  Understanding the origins of stellar radio emission can provide invaluable
insight into the strength and geometry of stellar magnetic fields and the
resultant space weather environment experienced by exoplanets. Here, we present
the first model capable of predicting radio emission through the electron
cyclotron maser instability using observed stellar magnetic maps of low-mass
stars. We determine the structure of the coronal magnetic field and plasma
using spectropolarimetric observations of the surface magnetic fields and the
X-ray emission measure. We then model the emission of photons from the
locations within the corona that satisfy the conditions for electron cyclotron
maser emission. Our model predicts the frequency, and intensity of radio
photons from within the stellar corona.
  We have benchmarked our model against the low-mass star V374 Peg. This star
has both radio observations from the Very Large Array and a nearly simultaneous
magnetic map. Using our model we are able to fit the radio observations of V374
Peg, providing additional evidence that the radio emission observed from
low-mass stars may originate from the electron cyclotron maser instability. Our
model can now be extended to all stars with observed magnetic maps to predict
the expected frequency and variability of stellar radio emission in an effort
to understand and guide future radio observations of low-mass stars.
