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The origin and properties (masses and spins) of a double neutron star system like GW170817 are the result of a long sequence of complex binary star interactions. [41] The gravitational wave signal indicated that it was produced by the collision of two neutron stars [9] [18] [20] [42] with a total mass of 2.82 +0.47 −0.09 solar masses (M ☉). [2]
A neutron star merger is the stellar collision of neutron stars. When two neutron stars fall into mutual orbit, they gradually spiral inward due to the loss of energy emitted as gravitational radiation. [1] When they finally meet, their merger leads to the formation of either a more massive neutron star, or—if the mass of the remnant exceeds ...
Simulated collision of two neutron stars. A stellar collision is the coming together of two stars [1] caused by stellar dynamics within a star cluster, or by the orbital decay of a binary star due to stellar mass loss or gravitational radiation, or by other mechanisms not yet well understood.
A neutron star is the collapsed core of a massive supergiant star. It results from the supernova explosion of a massive star—combined with gravitational collapse—that compresses the core past white dwarf star density to that of atomic nuclei.
A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf. [1] Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below ...
PSR J1946+2052 is a short-period binary pulsar system located 11,000–14,000 light-years (3,500–4,200 pc) away from Earth in the constellation Vulpecula.The system consists of a pulsar and a neutron star orbiting around their common center of mass every 1.88 hours, which is the shortest orbital period among all known double neutron star systems as of 2022.
This artist's impression shows a kilonova produced by two colliding neutron stars. On October 16, 2017, the LIGO and Virgo collaborations announced the first detection of a gravitational wave (GW170817 [9]) which would correspond with electromagnetic observations, and demonstrated that the source was a binary neutron star merger. [10]
An intermediate-mass binary pulsar (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10–200 ms consisting of a white dwarf with a relatively high mass of approximately . [7] The spin periods, magnetic field strengths, and orbital eccentricities of IMBPs are significantly larger than those of low mass binary pulsars (LMBPs). [7]