An interferometric study of B star multiplicity

TL;DR

This study uses interferometry to analyze the multiplicity of B stars, revealing that approximately 72% are in multiple systems, with a significant number being binaries, triples, or quadruples, and combining data from various sources for comprehensive results.

Contribution

First interferometric survey of B star multiplicity over 0.5-35 au, providing new statistics and insights into their companion fractions and system configurations.

Findings

Approximately 72% of B stars are in multiple systems.

Binary systems are the most common, followed by triples and quadruples.

Including spectroscopic and Gaia data increases the overall multiplicity fraction to 88%.

Abstract

Massive stars can have extreme effects on their environments from local to galactic scales. While O star multiplicity has been studied over a broad separation range (to the point where absolute masses of these systems have been determined and investigations into multiple system formation and interactions have been performed), studies of B star multiplicity are lacking. Using interferometry, we investigated the multiplicity of a statistically significant sample of B stars over a range of separations (~0.5-35 au, given that the average distance to our sample is 412 pc). We analysed high angular resolution interferometric data taken with VLTI/PIONIER for a sample of 32 B stars. Using parametric modelling of the closure phases and visibilities, we determined best-fitting models to each of the systems and investigated whether each source was best represented by a single star or a higher-order system. The detection limits were calculated for companions to determine whether they were significant. We then combined our findings from the interferometric data with results from a literature search to determine whether other companions were reported at different separation ranges. Within the interferometric range 72+/-8% of the B stars are resolved as multiple systems. The most common type of system is a binary system, followed by single stars, triple systems, and quadruple systems. The interferometric companion fraction derived for the sample is 1.88+/-0.24. When we accounted for spectroscopic companions that have been confirmed in the literature and wide companions inferred from Gaia data in addition to the companions we found with interferometry, we obtain multiplicity and companion fractions of 0.88+/-0.06 and 2.31+/-0.27, respectively, for our sample. The number of triple systems increases to the second-most populous type of system when accounting for spectroscopic companions.