Stronger radiation environments produce more massive, hotter protostellar discs whose fragments are large and disruptive rather than planetary-mass.
The Astrophysical Journal847(1), 43 (2017)
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The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.