Using the Very Long Baseline Array (VLBA) and the Very Large Array (VLA), w
e have observed the quiescent coronal microwave emission from the active RS
CVn system UX Ari. We complement the data with X-ray information obtained
from the X-ray satellite ASCA. The 8.4 GHz continuum radio source is resolv
ed on linear scales comparable to the projected separation of the binary co
mponents, indicating the existence of large magnetic structures. Circular p
olarization is detected, and a polarization gradient across the radio sourc
e is observed, suggesting the existence of interacting magnetic fields betw
een the components or a large magnetic loop anchored to one component. The
VLBA lower limit to the brightness temperature (similar to 26 MK) is close
to the broad temperature peak in the contemporaneous emission measure distr
ibution seen by ASCA; we examine the possibility that the quiescent radio f
lux may be gyrosynchrotron emission from a thermal electron energy distribu
tion. We find that no simple thermal model can reproduce the observed spect
ral index of the quiescent emission.