Distribution of shape elongations of main belt asteroids derived from Pan-STARRS1 photometry

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10385760" target="_blank" >RIV/00216208:11320/18:10385760 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/201731554" target="_blank" >https://doi.org/10.1051/0004-6361/201731554</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201731554" target="_blank" >10.1051/0004-6361/201731554</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Distribution of shape elongations of main belt asteroids derived from Pan-STARRS1 photometry

Popis výsledku v původním jazyce

Context. A considerable amount of photometric data is produced by surveys such as Pan-STARRS, LONEOS, WISE, or Catalina. These data are a rich source of information about the physical properties of asteroids. There are several possible approaches for using these data. Light curve inversion is a typical method that works with individual asteroids. Our approach in focusing on large groups of asteroids, such as dynamical families and taxonomic classes, is statistical; the data are not sufficient for individual models. Aims. Our aim is to study the distributions of shape elongation b/a and the spin axis latitude beta for various subpopulations of asteroids and to compare our results, based on Pan-STARRS1 survey, with statistics previously carried out using various photometric databases, such as Lowell and WISE. Methods. We used the LEADER algorithm to compare the b/a and beta distributions for various subpopulations of asteroids. The algorithm creates a cumulative distributive function (CDF) of observed brightness variations, and computes the b/a and beta distributions with analytical basis functions that yield the observed CDF. A variant of LEADER is used to solve the joint distributions for synthetic populations to test the validity of the method. Results. When comparing distributions of shape elongation for groups of asteroids with different diameters D, we found that there are no differences for D &lt; 25 km. We also constructed distributions for asteroids with different rotation periods and revealed that the fastest rotators with P = 0-4 h are more spheroidal than the population with P = 4-8 h.

Název v anglickém jazyce

Distribution of shape elongations of main belt asteroids derived from Pan-STARRS1 photometry

Popis výsledku anglicky

Context. A considerable amount of photometric data is produced by surveys such as Pan-STARRS, LONEOS, WISE, or Catalina. These data are a rich source of information about the physical properties of asteroids. There are several possible approaches for using these data. Light curve inversion is a typical method that works with individual asteroids. Our approach in focusing on large groups of asteroids, such as dynamical families and taxonomic classes, is statistical; the data are not sufficient for individual models. Aims. Our aim is to study the distributions of shape elongation b/a and the spin axis latitude beta for various subpopulations of asteroids and to compare our results, based on Pan-STARRS1 survey, with statistics previously carried out using various photometric databases, such as Lowell and WISE. Methods. We used the LEADER algorithm to compare the b/a and beta distributions for various subpopulations of asteroids. The algorithm creates a cumulative distributive function (CDF) of observed brightness variations, and computes the b/a and beta distributions with analytical basis functions that yield the observed CDF. A variant of LEADER is used to solve the joint distributions for synthetic populations to test the validity of the method. Results. When comparing distributions of shape elongation for groups of asteroids with different diameters D, we found that there are no differences for D &lt; 25 km. We also constructed distributions for asteroids with different rotation periods and revealed that the fastest rotators with P = 0-4 h are more spheroidal than the population with P = 4-8 h.

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/GA15-04816S" target="_blank" >GA15-04816S: Celkový obraz hlavního pásu planetek - fyzikální vlastnosti planetek odvozené inverzí optické a infračervené fotometrie</a><br>

Návaznosti

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

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

Astronomy &amp; Astrophysics [online]

ISSN

1432-0746

e-ISSN

—

Svazek periodika

611

Číslo periodika v rámci svazku

Neuveden

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

—

Kód UT WoS článku

000429093500003

EID výsledku v databázi Scopus

2-s2.0-85045197138