We present sub-millimeter and mid-infrared images of the circumstellar disk around the nearby F2V star \eta Corvi .
The disk is resolved at 850 \mu m with a size of \sim 100 AU .
At 450 \mu m the emission is found to be extended at all position angles , with significant elongation along a position angle of 130 \pm 10 ^ { \circ } ; at the highest resolution ( 9 \farcs 3 ) this emission is resolved into two peaks which are to within the uncertainties offset symmetrically from the star at 100 AU projected separation .
Modeling the appearance of emission from a narrow ring in the sub-mm images shows the observed structure can not be caused by an edge-on or face-on axisymmetric ring ; the observations are consistent with a ring of radius 150 \pm 20 AU seen at 45 \pm 25 ^ { \circ } inclination .
More face-on orientations are possible if the dust distribution includes two clumps similar to Vega ; we show how such a clumpy structure could arise from the migration over 25 Myr of a Neptune mass planet from 80-105 AU .
The inner 100 AU of the system appears relatively empty of sub-mm emitting dust , indicating that this region may have been cleared by the formation of planets , but the disk emission spectrum shows that IRAS detected an additional hot component with a characteristic temperature of 370 \pm 60 K ( implying a distance of 1-2 AU ) .
At 11.9 \mu m we found the emission to be unresolved with no background sources which could be contaminating the fluxes measured by IRAS .
The age of this star is estimated to be \sim 1 Gyr .
It is very unusual for such an old main sequence star to exhibit significant mid-IR emission .
The proximity of this source makes it a perfect candidate for further study from optical to mm wavelengths to determine the distribution of its dust .