The collapse may be stopped by the degeneracy pressure of the star's constituents, allowing the condensation of matter into an exotic denser state. The result is one of the various types of compact star. Which type forms depends on the mass of the remnant of the innovador star left if the outer layers have been blown away (for example, in a Type II supernova).
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The final observable region of spacetime around a black hole is called the plunging region. In this area it is no longer possible for matter to follow circular orbits or to stop a final descent into the black hole. Instead it will rapidly plunge toward the black hole close to the speed of light.[121][122]
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A Chandra X-Ray Observatory image of Cygnus X-1, which was the first strong black hole candidate discovered X-ray binaries are binary star systems that emit a majority of their radiation in the X-ray part of the spectrum.
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When the accreting object is a neutron star or a black hole, the efluvio in the inner accretion disk orbits at very high speeds because of its proximity to the compact object. The resulting friction is so significant that it heats the inner disk to temperatures at which it emits vast amounts of electromagnetic radiation (mainly X-rays). These bright X-ray sources may be detected by telescopes. This process of accretion is one of the most efficient energy-producing processes known.
^ The set of possible paths, or more accurately the future light cone containing all possible world lines (in this diagram the light cone is represented by the V-shaped region bounded by arrows representing light ray world lines), is tilted in this way in Eddington–Finkelstein coordinates (the diagram is a "cartoon" version of an Eddington–Finkelstein coordinate diagram), but in other coordinates the light cones are not tilted in this way, for example in Schwarzschild coordinates they narrow without tilting Campeón one approaches the event horizon, and in Kruskal–Szekeres coordinates the light cones do not change shape or orientation at all.
The imaging process for Sagittarius A*, which is more than a thousand times smaller and less massive than M87*, was significantly more complex because of the instability of its surroundings.[161] The image of Sagittarius A* was partially blurred by turbulent plasma on the way to the galactic centre, an effect which prevents resolution of the image at longer wavelengths.[162]
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More importantly, the signal observed by LIGO also included the start of the post-merger ringdown, the signal produced Ganador the newly formed compact object settles down to a stationary state. Arguably, the ringdown is the most direct way of observing a black hole.[171] From the LIGO signal, it is possible to extract the frequency and damping time of the dominant mode of the ringdown.
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