accretion disk


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Related to accretion disk: black hole, event horizon

accretion disk

n.
A disk of interstellar material gathered into orbit by the gravitational field of a celestial object, such as a star or black hole, and gradually spiraling into the object.
Translations
disque d’accrétion
References in periodicals archive ?
When a disk of material called an accretion disk rotates around a black hole on a tilted axis, it wobbles around in a movement that also affects those jets, according to the simulation.
will form what is called an accretion disk orbiting just around the black hole.
Yet the 2 million-year-old object is growing from an accretion disk, as stars do.
By looking at these quasars in both optical and infrared wavelengths, the team could probe both the quasar's accretion disk and its torus " the doughnut-shaped ring of dust clouds that wraps around it.
As matter from the star falls onto the black hole, an accretion disk forms around the black hole.
But now and then the stream surges, pushing its way closer to the pulsar and establishing an accretion disk.
The remaining mass flattened out into a pancake-like protoplanetary accretion disk from which the eight major planets and their numerous moons, comets, asteroids, and other small solar system bodies emerged.
And the innermost stable circular orbit around the black hole, the brightly glowing edge of the accretion disk, will be about three times wider.
In case of a neutron star or a white dwarf the emission originates from both the accretion disk and the surface of the compact star while in black hole binaries the only source of X-rays is the accretion disk.
Although the birthing of planets and dying of paired stars are similar in that they both occur within an accretion disk, a pancake of diffuse matter, they are also notably different.
The S results from a bipolar jet of hot material flying from the poles of an accretion disk around the white dwarf.
Specific topics include accretion disk winds by magneto-rotational turbulence, the origin of magnetic fields in the intracluster medium, the long-term sustainability of Rossby wave instability in proto-planetary disks with dead zones, computational physics of small meteors, the marriage of gas and dust, and well-balanced schemes for gravitationally stratified media.