Orbital and Absolute Magnitude Distribution of Hilda Population
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10511144" target="_blank" >RIV/00216208:11320/25:10511144 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=dxXrNsS.d5" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=dxXrNsS.d5</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-3881/adbe7b" target="_blank" >10.3847/1538-3881/adbe7b</a>
Alternative languages
Result language
angličtina
Original language name
Orbital and Absolute Magnitude Distribution of Hilda Population
Original language description
The Hilda population of asteroids is located in a large orbital zone of long-term stability associated with the Jupiter J3/2 mean-motion resonance. They are a sister population of the Jupiter Trojans, since both of them are likely made up of objects captured from the primordial Kuiper Belt early in the solar system history. Comparisons between the orbital and physical properties of the Hilda and Trojan populations thus represent a test of outer planet formation models. Here we use a decade of observations from the Catalina Sky Survey (G96 site) to determine the bias-corrected orbital and magnitude distributions of Hildas. We also identify collisional families and the background population by computing a new catalog of synthetic proper elements for Hildas. We model the cumulative magnitude distribution of the background population using a local power-law representation with slope gamma(H), where H is the absolute magnitude. For the largest Hildas, we find gamma similar or equal to 0.5 with large uncertainty due to the limited population. Beyond H similar or equal to 11, we find that gamma transitions to a mean value gamma<overline>=0.32 +/- 0.04 with a slight dependence on H (significantly smaller than Jupiter Trojans with gamma<overline>=0.43 +/- 0.02 ). We find that members of identified collisional families represent more than 60% of the total population (both bias counts). The bias-corrected populations contain about the same number of Hildas within the families and the background for H <= 16, but this number may increase to 60% of families when their location in the orbital space is further improved in the future.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA25-16507S" target="_blank" >GA25-16507S: Early dynamics of planets and analysis of asteroid populations</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
The Astronomical Journal
ISSN
0004-6256
e-ISSN
1538-3881
Volume of the periodical
169
Issue of the periodical within the volume
5
Country of publishing house
US - UNITED STATES
Number of pages
31
Pages from-to
242
UT code for WoS article
001458735300001
EID of the result in the Scopus database
2-s2.0-105002414663