Astronomy Technical Terms for Black Holes.

Technical Terms for Black Holes.


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Black Hole is a region of space-time having so much gravitation effects that nothing – not even particles and electromagnetic radiation such as light can escape from inside it.

The concept of Black Hole was predicted by Albert Einstein in 1916 with his General Theory of Relativity. The theory predicts that a sufficiently compact mass can deform spacetime to form a black hole. The term black hole was firstly used by American Astronomer John Wheeler in 1967 and the discovery of first Black Hole was in 1971.

According to scientists, we can observe three kinds of the Black Holes. Stellar Black Holes, Intermediate Black Holes, and Supermassive Black Holes. The description about all these Black Holes has been discussed in this article. But in this article, we’ll discuss the basic terms used to know Black Holes.


It is a natural phenomenon by which all things with mass are brought toward one another, including objects ranging atoms and photons to planets and stars.


In physics, Space-time is any mathematical model that fuses the three dimensions of space and the one dimension of time into a single four-dimensional continuum.


An active galactic nucleus of very high luminosity. A quasar consists of the supermassive black hole surrounded by an orbiting accretion disk of gas.


Mass is both a property of a physical body and measure of its resistance to acceleration. (A change in its state of motion) when a net force is applied.


In astronomy, luminosity is the total amount of energy emitted by a star, galaxy or other astronomical objects per unit time. It is related to the brightness, which is the luminosity of an object in a given spectral region.

Event Horizon

In General Relativity, an Event Horizon is a boundary in spacetime beyond which events cannot affect an outside observer. In Layman’s terms, it is defined as the shell of “points of no return”, i.e. the points at which gravitational pull becomes so great as to make escape impossible, even for light.

Hawking Radiation

Hawking radiation, also known as Hawking–Zel’dovich radiation, is blackbody radiation that is predicted to be released by black holes, due to quantum effects near the event horizon. It is named after the physicist Stephen Hawking, who provided a theoretical argument for its existence in 1974, and sometimes also after Jacob Bekenstein, who predicted that black holes should have a finite entropy.

Neutron Star

A neutron star is the collapsed core of a large star which before collapse had a total of between 10 to 29 solar masses. Neutron stars are the smallest and densest stars known to exist.

Supermassive Black Hole

A Supermassive Black Hole (SMBH or SBH) is the largest type of black hole on the order of hundreds of thousands to billions of solar masses.

Solar Mass

The solar mass is a standard unit of mass in astronomy, equal to approximately 2* 10^3 kg. It is used to indicate the masses of other masses of other stars as well as clusters, nebulae, and galaxies. It is equal to the mass of the Sun about two nonillions (two quintillions in the long scale) Kilograms.

Electromagnetic Radiation

In physics, electromagnetic radiation (EM radiation or EMR) refers to the waves (or their quanta, photons) of the electromagnetic field, propagating (radiating) through space-time, carrying electromagnetic radiant energy.




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