Asteroid families interacting with secular resonances

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10385777" target="_blank" >RIV/00216208:11320/18:10385777 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1016/j.pss.2018.03.009" target="_blank" >https://doi.org/10.1016/j.pss.2018.03.009</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.pss.2018.03.009" target="_blank" >10.1016/j.pss.2018.03.009</a>

Result language

angličtina

Original language name

Asteroid families interacting with secular resonances

Original language description

Asteroid families are formed as the result of collisions. Large fragments are ejected with speeds of the order of the escape velocity from the parent body. After a family has been formed, the fragments&apos; orbits evolve in the space of proper elements because of gravitational and non-gravitational perturbations, such as the Yarkovsky effect. Disentangling the contribution to the current orbital position of family members caused by the initial ejection velocity field and the subsequent orbital evolution is usually a difficult task. Among the more than 100 asteroid families currently known, some interact with linear and non-linear secular resonances. Linear secular resonances occur when there is a commensurability between the precession frequency of the longitude of the pericenter (g) or of the longitude of node (s) of an asteroid and a planet, or a massive asteroid. The linear secular resonance most effective in increasing an asteroid eccentricity is the nu(6), that corresponds to a commensurability between the precession frequency g of an asteroid and Saturn&apos;s g(6). Non-linear secular resonances involve commensurabilities of higher order, and can often be expressed as combinations of linear secular resonances. This is the case, for instance, of the z(k) = k(g-g(6)) + (s-s(6)) resonances. Asteroid families that are crossed by, or even have a large portion of their members, in secular resonances are of particular interest in dynamical astronomy. First, they often provide a clear evidence of asteroid orbit evolution due to the Yarkovsky effect. Second, conserved quantities of secular dynamics can be used to set valuable constraints on the magnitude of the original ejection velocity field. For the case of the nu(6), secular resonance, objects in anti-aligned (paradoxal) librating states can be prevented to achieve high values of eccentricity and remain long-term stable (the case for members of the Tina family). Finally, by changing the value of inclination of family members, and, indirectly, of the nu(w) component of the observed ejection velocity field, nodal secular resonances with massive asteroids or dwarf planets, such as the s-sc secular resonance with Ceres, can cause nu(w) to become more and more leptokurtic (i.e., more peaked and with larger tails than that of a Gaussian distribution). By simulating fictitious asteroid families and by requiring that the current value of the Pearson kurtosis of nu(w), gamma(2) (nu(w)), be attained, independent constraints on the value of families ages can be obtained for families affected by these kinds of resonances.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA13-01308S" target="_blank" >GA13-01308S: Dynamics of small bodies in the solar system</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2018

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Planetary and Space Science

ISSN

0032-0633

e-ISSN

—

Volume of the periodical

157

Issue of the periodical within the volume

Neuveden

Country of publishing house

US - UNITED STATES

Number of pages

10

Pages from-to

72-81

UT code for WoS article

000435052100009

EID of the result in the Scopus database

2-s2.0-85044758602