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The origin of high eccentricity planets: The dispersed planet formation regime for weakly magnetized disks
In the tandem planet formation regime, planets form at two distinct sites where solid particles are densely accumulated due to the on/off state of the magnetorotational instability (MRI). We found that tandem planet formation can reproduce the solid component distribution of the Solar System and tends to produce a smaller number of large planets through continuous pebble flow into the planet formation sites. In the present paper, we investigate the dependence of tandem planet formation on thedoi:10.1016/j.gsf.2016.07.001 fatcat:qyaaqdt5bjdpdk6dl3d6xumyri