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 ...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 (<em>NSs</em>) to be born with the same initial mass of <img src="Edit_4d2d9e5f-812f-41d7-9422-5cfb3fc10997.bmp" alt="" />, we argue that the remnant of GW170817 should be a relatively faint <em>NS</em> with a massive central core made of SuSu-matter. The effective mass and radius of the remnant are predicted to be <img src="Edit_6702e3a8-abff-41f9-a45b-a2bc1e6c61b0.bmp" alt="" /> and <span style="white-space:nowrap;"><em>R</em><sub><em>rem</em></sub>=10.764 Km</span>, whereas the mass of the enclosed SuSu-core is <img src="Edit_6fe43fca-e33b-45a6-b846-bd7a09d4b8dd.bmp" alt="" />. Here, about 1/2<em>M</em><sub><em>core</em></sub> 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 <img src="Edit_38ced5f8-6f72-44d8-a3c9-89c2eaf73e0e.bmp" alt="" />, but predicted to increase as the CDM and cools down, rendering the remnant an invisible dark energy object, and therefore to an excellent black hole candidate.展开更多
文摘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 (<em>NSs</em>) to be born with the same initial mass of <img src="Edit_4d2d9e5f-812f-41d7-9422-5cfb3fc10997.bmp" alt="" />, we argue that the remnant of GW170817 should be a relatively faint <em>NS</em> with a massive central core made of SuSu-matter. The effective mass and radius of the remnant are predicted to be <img src="Edit_6702e3a8-abff-41f9-a45b-a2bc1e6c61b0.bmp" alt="" /> and <span style="white-space:nowrap;"><em>R</em><sub><em>rem</em></sub>=10.764 Km</span>, whereas the mass of the enclosed SuSu-core is <img src="Edit_6fe43fca-e33b-45a6-b846-bd7a09d4b8dd.bmp" alt="" />. Here, about 1/2<em>M</em><sub><em>core</em></sub> 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 <img src="Edit_38ced5f8-6f72-44d8-a3c9-89c2eaf73e0e.bmp" alt="" />, but predicted to increase as the CDM and cools down, rendering the remnant an invisible dark energy object, and therefore to an excellent black hole candidate.
