  Supernovae near the galactic center evolve differently from regular galactic
supernovae. This is mainly due to the environment into which the supernova
remnants propagate. Instead of a static, uniform density medium, SNRs near the
galactic center propagate into a wind swept environment with a velocity away
from the galactic center, and a graded density profile. This causes these SNRs
to be non - spherical, and to evolve faster than their galactic counterparts.
We develop an analytic theory for the evolution of explosions within a stellar
wind, and verify it using a hydrodynamic code. We show that such explosions can
evolve in one of three possible morphologies. Using these results we discuss
the association between the two SNRs (SGR East and SGR A's bipolar radio/X-ray
Lobes) and the two neutron stars (the cannonball and SGR J1745-2900) near the
galactic center. We show that, given the morphologies of the SNR and positions
of the neutron stars, the only possible association is between SGR A's bipolar
radio/X-ray Lobes and SGR J1745-2900. The compact object created in the
explosion of SGR East remains undetected, and the SNR of the supernova that
created the cannonball has already disappeared.
