  We present Atacama Large Millimeter/submillimeter Array observations of the
$\sim$10 kAU environment surrounding 21 protostars in the Orion A molecular
cloud tracing outflows. Our sample is composed of Class 0 to flat-spectrum
protostars, spanning the full $\sim$1 Myr lifetime. We derive the angular
distribution of outflow momentum and energy profiles and obtain the first
two-dimensional instantaneous mass, momentum, and energy ejection rate maps
using our new approach: the Pixel Flux-tracing Technique (PFT). Our results
indicate that by the end of the protostellar phase, outflows will remove
$\sim$2 to 4 M$_\odot$ from the surrounding $\sim$1 M$_\odot$ low-mass core.
These high values indicate that outflows remove a significant amount of gas
from their parent cores and continuous core accretion from larger scales is
needed to replenish core material for star formation. This poses serious
challenges to the concept of ``cores as well-defined mass reservoirs", and
hence to the simplified core-to-star conversion prescriptions. Furthermore, we
show that cavity opening angles, and momentum and energy distributions all
increase with the protostar evolutionary stage. This is clear evidence that
even garden-variety protostellar outflows: (a) effectively inject energy and
momentum into their environments on $10$ kAU scales, and (b) significantly
disrupt their natal cores, ejecting a large fraction of the mass that would
have otherwise fed the nascent star. Our results support the conclusion that
protostellar outflows have a direct impact on how stars get their mass, and
that the natal sites of individual low-mass star formation are far more dynamic
than commonly accepted theoretical paradigms.
