Authors:Backus et alAbstract:We investigate the conditions required for planet formation via gravitational instability (GI) and protoplanetary disk (PPD) fragmentation around M-dwarfs. Using a suite of 64 SPH simulations with 106 particles, the parameter space of disk mass, temperature, and radius is explored, bracketing reasonable values based on theory and observation. Our model consists of an equilibrium, gaseous, and locally isothermal disk orbiting a central star of mass M∗=Msol/3. Disks with a minimum Toomre Q of Qmin≲0.9 will fragment and form gravitationally bound clumps. Some previous literature has found Qmin
Sunday, November 13, 2016
Fragmentation of protoplanetary disks around M-dwarfs
Posted by Will Baird at 4:00 PM
Labels: circumstellar disks, M dwarf, protoplanetary disks
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