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

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - 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)

Project

<a href="/en/project/GA15-04816S" target="_blank" >GA15-04816S: A big picture of the main asteroid belt - physical properties of asteroids derived by inversion of optical and infrared photometry</a><br>

Continuities

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

Publication year

2018

Confidentiality

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

Name of the periodical

Astronomy &amp; Astrophysics [online]

ISSN

1432-0746

e-ISSN

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Volume of the periodical

611

Issue of the periodical within the volume

Neuveden

Country of publishing house

FR - FRANCE

Number of pages

10

Pages from-to

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UT code for WoS article

000429093500003

EID of the result in the Scopus database

2-s2.0-85045197138