Orbital and Absolute Magnitude Distribution of Hilda Population

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Orbital and Absolute Magnitude Distribution of Hilda Population

Popis výsledku v původním jazyce

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&lt;overline&gt;=0.32 +/- 0.04 with a slight dependence on H (significantly smaller than Jupiter Trojans with gamma&lt;overline&gt;=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 &lt;= 16, but this number may increase to 60% of families when their location in the orbital space is further improved in the future.

Název v anglickém jazyce

Orbital and Absolute Magnitude Distribution of Hilda Population

Popis výsledku anglicky

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&lt;overline&gt;=0.32 +/- 0.04 with a slight dependence on H (significantly smaller than Jupiter Trojans with gamma&lt;overline&gt;=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 &lt;= 16, but this number may increase to 60% of families when their location in the orbital space is further improved in the future.

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/GA25-16507S" target="_blank" >GA25-16507S: Raný orbitální vývoj planet a výzkum populací asteroidů</a><br>

Návaznosti

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

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

The Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Svazek periodika

169

Číslo periodika v rámci svazku

5

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

31

Strana od-do

242

Kód UT WoS článku

001458735300001

EID výsledku v databázi Scopus

2-s2.0-105002414663