The formation of protostars and their disks has been understood as the result of the
gravitational collapse phase of an accumulation of dense gas that determines the mass …

Stars are among the most fundamental structures of our Universe. They comprise most of the
baryonic and luminous mass of galaxies; synthesize heavy elements; and inject mass …

Age is one of the most fundamental parameters of a star, yet it is one of the hardest to
determine as it requires modelling various aspects of stellar formation and evolution. When …

Abstract We present Atacama Large Millimeter/submillimeter Array observations of the∼
10,000 au environment surrounding 21 protostars in the Orion A molecular cloud tracing …

The stellar initial mass function (IMF) is commonly interpreted to be a scale-invariant
probability density distribution function (PDF) such that many small clusters yield the same …

Abstract Investigating Protostellar Accretion (IPA) is a JWST Cycle 1 GO program that uses
NIRSpec integral field units and MIRI Medium Resolution Spectrograph to obtain 2.9–28 μm …

We demonstrate that planet formation via pebble accretion is sensitive to external
photoevaporation of the outer disc. In pebble accretion, planets grow by accreting from a flux …

Most stars form in highly clustered environments within molecular clouds, but eventually
disperse into the distributed stellar field population. Exactly how the stellar distribution …

We perform simulations of star cluster formation to investigate the morphological evolution of
embedded star clusters in the earliest stages of their evolution. We conduct our simulations …

We introduce the star formation and supernova (SN) feedback model of the satin (S
imulating A GNs T hrough I SM with N on-Equilibrium Effects) project to simulate the …