Zooming in on Individual Star Formation: Low- and High-mass Stars
  Star formation is a multi-scale, multi-physics problem ranging from the size
scale of molecular clouds ($\sim$10s pc) down to the size scales of dense
prestellar cores ($\sim$0.1 pc) that are the birth sites of stars. Several
physical processes like turbulence, magnetic fields and stellar feedback, such
as radiation pressure and outflows, are more or less important for different
stellar masses and size scales. During the last decade a variety of
technological and computing advances have transformed our understanding of star
formation through the use of multi-wavelength observations, large scale
observational surveys, and multi-physics multi-dimensional numerical
simulations. Additionally, the use of synthetic observations of simulations
have provided a useful tool to interpret observational data and evaluate the
importance of various physical processes on different scales in star formation.
Here, we review these recent advancements in both high- ($M \gtrsim 8 \, M_{\rm
\odot}$) and low-mass star formation.
