Galactic globular clusters are old, dense star systems typically containing 10 4–10 6 stars.
As an old population of stars, globular clusters contain many collapsed and degenerate …

We present a model for the concurrent formation of globular clusters (GCs) and
supermassive stars (SMSs,≳ 103 M⊙) to address the origin of the HeCNONaMgAl …

In the cores of young dense star clusters, repeated stellar collisions involving the same
object can occur. It has been suggested that this leads to the formation of an intermediate …

We present MUSE, a software framework for combining existing computational tools for
different astrophysical domains into a single multiphysics, multiscale application. MUSE …

Stellar mergers are responsible for a wide variety of phenomena such as rejuvenated blue
stragglers, highly magnetised stars, spectacular transients, iconic nebulae, and stars with …

In young dense clusters repeated collisions between massive stars may lead to the
formation of a very massive star (above 100 M⊙). In the past, the study of the long-term …

The majority of massive stars are found in close binaries which:(i) are prone to merge and
(ii) are accompanied by another distant tertiary star (triples). Here, we study the evolution of …

Even though the existence of intermediate-mass black holes (IMBHs; black holes with
masses ranging between 10 2 M☉ and 10 4 M☉) has not yet been corroborated …

We explore the hypothesis that some high-velocity runaway stars attain their peculiar
velocities in the course of exchange encounters between hard massive binaries and a very …

Most back hole and neutron star progenitors are found in triples or higher multiplicity
systems. Here, we present a new triple stellar evolution code,, which simultaneously takes …