English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Context. A lot of photometric data is produced by surveys such as Pan-STARRS,LONEOS, WISE or Catalina. These data are a rich source of information about thephysical properties of asteroids. There are several possible approaches forutilizing these data. Lightcurve inversion is a typical method that works withindividual asteroids. Our approach in this paper is statistical when we focusedon large groups of asteroids like dynamical families and taxonomic classes, andthe data were not sufficient for individual models.  Aims. Our aim was to study the distributions of shape elongation $b/a$ andthe spin axis latitude $\beta$ for various subpopulations of asteroids and tocompare our results, based on Pan-STARRS1 survey, with statistics previouslydone using different photometric data (Lowell database, WISE data).  Methods. We use the LEADER algorithm to compare the $b/a$ and $\beta$distributions for different subpopulations of asteroids. The algorithm createsa cumulative distributive function (CDF) of observed brightness variations, andcomputes the $b/a$ and $\beta$ distributions using analytical basis functionsthat yield the observed CDF. A variant of LEADER is used to solve the jointdistributions for synthetic populations to test the validity of the method.  Results. When comparing distributions of shape elongation for groups ofasteroids with different diameters $D$, we found that there are no differencesfor $D < 25$ km. We also constructed distributions for asteroids with differentrotation periods and revealed that the fastest rotators with $P = 0 - 4$ h aremore spheroidal than the population with $P = 4 - 8$ h.

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