Young asteroid families as the primary source of meteorites

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10491143" target="_blank" >RIV/00216208:11320/24:10491143 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=6HnViUqrCd" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=6HnViUqrCd</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1038/s41586-024-08006-7" target="_blank" >10.1038/s41586-024-08006-7</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Young asteroid families as the primary source of meteorites

Popis výsledku v původním jazyce

Understanding the origin of bright shooting stars and their meteorite samples is among the most ancient of astronomy-related questions, which at larger scales has human consequences(1-3). As of today, only approximately 6% of meteorite falls have been firmly linked to their sources (Moon, Mars or asteroid (4) Vesta(4-6)). Here we show that approximately 70% of meteorites originate from three recent break-ups of D &gt; 30 km asteroids that occurred 5.8, 7.6 and less than about 40 Myr ago. These break-ups, including the well-known Karin family(7), took place in the prominent yet old Koronis and Massalia families and are at the origin of the dominance of H and L ordinary chondrites among meteorite falls. These young families are distinguished among all main belt asteroids by having a uniquely high abundance of small fragments. Their size-frequency distribution remained steep for a few tens of millions of years, exceeding temporarily the production of metre-sized fragments by the largest old asteroid families (for example, Flora and Vesta). Supporting evidence includes the existence of associated dust bands(8-10), the cosmic-ray exposure ages of H-chondrite meteorites(11,12) and the distribution of the pre-atmospheric orbits of meteorites(13-15).

Název v anglickém jazyce

Young asteroid families as the primary source of meteorites

Popis výsledku anglicky

Understanding the origin of bright shooting stars and their meteorite samples is among the most ancient of astronomy-related questions, which at larger scales has human consequences(1-3). As of today, only approximately 6% of meteorite falls have been firmly linked to their sources (Moon, Mars or asteroid (4) Vesta(4-6)). Here we show that approximately 70% of meteorites originate from three recent break-ups of D &gt; 30 km asteroids that occurred 5.8, 7.6 and less than about 40 Myr ago. These break-ups, including the well-known Karin family(7), took place in the prominent yet old Koronis and Massalia families and are at the origin of the dominance of H and L ordinary chondrites among meteorite falls. These young families are distinguished among all main belt asteroids by having a uniquely high abundance of small fragments. Their size-frequency distribution remained steep for a few tens of millions of years, exceeding temporarily the production of metre-sized fragments by the largest old asteroid families (for example, Flora and Vesta). Supporting evidence includes the existence of associated dust bands(8-10), the cosmic-ray exposure ages of H-chondrite meteorites(11,12) and the distribution of the pre-atmospheric orbits of meteorites(13-15).

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/GA21-11058S" target="_blank" >GA21-11058S: Raný orbitální a chemický vývoj planetárních soustav</a><br>

Návaznosti

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

Rok uplatnění

2024

Kód důvěrnosti údajů

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

Název periodika

Nature

ISSN

0028-0836

e-ISSN

1476-4687

Svazek periodika

634

Číslo periodika v rámci svazku

8034

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

12

Strana od-do

566-577

Kód UT WoS článku

001342107700004

EID výsledku v databázi Scopus

2-s2.0-85196420231