get dispersed, making it difficult to associate them to the configuration at break-up. In this work, we present a procedure to back-trace the debris, reconnecting them to their original configuration. To this end, we compute the proper elements, namely dynamical quantities which stay nearly constant over time. While the osculating elements might spread and lose connection with the values at break-up, the proper elements, which have been already successfully used to identify asteroid families, retain the dynamical features of the original configuration. We show the efficacy of the procedure, based on a hierarchical implementation of perturbation theory, by analyzing the following four different case studies associated to satellites that underwent a catastrophic event: Ariane 44lp, Atlas V Centaur, CZ-3, Titan IIIc Transtage. The link between (initial and final) osculating and proper elements is evaluated through tools of statistical data analysis. The results show that proper elements allow one to reconnect the fragments to their parent body.

Spin clusters inside four young asteroid groups

2020 ◽  
Vol 493 (2) ◽  
pp. 2556-2567
Author(s):  
V Carruba ◽  
L G M Ramos ◽  
F Spoto
Keyword(s):  
Numerical Simulations ◽  
Transition Region ◽  
Semimajor Axis ◽  
Family Members ◽  
Proper Elements ◽  
The Family ◽  
Induced Fission ◽  
Spin Clusters ◽  
Spin Pairs ◽  
Asteroid Families

ABSTRACT Asteroid groups may either form because of collisions or because of spin induced fission. Recently it has been shown that young spin clusters tend to form more frequently in young collisional families than in older groups. Here, we study the occurrence of spin clusters inside four very recently identified asteroid groups: the (525) Adelaide, (2258) Viipuri, (6142) Tantawi, and (18429) (1994 AO1) groups. Using combinations of techniques based on backward numerical simulations, we identify four spin pairs among the family members. All groups have fractions of observed spin clusters well above 5 per cent, so confirming an observed trend for other young asteroid groups. The (2258) Viipuri and (18429) (1994 AO1) groups are compatible with an origin as a spin clusters themselves, and could be other occurrences of cascade spin clusters, as recently detected in other asteroid groups. Finally, the separation between collisional asteroid families and spin clusters in domains of dispersion of proper semimajor axis, σa, versus age seems to be more complex than previously thought. While spin clusters tend to be much more compact in proper elements than collisional families, there appears to be a transition region in σa where both the groups be found.

Sign in / Sign up

Export Citation Format

Share Document