Star formation is governed by many complex physical processes that intertwine at all scales, some of which include turbulent motions, mass inflow, thermal pressure and magnetic fields. These physical processes have direct impacts on the formation of many types of systems (e.g., single stars, multiple star systems, stellar clusters). Recent work studying a survey of all starless cores in Orion...
Massive stars, those several times the mass of the Sun, are typically found in multiple-star systems. A key unresolved question in astronomy is how close binary-star systems, those with separations ≲ 1 au, form. Because protostellar objects are generally too extended to initially fit into these tight configurations, migration is considered to play an essential in their formation. In this talk,...
We explore the multiplicity statistics (semi-major axis, period, eccentricity, degree of dynamical biasing, binary and tertiary mass ratios, mutual orbital inclination, and ejection velocity) of stars born in small-N subclusters using numerical N-body experiments. In these experiments, subclusters are evolved as if they are the fragmentation products of a single isolated prestellar core from...
Binaries in dense environments are traditionally classified as soft or hard based on their binding energy relative to the kinetic energy of surrounding stars. Heggie's law suggests that stellar encounters tend to soften soft binaries and harden hard binaries, altering their separations. However, interactions with gas in such environments can significantly modify this behavior. This study...
Traditionally, star formation has been viewed as a distinct phase where a collapsing gas and dust cloud forms a protostar and its disk. However, recent observations and simulations reveal that star formation is prolonged and dynamic, especially in binary and multiple star systems. Chaotic late infall continues long after the initial collapse, feeding planet-forming disks through filamentary...
Observations show that most main sequence stars, unlike our Sun, are members of systems with two or more stars. Exactly how these systems form and when these stars become gravitationally bound together remains debated, since resolving the earliest stages of star formation is challenging. I will discuss how multiple star systems form and evolve in simulations of star cluster formation...
Multiplicity is a common outcome of the star formation process. Previous stellar multiplicity studies in young, star-forming regions have identified a trend in wide (100 - 10,000 au) companion frequency with stellar density where higher frequencies are found in lower density regions, but it is unclear if this is primordial due to star formation physics or from dynamical interactions....
