It is thought that stars of this size undergo a series of these pulses until they shed sufficient mass to drop below 100 solar masses, at which point they are no longer hot enough to support pair-creation. This increases the energy of the gamma rays that are produced making them more likely to interact and so increases the rate at which energy is absorbed in further pair production. They can form pairs of particles, such as electron-positron pairs, and electron-positron pairs can also meet and annihilate each other to create gamma rays again, in accordance with At the very high density of a large stellar core, pair production and annihilation occur rapidly.
The content is provided for information purposes only. Instead, the contraction caused by pair-creation provokes increased thermonuclear activity within the star that repulses the inward pressure and returns the star to equilibrium. This process is called pulsational pair-instability (PPI). The results mean that the 50 solar mass black hole … The exciting detection of gravitational waves with LIGO (laser interferometer gravitational-wave observatory) and VIRGO (Virgo interferometric gravitational-wave antenna) have shown the presence of merging The masses of the observed black holes before merging have been measured and turned out to have a much larger than previously expected To answer this question, a research team at the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU) consisting of Project Researcher Shing-Chi Leung (currently at the California Institute of Technology), Senior Scientist Ken'ichi Nomoto, and Visiting Senior Scientist Sergei Blinnikov (professor at the Institute for Theoretical and Experimental Physics in Mosow) have investigated the final stage of the evolution of very In close binary systems, initially 80 to 130 solar mass stars lose their hydrogen-rich envelope and become helium stars of 40 to 65 solar masses. by Kavli Institute for the Physics and Mathematics of the Universe Through simulations of a dying star, a team of theoretical physics researchers have found the evolutionary origin and the maximum mass of black holes which are discovered by the detection of gravitational waves. Comprehensive models of the late-stage evolution of very massive stars predict that a In very large hot stars with a temperature above about Sufficiently energetic gamma rays can interact with nuclei, electrons, or one another. A part of the stellar outer layer is ejected, while the inner part cools down and collapses again. Apart from any fair dealing for the purpose of private study or research, no
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pair instability gap black hole