Cascade disruptions in asteroid clusters

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10422092" target="_blank" >RIV/00216208:11320/20:10422092 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=BpxZbDh0hB" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=BpxZbDh0hB</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.icarus.2019.113554" target="_blank" >10.1016/j.icarus.2019.113554</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Cascade disruptions in asteroid clusters

Popis výsledku v původním jazyce

We studied asteroid clusters suggesting a possibility of at least two disruption events in their recent history (&lt;= 5Myr). We searched for new members of known asteroid pairs and clusters and we verified their membership using backward orbital integrations. We found four asteroid clusters, namely the clusters of (11842) Kap&apos;bos, (14627) Emilkowalski, (63440) 2001 MD30 and (157123) 2004 NW5 that show at least two secondary separation events that occurred at significantly different times. We considered a possible formation mechanism for these clusters: The parent of an asteroid cluster was spun up to its critical rotation frequency, underwent a rotation fission and was slowed down by escape of the newly formed secondary/ies. Then the YORP effect spun up the primary again and it reached its critical rotation frequency and underwent another fission. We created a simple model to test whether the scenario of two rotation fission events of a parent primary induced via the YORP effect is possible for the four clusters. We obtained a good agreement between the model and the cluster properties for the clusters of Kap&apos;bos and (63440). For the cluster of Emilkowalski, our model explained the unusually slow rotation of the primary. However, the time needed for the primary to reach its critical frequency after the first fission event was predicted to be too long by a factor of several. We suspect, considering also its D type taxonomic classification and the existence of a dust band associated with the cluster, that the asteroid Emilkowalski may actually be a cometary nucleus. Regarding the cluster of (157123), the final rotational frequency of the primary after the last fission event predicted by our model is in a good agreement with the observed rotation frequency of (157123). However, a separation of the older secondary is not possible in our model due to the deficiency of free energy needed for an escape of the large secondary. This could be due to an error in the H value of the secondary or the possibility that we did not find the real primary of this cluster.y

Název v anglickém jazyce

Cascade disruptions in asteroid clusters

Popis výsledku anglicky

We studied asteroid clusters suggesting a possibility of at least two disruption events in their recent history (&lt;= 5Myr). We searched for new members of known asteroid pairs and clusters and we verified their membership using backward orbital integrations. We found four asteroid clusters, namely the clusters of (11842) Kap&apos;bos, (14627) Emilkowalski, (63440) 2001 MD30 and (157123) 2004 NW5 that show at least two secondary separation events that occurred at significantly different times. We considered a possible formation mechanism for these clusters: The parent of an asteroid cluster was spun up to its critical rotation frequency, underwent a rotation fission and was slowed down by escape of the newly formed secondary/ies. Then the YORP effect spun up the primary again and it reached its critical rotation frequency and underwent another fission. We created a simple model to test whether the scenario of two rotation fission events of a parent primary induced via the YORP effect is possible for the four clusters. We obtained a good agreement between the model and the cluster properties for the clusters of Kap&apos;bos and (63440). For the cluster of Emilkowalski, our model explained the unusually slow rotation of the primary. However, the time needed for the primary to reach its critical frequency after the first fission event was predicted to be too long by a factor of several. We suspect, considering also its D type taxonomic classification and the existence of a dust band associated with the cluster, that the asteroid Emilkowalski may actually be a cometary nucleus. Regarding the cluster of (157123), the final rotational frequency of the primary after the last fission event predicted by our model is in a good agreement with the observed rotation frequency of (157123). However, a separation of the older secondary is not possible in our model due to the deficiency of free energy needed for an escape of the large secondary. This could be due to an error in the H value of the secondary or the possibility that we did not find the real primary of this cluster.y

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA17-00774S" target="_blank" >GA17-00774S: Fyzikální vlastnosti a evoluční procesy subkilometrových asteroidů</a><br>

Návaznosti

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

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název periodika

Icarus

ISSN

0019-1035

e-ISSN

—

Svazek periodika

338

Číslo periodika v rámci svazku

březen

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

11

Strana od-do

—

Kód UT WoS článku

000516888000037

EID výsledku v databázi Scopus

2-s2.0-85075333356