Most stars form in multiple systems, profoundly influencing numerous astronomical phenomena intrinsically linked to multiplicity. However, our knowledge of the process by which multiple stellar systems form remains incomplete and is biased toward nearby molecular clouds forming only low-mass stars, which do not represent the typical stellar population of the Galaxy. Most stars form within...
The formation of stellar multiples is a frequent occurrence during the formation and evolution of massive stars. The characterisation of stellar multiplicity rates, separations, and mass ratios is a crucial input for star formation theories, and for investigating how the natal clusters influence the process. However, the multiplicity of young, massive stars remains poorly understood because of...
Some studies indicate that OB associations are not just structures that evolved from dispersing dense stellar clusters, but most likely were formed in a configuration similar to how they appear today - i.e. as an assembly of loose stellar groups. Early evolution of multiple stellar systems in such low density subgroups might be significantly different from their evolution in a dense stellar...
The question of the formation of massive stars, and massive binaries in particular is still very open. More than 90%, and perhaps all, high-mass main sequence stars are found in binary systems, while close massive binaries are responsible for some of the most energetic phenomena in the Universe. In order to understand massive stars and their evolution, it is therefore essential to find out how...
Massive stars, characterized by their extreme luminosities and crucial roles in stellar and galactic evolution, are often found in complex multiple systems. Understanding their primordial multiplicity provides key insights into their formation, interactions, and ultimate fates. One proposed mechanism to explain the relatively high rate (>30%) of massive short-period (< few months) binaries is...
Detailed observations of the multiplicity properties of massive stars probing the full mass ratio and separation range are crucial for constraining massive star and binary formation models. However, the low-mass end of the companion mass function around massive stars remains largely unexplored due to the contrast limitations of previous spectroscopic and interferometric studies. Recently, the...
