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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 ...
The first identification of r-process elements in a neutron star merger was obtained during a re-analysis of GW170817 spectra. [77] The spectra provided direct proof of strontium production during a neutron star merger. This also provided the most direct proof that neutron stars are made of neutron-rich matter.
White dwarfs are the remnants of low-mass stars which, if they form a binary system with another star, can cause large stellar explosions known as type Ia supernovae. The normal route by which this happens involves a white dwarf drawing material off a main sequence or red giant star to form an accretion disc.
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 ...
Zooming to RX J1856.5−3754 which is one of the Magnificent Seven and, at a distance of about 400 light-years, the closest-known neutron star. Neutron stars are the collapsed cores of supergiant stars. [1] They are created as a result of supernovas and gravitational collapse, [2] and are the second-smallest and densest class of stellar objects ...
The star is possibly highly unstable, too massive to remain as a white dwarf, and it is predicted to collapse into a neutron star within ten thousand years. [ 8 ] Both the central star and the nebula contain large amounts of neon , magnesium , silicon , and sulfur (but no hydrogen, helium, or nitrogen), with such requiring an origin in a recent ...
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]