Source regions of carbonaceous meteorites and near-Earth objects

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10491335" target="_blank" >RIV/00216208:11320/24:10491335 - isvavai.cz</a>

Result on the web

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=y5DHSK5jwt" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=y5DHSK5jwt</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202450532" target="_blank" >10.1051/0004-6361/202450532</a>

Result language

angličtina

Original language name

Source regions of carbonaceous meteorites and near-Earth objects

Original language description

Context. The source regions of ordinary chondrites (similar to 80% of all falls) and large S-type near-Earth objects (NEOs; similar to 30%) have recently been identified with three young asteroid families (Karin, Koronis, Massalia) being at the origin of most ordinary chondrite falls. Aims. The present work is a continuation of our previous studies and aims to determine the source regions of the remaining meteorite and NEO classes, with an emphasis on carbonaceous chondrites (CM, CI, CO, CV, CK, CR, CH, CB, or C-ungrouped). Methods. We studied 38 individual asteroid families, including young and old ones, and determined their contributions to the NEO populations at metre and kilometre sizes using collisional and orbital models. Our models are in agreement with spectroscopic observations of NEOs, cosmic-ray exposure ages of meteorites, statistics of bolides, infrared emission from dust bands, composition of interplanetary dust particles (IDPs), and abundance of extraterrestrial helium-3. Results. We identified the Veritas, Polana, and Eos families as the primary sources of CM/CR, CI, and CO/CV/CK chondrites, respectively. Substantial contributions are also expected from CM-like Konig and CI-like Clarissa, Misa, and Hoffmeister families. The source regions of kilometre-sized bodies are generally different. The Adeona family is by far the main source of CM-like NEOs, whereas the Polana (low-i) and Euphrosyne (high-i) families are at the origin of most CI-like NEOs. The Polana family is the likely source of both Ryugu and Bennu. We were able to link spectroscopically and dynamically several NEOs to the Baptistina family. Finally, it appears that the pre-atmospheric flux of carbonaceous chondrites at metre sizes is about the same as that of ordinary chondrites. Given the difference in fall statistics between the two groups (80% versus 4.4%), this implies either substantial atmospheric fragmentation of carbonaceous bodies at the level of similar to 0.5 MPa or destruction by thermal cracking and water desorption. Conclusions. The source regions of most meteorites and kilometre-sized NEOs have now been determined, including some minor classes such as enstatite chondrites and achondrites (Nysa, Hungaria), acapulcoites and lodranites (Iannini). Future work should focus on the few remaining classes (essentially, iron meteorites, pallasites, and ureilites).

Czech name

—

Czech description

—

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/GA21-11058S" target="_blank" >GA21-11058S: Orbital and chemical evolution of emerging planetary systems</a><br>

Continuities

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

Publication year

2024

Confidentiality

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

Name of the periodical

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

689

Issue of the periodical within the volume

září

Country of publishing house

FR - FRANCE

Number of pages

24

Pages from-to

A183

UT code for WoS article

001322521400023

EID of the result in the Scopus database

2-s2.0-85204292319