accretion disk

(redirected from Accretion disc)
Also found in: Dictionary, Wikipedia.
Related to Accretion disc: accretion disk

accretion disk

See black hole; mass transfer; quasar.
Collins Dictionary of Astronomy © Market House Books Ltd, 2006

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).
McGraw-Hill Dictionary of Scientific & Technical Terms, 6E, Copyright © 2003 by The McGraw-Hill Companies, Inc.
References in periodicals archive ?
While some matter in the accretion disc -- the belt of gas orbiting Sagittarius A* at relativistic speeds [2] -- can orbit the black hole safely, anything that gets too close is doomed to be pulled beyond the event horizon.
A spinning black hole like that in Interstellar would create a radiant and glowing accretion disc, simply due to the heat and speed of movement.
They are thought to arise from the interaction of the secondary star orbit with a slowly precessing eccentric accretion disc. The eccentricity of the disc arises because a 3:1 resonance occurs between the secondary star orbit and the motion of matter in the outer accretion disc.
"By being able to measure the distance between the black hole and the accretion disc, we believe we can more effectively measure the spin of black holes."
The observation agrees closely with recent theoretical work, also at Leicester and using the UK's Dirac supercomputer facility simulating the 'tearing' of misaligned accretion discs. This work has shown that rings of gas can break off and collide with each other, cancelling out their rotation and leaving gas to fall directly towards the black hole.
"These accretion discs are extremely stable from a hydrodynamic perspective as according to Kepler's laws of planetary motion angular momentum increases from the center towards the periphery," Helmholtz-Zentrum Dresden-Rossendorf physicist Dr.
The eclipse depth in eclipsing SU UMa systems is often strongly affected by the location of the superhump: eclipses are shallower when hump maximum coincides with eclipse, such as is found, for example, in the case of DV UMa, (10) IY UMa (11) and SDSS J122740.83+513925.9.12 In such systems, since the accretion disc is elliptical and precesses, the eclipse depth varies with the precession period (which is the beat period between [P.sub.sh] and [P.sub.orb]).
One theory suggests that they develop within the 'accretion disc' - the matter sucked into the orbit of a growing black hole.
Several regularly-spaced dips in the emission were seen in an uninterrupted 14.5 hour observation with XMM-Newton, caused by the uneven rim of the black hole's accretion disc briefly obscuring the X-rays as the system rotates, its disc almost edge-on along XMM-Newton's line of sight.
In the absence of a significant white dwarf magnetic field, material from the secondary passes through an accretion disc before settling on the surface of the white dwarf.