On the age of the Nele asteroid family

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10385775" target="_blank" >RIV/00216208:11320/18:10385775 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/sty777" target="_blank" >https://doi.org/10.1093/mnras/sty777</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/sty777" target="_blank" >10.1093/mnras/sty777</a>

Jazyk výsledku

angličtina

Název v původním jazyce

On the age of the Nele asteroid family

Popis výsledku v původním jazyce

The Nele group, formerly known as the Iannini family, is one of the youngest asteroid families in the main belt. Previously, it has been noted that the pericentre longitudes (omega) over bar and nodal longitudes Omega of its largest member asteroids are clustered at the present time, therefore suggesting that the collisional break-up of parent body must have happened recently. Here, we verify this conclusion by detailed orbit-propagation of a synthetic Nele family and show that the current level of clustering of secular angles of the largest Nele family members requires an approximate age limit of 4.5 Myr. Additionally, we make use of an updated and largely extended Nele membership to obtain, for the first time, an age estimate of this family using the backward integration method. Convergence of the secular angles in a purely gravitational model and in a model including the non-gravitational forces caused by the Yarkovsky effect are both compatible with an age younger than 7 Myr. More accurate determination of the Nele family age would require additional data about the spin state of its members.

Název v anglickém jazyce

On the age of the Nele asteroid family

Popis výsledku anglicky

The Nele group, formerly known as the Iannini family, is one of the youngest asteroid families in the main belt. Previously, it has been noted that the pericentre longitudes (omega) over bar and nodal longitudes Omega of its largest member asteroids are clustered at the present time, therefore suggesting that the collisional break-up of parent body must have happened recently. Here, we verify this conclusion by detailed orbit-propagation of a synthetic Nele family and show that the current level of clustering of secular angles of the largest Nele family members requires an approximate age limit of 4.5 Myr. Additionally, we make use of an updated and largely extended Nele membership to obtain, for the first time, an age estimate of this family using the backward integration method. Convergence of the secular angles in a purely gravitational model and in a model including the non-gravitational forces caused by the Yarkovsky effect are both compatible with an age younger than 7 Myr. More accurate determination of the Nele family age would require additional data about the spin state of its members.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA18-06083S" target="_blank" >GA18-06083S: Vývoj pevných těles v protoplanetárních discích a během kolizí</a><br>

Návaznosti

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

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Svazek periodika

477

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

10

Strana od-do

1308-1317

Kód UT WoS článku

000432660300091

EID výsledku v databázi Scopus

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