Although the name has persisted, now we know that they are in fact the end states of low mass stars, and would only involve planets if a binary companion in one
of the accretion scenarios above were in fact a large planet.
Not exact matches
The standard
scenario for the birth
of gas giants posits a continuation
of the rocks - crashing - together process, also known as core
accretion.
Weiss says that if the solar nebula was around in the first 4 million years
of solar system formation, this would give support to the core
accretion scenario, which is generally favored among scientists.
There are, however, a range
of different
scenarios for the production
of these
accretion disks.
There are two different black hole
scenarios proposed to explain these objects: (1) they contain very «big» black holes that could be more than a thousand times more massive than the Sun (Note 1), or (2) they are relatively small black holes, «little monsters» with masses no more than a hundred times that
of the Sun, that shine at luminosities exceeding theoretical limits for standard
accretion (called «supercritical (or super-Eddington)
accretion,» Note 2).
They discuss a unified
scenario for understanding brightness variations from
accretion discs around different types
of stars and compact objects.
We discuss the existence
of the long cycle and these flare properties in the backdrop
of two rival
scenarios to produce hard X-rays, a magnetic star - disk interaction and the
accretion of blobs onto a secondary white dwarf.
Under the most accepted
scenario, planets form over tens
of millions
of years from the slow
accretion of dust, rocks, and gas.