We combine new VLA D array HI data of NGC 2613 with previous high resolution data to show new disk-halo features in this galaxy .
The global HI distribution is modeled in detail using a technique which can disentangle the effects of inclination from scale height and can also solve for the average volume density distribution in and perpendicular to the disk .
The model shows that the galaxy ’ s inclination is on the low end of the range given by Chaves & Irwin ( 2001 ) and that the HI disk is thin ( z _ { e } = 188 pc ) , showing no evidence for halo .

Numerous discrete disk-halo features are observed , however , achieving z heights up to 28 kpc from mid-plane .
One prominent feature in particular , of mass , 8 \times 10 ^ { 7 } M _ { \odot } and height , 22 kpc , is seen on the advancing side of the galaxy at a projected galactocentric radius of 15.5 kpc .
If this feature achieves such high latitudes because of events in the disk alone , then input energies of order \sim 10 ^ { 56 } ergs are required .
We have instead investigated the feasibility of such a large feature being produced via buoyancy ( with drag ) within a hot , pre-existing X-ray corona .
Reasonable plume densities , temperatures , stall height ( \sim 11 kpc ) , outflow velocities and ages can indeed be achieved in this way .
The advantage of this scenario is that the input energy need only be sufficient to produce blow-out , a condition which requires a reduction of three orders of magnitude in energy .
If this is correct , there should be an observable X-ray halo around NGC 2613 .