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A strange star, also called a strange quark star, [1]: 352 is a hypothetical compact astronomical object, a quark star made of strange quark matter. [2] [3] [4] Strange stars might exist without regard to the Bodmer–Witten assumption of stability at near-zero temperatures and pressures, as strange quark matter might form and remain stable at ...
A star is a massive luminous spheroid astronomical object made of plasma that is held together by its own gravity.Stars exhibit great diversity in their properties (such as mass, volume, velocity, stage in stellar evolution, and distance from Earth) and some of the outliers are so disproportionate in comparison with the general population that they are considered extreme.
A black hole (artist concept); Vela Pulsar, a rotating neutron star; M80, a globular cluster, and the Pleiades, an open star cluster; The Whirlpool galaxy and Abell 2744, a galaxy cluster; Superclusters, galactic filaments and voids
No, actually -- even NASA is calling this star the "loneliest" in the universe. "The unusual object, called CX330, was first detected as a source of X-ray light in 2009," according to a NASA news ...
Stars made of strange quark matter are known as strange stars. These form a distinct subtype of quark stars. [11] Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, they could also be created in the early cosmic phase separations following the Big Bang. [9]
Quark stars that contain strange matter are called strange stars. Based on observations released by the Chandra X-Ray Observatory on 10 April 2002, two objects, named RX J1856.5−3754 and 3C 58 , were suggested as quark star candidates.
The following is a list of particularly notable actual or hypothetical stars that have their own articles in Wikipedia, but are not included in the lists above. BPM 37093 — a diamond star Cygnus X-1 — X-ray source
Stars of greater mass have a higher rate of core energy generation, and heavier stars' luminosities increase far out of proportion to the increase in their masses. The Eddington limit is the point beyond which a star ought to push itself apart, or at least shed enough mass to reduce its internal energy generation to a lower, maintainable rate.