Evolution of Supernova Remnants near the Galactic Center

TL;DR

This paper develops an analytic model for supernova remnants evolving near the galactic center, accounting for the unique wind-swept environment, and applies it to interpret observed remnants and neutron stars.

Contribution

It introduces a new analytic theory for supernova remnants in stellar wind environments and verifies it with hydrodynamic simulations, explaining their morphologies and associations near the galactic center.

Findings

Supernova remnants near the galactic center evolve faster and are non-spherical.

Three possible morphologies for SNRs in wind environments are identified.

The study confirms the association between SGR A's bipolar lobes and SGR J1745-2900.

Abstract

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.