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As the material in this disk cooled, chunks of rock grew and accreted to form the planets.
Most of the material in this disk is swallowed by the black hole, but some of it is swept outwards in jets (colored blue) by quickly spinning magnetic fields close to the black hole.
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Spinning material in the disk falls onto the neutron star, increasing its rotation rate.
Other material in the disk may coalesce to form other stars and/or planets.
Meanwhile, the material in the disk collides, coalesces, and gradually forms larger and larger objects, as in Kant's theory.
When a planet lies embedded within a circumstellar disk, it exchanges angular momentum with material in the disk.
Because the disk material needs to lose energy to accrete onto the central object, the material in the disk gets hot, and the heat generated escapes through both sides of the disk.
Planets, on the other hand, form when material in the disk around a pre-existing star begins to condense around rock/ice cores.
As the material in the disk comes closer to the accretor, it speeds up in response to the stronger gravitational pull and moves along a spiral path at supersonic orbital speeds while still drifting gradually inward at subsonic speeds.
The orientation of the magnetic material in the disk media has changed from in the plane of the disk to out of the plane of the disk in order to achieve higher magnetic recording densities.
The SS Cygni light curve above was observed in the optical part of the spectrum and displays the dynamics among the accretion disk - the material in the disk that was accreted from its companion star - and the surface of the white dwarf.
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Justyna Jupowicz-Kozak
CEO of Professional Science Editing for Scientists @ prosciediting.com