Journey into the Enigmatic Universe of Black Holes

Black holes are regions of spacetime where gravity is so strong that nothing can escape its event horizon, including light. The boundary of no escape is called the event horizon. Black holes act like an ideal black body and reflect no light. Quantum field theory in curved spacetime predicts that event horizons emit Hawking radiation. Black holes of stellar mass form when massive stars collapse at the end of their life cycle. Supermassive black holes of millions of solar masses may form by absorbing other stars and merging with other black holes. The presence of a black hole can be inferred through its interaction with other matter and with electromagnetic radiation such as visible light. The idea of a body so big that even light could not escape was briefly proposed by John Michell in a letter published in November 1784. The term "black hole" was reportedly coined by physicist Robert H. Dicke in the early 1960s. The no-hair theorem postulates that, once it achieves a stable condition after formation, a black hole has only three independent physical properties: mass, electric charge, and angular momentum. When an object falls into a black hole, any information about the shape of the object or distribution of charge on it is evenly distributed along the horizon of the black hole, and is lost to outside observers. The simplest static black holes have mass but neither electric charge nor angular momentum.Black Holes: A Comprehensive Summary

Black holes have a gravitational field that is identical to any other spherical object of the same mass. This means the popular notion of a black hole "sucking in everything" in its surroundings is correct only near a black hole's horizon.
Black holes can be described by different solutions, such as non-rotating charged black holes and non-charged rotating black holes.
The total electric charge and the total angular momentum of a black hole are constrained by the mass. Black holes with the minimum possible mass satisfying this inequality are called extremal.
The defining feature of a black hole is the appearance of an event horizon, a boundary in spacetime through which matter and light can pass only inward towards the mass of the black hole. Nothing, not even light, can escape from inside the event horizon.
At the center of a black hole, there may lie a gravitational singularity, a region where the spacetime curvature becomes infinite. In both rotating and non-rotating black holes, the singular region has zero volume and infinite density.
The photon sphere is a spherical boundary in which photons that move on tangents to that sphere would be trapped in a circular orbit about the black hole.
Rotating black holes are surrounded by a region of spacetime in which it is impossible to stand still, called the ergosphere.
In general relativity, there exists an innermost stable circular orbit (ISCO), for which any infinitesimal inward perturbations to a circular orbit will lead to spiraling into the black hole.
Black holes are formed by gravitational collapse of heavy objects such as stars. Star formation in the early universe may have resulted in very massive stars, which upon their collapse would have produced black holes of up to 10 M☉.
Primordial black holes could have formed from density fluctuations in the early universe, and could be the seeds of the supermassive black holes found in the centers of most galaxies.
The gravitational collapse process takes a finite amount of time from the reference frame of infalling matter, but a distant observer would never see the formation of the event horizon.
The appearance of singularities in general relativity is commonly perceived as signaling the breakdown of the theory, but it is expected to occur in a situation where quantum effects should describe these actions.
There is no known mechanism (except possibly quark degeneracy pressure) powerful enough to stop the implosion of an object with a mass exceeding about 3-4 M☉, and the object will inevitably collapse to form a black hole.Black Holes: Formation, Growth, Evaporation, Observational Evidence, and Detection of Gravitational Waves
Primordial black holes could have formed in the early universe due to initial density perturbations, with models predicting their size ranging from a Planck mass to hundreds of thousands of solar masses.
Black holes can also be formed in high-energy collisions, but as of 2002, no such events have been detected, suggesting a lower limit for their mass.
Once formed, black holes can grow by absorbing additional matter, including gas and interstellar dust, and by merging with stars or other black holes.
Hawking radiation predicts that black holes emit small amounts of thermal radiation and will shrink and evaporate over time as they lose mass, but this is expected to be very weak for astrophysical black holes.
The Event Horizon Telescope has directly observed the immediate environment of black holes' event horizons, including the black hole at the center of the Milky Way and the black hole at the center of Messier 87.
The LIGO gravitational wave observatory made the first-ever successful direct observation of gravitational waves in 2015, providing the most concrete evidence for the existence of black holes to date.
Proper motions of stars orbiting Sagittarius A* provide strong observational evidence that these stars are orbiting a supermassive black hole at the center of the Milky Way.
The formation of supermassive black holes is still an open field of research, and their growth and evolution remain a topic of study.
Black holes challenge our understanding of the laws of physics, including general relativity and quantum mechanics, and their study may lead to new discoveries in theoretical physics.
The detection and study of black holes have important implications for astronomy, astrophysics, and cosmology, including the study of galaxy formation and evolution.
While black holes are often associated with destruction and danger, they also play a vital role in the universe as sources of energy and as natural laboratories for testing the laws of physics.
Further research and observation of black holes are necessary to deepen our understanding of these enigmatic objects and their role in the universe.Black Holes: Accretion of Matter, X-ray Binaries, Galactic Nuclei, Alternatives, Entropy and Thermodynamics, Information Loss Paradox, Microlensing, Quasi-Periodic Oscillations, Active Galactic Nuclei, M-Sigma Relation, Observation of Quasar Accretion Disk, Cygnus X-1, Soft X-ray Transients, V404 Cygni, Gravitational Lensing, Sagittarius A*, Upper Limit for Neutron Star Mass, Exotic Phases of Matter, Fuzzball Model, Gravastar, Black Star, Dark-energy Star, Holographic Principle, Statistical Mechanics, Quantum Gravity, Wald Formula, Hawking Radiation, Black Hole Complementarity, Firewall Paradox, Monogamy of Entanglement.