gerde-ye pirâ-siyah câl
Fr.: disque autour de trou noir
dual supermassive black hole
siyah-câl-e abar-porjerm-e dogâné
Fr.: trou noir supermassif double
The outcome of a → merger process between two galaxies, each with its own central → supermassive black hole (SMBH), resulting in a remnant galaxy hosting two SMBHs. Simulations of → galaxy mergers show there should be lots of dual → active galactic nuclei (AGN) visible at less than 10 kpc separations. As of 2015 more than 100 known dual supermassive black holes have been found. See also → binary supermassive black hole.
intermediate-mass black hole (IMBH)
siyah câl-e miyân jerm
Fr.: trou noir de masse intermédiaire
A → black hole with a mass in the range 102-104 solar masses. IMBHs may form as the result of multiple → mergers of smaller objects in the centers of dense stellar clusters in the present universe, assuming → mass loss from → stellar winds is not significant. They may also arise from the evolution of → very massive stars early in the history of the Universe, forming black hole "seeds" in the centers of massive halos (the precursors of the galaxies we see today) early in the history of the Universe, to redshifts z > 10. Currently the best observational evidence for IMBHs comes from models of ultraluminous X-ray sources (See, e.g., J. M. Centrella et al. 2010, astro-ph/1010.5260).
Kerr black hole
siyah câl-e Kerr (#)
Fr.: trou noir de Kerr
Named after the New Zealand mathematician Roy P. Kerr (1934-) who, in 1963, was the first to solve the → field equationss of Einstein's theory of → general relativity for a situation of this kind; → black hole.
Kerr-Newman black hole
siyah câl-e Kerr-Newman
Fr.: trou noir de Kerr-Newman
massive black hole
Fr.: trou noir massif
A black hole with a mass between millions and billions of solar masses residing in galactic nuclei. The mass of this type of black holes represents about 0.2% of the bulge mass. When matter is swallowed by the black hole, this gives rise to the tremendous energetic phenomena observed in quasars and active galactic nuclei.
mini black hole
Fr.: mini corps noir
A black hole of mass as low as 10-6 gram supposed to have formed in the early Universe following the Big Bang event. Same as primordial black hole.
Planck's blackbody formula
disul-e siyah jesm-e Planck
Fr.: formule du corps noir de Planck
A formula that determines the distribution of intensity of radiation that prevails under conditions of thermal equilibrium at a temperature T: Bv = (2hν3 / c2)[exp(hν / kT) - 1]-1 where h is Planck's constant and ν is the frequency.
primordial black hole
Fr.: trou noir primordial
A black hole formed following the Big Bang event due to incredibly violent turbulence that squeezed concentrations of matter to high densities. These black holes, first suggested by Stephen Hawking, are expected to have a mass comparable to that of a mountain and a size as small as an atom. Same as → mini black hole.
Reissner-Nordstrom black hole
siyah câl-e Reissner-Nordström
Fr.: tou noir de Reissner-Nordström
Named after the German physicist Hans Jacob Reissner (1874-1967) in 1916 and the Finnish Gunnar Nordstrom (1881-1923) in 1918 independently worked out solutions different from those of Schwarzschild; → black hole.
rotating black hole
Fr.: trou noir en rotation
A black hole that possesses angular momentum, as first postulated by Roy C. Kerr in 1963. Opposite of a stationary black hole. → ergosphere.
Schwarzschild black hole
Fr.: trou noir de Schwarzschild
Karl Schwarzschild (1873-1916), German mathematical physicist, who carried out the first relativistic study of black holes. → black hole.
second law of black-hole mechanics
qânun-e dovom-e mekânik-e siyah-câl
Fr.: deuxième loi de la mécanique des trous noirs
The surface area of a black hole's horizon can never decrease.
stationary black hole
Fr.: trou noir stationnaire
stellar black hole
siyah câl-e setâre-yi
Fr.: trou noir stellaire
A → black hole with a mass in the range 3-30 → solar masses representing the end-product of → massive star evolution. Since → neutron stars cannot have masses larger than 3 solar masses, compact objects more massive than this must be black holes. There is good observational evidence for the existence of stellar black holes, based in particular on dynamical measurements of the masses of compact objects in → transient X-ray sources. Same as → stellar-mass black hole.
stellar-mass black hole
siyah câl bâ jerm-e setâre-y
Fr.: trou noir de masse stellaire
Same as → stellar black hole.
supermassive black hole (SMBH)
Fr.: trou noir supermassif
A → black hole of tremendous mass, equivalent to those of millions or even billions of stars, which is believed to exist and occupy the centers of many galaxies. The supermassive black hole residing in the center of our → Milky Way Galaxy is the object → Sgr A* with a mass of 4 x 106→ solar masses within a radius of 100 → astronomical units.