Supernova Kicks and Dynamics of Compact Remnants in the Galactic Centre
  The Galactic Centre (GC) is a unique place to study the extreme dynamical
processes occurring near a super-massive black hole (SMBH). Here we investigate
the role of supernova (SN) explosions occurring in massive binary systems lying
in a disc-like structure within the innermost parsec. We use a regularized
algorithm to simulate 30,000 isolated three-body systems composed of a stellar
binary orbiting the SMBH. We start the integration when the primary member
undergoes a SN explosion, and we analyze the impact of SN kicks on the orbits
of stars and compact remnants. We find that SN explosions scatter the lighter
stars in the pair on completely different orbits, with higher eccentricity and
inclination. In contrast, stellar-mass black holes (BHs) and massive stars
retain memory of the orbit of their progenitor star. Our results suggest that
SN kicks are not sufficient to eject BHs from the GC. We thus predict that all
BHs that form in situ in the central parsec of our Galaxy remain in the GC,
building up a cluster of dark remnants. In addition, the change of NS orbits
induced by SNe may partially account for the observed dearth of NSs in the GC.
About 40 per cent of remnants stay bound to the stellar companion after the
kick; we expect up to 70 per cent of them might become X-ray binaries through
Roche-lobe filling. Finally, the eccentricity of some light stars becomes > 0.7
as an effect of the SN kick, producing orbits similar to those of the G1 and G2
dusty objects.
