A Catalog of Multiplicity among Bright Stellar Systems

TL;DR

This paper catalogs bright stellar systems with magnitude brighter than 6.00, analyzing their multiplicity frequencies, distributions, and implications for star formation and galactic evolution, highlighting data limitations and uncertainties.

Contribution

It provides a comprehensive catalog of bright stellar system multiplicities and analyzes their distributions, offering insights into stellar formation and evolution.

Findings

4559 bright systems identified, including the Sun

Multiplicity frequencies range from 1 to 7 components

Higher multiplicities are more common in brighter, more massive stars

Abstract

We consider the multiplicity of stellar systems with (combined) magnitude brighter than 6.00 in Hipparcos magnitudes. We identify 4559 such bright systems (including the Sun), and the frequencies of multiplicities 1, 2,..., 7 are found to be 2718, 1437, 285, 86, 20, 11 and 2. We discuss the uncertainties, which are substantial. We also consider the distributions of periods of orbits and sub-orbits. We note that for the even more restricted set of 478 systems with V_H <= 4.00 the proportions of higher multiples up to sextuple are progressively larger (213, 179, 54, 19, 8, 5), suggesting substantial incompleteness in even the reasonably well-studied larger sample. This sample can be seen as relatively thoroughly studied for multiplicity, and reasonably representative of stars more massive than the Sun. But the restriction to V_H <= 6 means that our sample contains hardly any systems where all components are low-mass main-sequence stars (K or M). Data on multiplicity is important as a constraint on (a) the star-formation problem, (b) the problem of the evolution of the Galactic stellar population, and (c) the interaction of dynamics and evolution through the effect of Kozai cycles. We discuss these topics briefly.