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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 ...
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 ...
[3] [12] Besides depictions of the aftermath, Baxter's 2000 novel Manifold: Space (a.k.a. Space: Manifold 2) depicts the construction of immense radiation shields to serve as protection, and the 2005–2006 television series Threshold portrays the lead-up to the anticipated destruction of the Earth by the shockwave from a neutron star merger ...
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.
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.
The first radio pulsar was discovered in 1967 by Jocelyn Bell and her adviser, Antony Hewish using the Interplanetary Scintillation Array. [4] Franco Pacini and Thomas Gold quickly put forth the idea that pulsars are highly magnetized rotating neutron stars, which form as a result of a supernova at the end of the life of stars more massive than about 10 times the mass of the Sun (M ☉).
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]
However, the remnant star of Pa 30 is a white dwarf, not one of the conventional supernova remnants (neutron stars or black holes). It has been suggested that Pa 30 is the remnant of a rare class of supernovae known as " sub-luminous Type Iax Supernova " and that a merger of a CO white dwarf and an ONe white dwarf produced the remnant shell ...