Extended Data Fig. 4: Effect of the semimajor axis distribution of rogue planetesimals.
From: An upper limit on late accretion and water delivery in the TRAPPIST-1 exoplanet system
The top left panel shows our the subset of our fiducial batch of simulations with 1000 rogue planetesimals with a total mass in rogue planetesimals between 0.01 and 1 Earth mass. The top right and bottom left panels show the sets of simulations with arogue = 0.2 − 0.3 au and arogue = 0.7 − 1 au, and the same periastron distribution as in the fiducial set (with orbits initially crossing those of only the outer planets). The bottom right panel shows a set of simulations in which the rogue planetesimals were on extremely eccentric orbits, with semimajor axes arogue = 0.7 − 1 au and periastron distance qrogue randomly chosen to sample a logarithmic distribution in the range 0.005 − 0.06 au. As in Fig. 1 in the main text, blue filled circles indicate systems that remained in resonant chains, red diamonds those that remained stable for 10 Myr but lost their resonant structure, and black empty circles those that underwent dynamical instabilities.
