accretion disk


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Related to accretion disk: black hole, event horizon

accretion disk

See black hole; mass transfer; quasar.

accretion disk

[ə′krē·shən ‚disk]
(astronomy)
A viscous structure consisting of gas lost by a red giant or supergiant flowing around a companion main-sequence star or compact object (white dwarf, neutron star, or black hole).
References in periodicals archive ?
And the innermost stable circular orbit around the black hole, the brightly glowing edge of the accretion disk, will be about three times wider.
SS 433-The parameters of the eclipsing system with a processing thick accretion disk.
It has also been shown [7] that particle interactions in the black-hole accretion disks cause an excess production of positrons as compared to electrons, however, this disparity alone, without emission directionality considerations, does not constitute a non-conservation of parity.
It showed portions of the accretion disk swinging up over the top and down under Gargantua's shadow, and also in front of the shadow's equator, producing an image of a split shadow that has become iconic for the movie.
After carefully examining several possibilities, the team concluded that huge amounts of gas are rapidly falling onto "little monster" black holes in each of these ULXs, which produces a dense disk wind flowing away from the supercritical accretion disk.
The astronomers were able to confirm the hypothesis surrounding a black hole's corona, similar to that of our Sun's corona, above the accretion disk as a result of the intensifying magnetic fields.
The accretion disk is searingly hot and quite massive, and can linger around a young star for 10,000,000 years or so.
Since there is a direct relationship between the jets and a star's accretion disk, there is a great deal to be learned about stellar formation by simply studying the jets.
Schnittman developed a process for modeling the inner region of a black hole's accretion disk, tracking the emission and movement of X-rays, and comparing the results to observations of real black holes.
Sixty-nine papers from the October 2011 conference present research on the physical characteristics of active galactic nuclei (AGN) accretion disk winds.
This is caused by the passage across the front of the accretion disk of the bright spot where gas streaming from the secondary star impacts the edge of the disk.
Gas falling toward a black hole spirals inward and piles up into an accretion disk, where it becomes compressed and heated.