Its All about Pj Problem Strings - 7 Spaces Of Interest and their associated Basic Sequences; 7 Pj Problems of Interest (PPI) and their Alleles (A)
A celestial star is a small, large or super large celestial body in which hydrogen is being fused (nuclear reaction) into helium. It shines because of the energy it releases during fusion.
Uneven distribution of nebulae (clouds of hydrogen (H) and Helium (He) gases) are the matter resident in space prior to the formation of a star. Gravity clumps and collapses nebulae into a very hot and dense core of spherical H and He atoms. This dense core is called a protostar. As gravity continues to collapse a protostar, its core eventually attains an exceedingly high temperature (in the millions of degree Kelvin). First a plasma phase is established in the core and electrons separate from their nuclei. At a higher temperature called a flash point, the strong force overcomes the electromagnetic repulsion of nuclei. Fusion begins when smaller nuclei bond together to form larger nuclei with the release of tremendous amount of energy. This energy provides an outward thermal pressure that balances the inner pull of gravity that is collapsing the protostar. Consequently, the protostar's size is stabilized and a star is born. This fusion can sequentially form helium (He), carbon (C), neon (Ne), oxygen (O), silicon (Si) and nickel (Ni). The formation of iron (Fe) in a star's core, marks the limit of a star's capacity to form elements during its lifetime. Higher mass elements are formed during the event known as a SUPERNOVA.
A star dies when there is no outward energy from fusion to balance the inward pull of gravity. For example, a star with an iron (Fe) core is eventually subjected to intense pressure and high temperature that results in an endothermic reaction that breaks Fe nuclei into alpha particles, protons and neutrons. The absence of outward thermal pressure causes gravity to rapidly and forcefully collapse the outer layers of the star. The inner core is further compressed. Eventually, the outer layers violently rebound and are thrown outward as Planetary Nebulae in a Supernova. High concentration of neutrons are ejected from the core and are captured rapidly (r-process) or slowly(s-process) by surrounding nuclei. Each captured neutron decays to a proton by emitting an electron and an anti-neutrino. A higher mass element is formed when this proton increases the proton count of the nucleus.
The energy that dispersed the hydrogen and helium atoms into space; the space into which the atoms are dispersed; the atoms themselves; the nebulae formed by the atoms; the gravity that collapses the nebulae into protostars; the high temperature in the protastar; the fusion that results from the high temperature; the resultant thermal pressure that balances gravity; the deaths of stars; the Supernovas and the higher elements they dispersed; are all expressions of Pj Problems. Consequently, celestial stars are expressions of Pj Problems
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