Our bimetric spacetime model of glitching pulsars is applied to the remnant of GW170817 .
Accordingly , pulsars are born with embryonic incompressible superconducting gluon-quark superfluid cores ( SuSu-matter ) that are embedded in Minkowski spacetime , whereas the ambient compressible and dissipative media ( CDM ) are imbedded in curved spacetime .
As pulsars cool down , the equilibrium between both spacetime is altered , thereby triggering the well-observed glitch phenomena .

Based thereon and assuming all neutron stars ( NSs ) to be born with the same initial mass of M _ { NS } ( t = 0 ) \approx 1.25 { M _ { \odot } } , we argue that the remnant of GW170817 should be a relatively faint NS with a hypermassive central core made of SuSu-matter .
The effective mass and radius of the remnant are predicted to be \mathcal { M } _ { tot } = 3.351 { M _ { \odot } } and R _ { rem } = 10.764 km , whereas the mass of the enclosed SuSu-core is \mathcal { M } _ { core } = 1.7 { M _ { \odot } } . Here , about 1 / 2 ~ { } \mathcal { M } _ { core } is an energy enhancement triggered by the phase transition of the gluon-quark-plasma from the microscopic into macroscopic scale . The current compactness of the remnant is \alpha _ { c } = 0.918 , but predicted to increase as the CDM cool down to finally turn the remnant invisible and therefore to an excellent black hole candidate .

Keywords : Relativity : numerical , general , black hole physics –magnetars– neutron stars–pulsars— superfluidity –superconductivity–gluons–quarks–plasmas— QCD