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Abstract <p>The aim of this study is to investigate the interaction of Earth-mass planets with a disk of planetesimals. It is shown that an Earth-like planet, initially located near the inner boundary of the planetesimal disk, migrates inside the disk. The magnitude of penetration of the planet into the disk is a random value determined by the angular momentum distribution of planetesimals approaching the planet. However, at a certain stage, the direction of the planet’s migration always changes, and the planet returns to the inner boundary of the disk. During such reversible migration, the planet perturbs the orbits of planetesimals and increases their relative velocities in the region of the disk where it was during its migration. The relative velocities of planetesimals increase to values sufficient for their fragmentation during collisions. Our estimates show that after the passage of an Earth-mass planet through the outer planetesimal disk (30–40 AU in our model), the average relative velocities in the main part of the disk increase to values sufficient for the fragmentation of monolithic basaltic planetesimals ~40 km in size. Thus, the interaction of even a small planet (of the order of Earth’s mass) with a planetesimal disk can lead to the formation of dust particles observed in outer debris disks.</p>

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Study of the Migration of Earth-Like Planets in Planetesimal Disks and the Formation of Debris Disks

  • 期刊论文

  • 发表日期：

    2025年9月1日

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  • O. S. Oleynik,
  • V. V. Emel’yanenko

摘要

Abstract

The aim of this study is to investigate the interaction of Earth-mass planets with a disk of planetesimals. It is shown that an Earth-like planet, initially located near the inner boundary of the planetesimal disk, migrates inside the disk. The magnitude of penetration of the planet into the disk is a random value determined by the angular momentum distribution of planetesimals approaching the planet. However, at a certain stage, the direction of the planet’s migration always changes, and the planet returns to the inner boundary of the disk. During such reversible migration, the planet perturbs the orbits of planetesimals and increases their relative velocities in the region of the disk where it was during its migration. The relative velocities of planetesimals increase to values sufficient for their fragmentation during collisions. Our estimates show that after the passage of an Earth-mass planet through the outer planetesimal disk (30–40 AU in our model), the average relative velocities in the main part of the disk increase to values sufficient for the fragmentation of monolithic basaltic planetesimals ~40 km in size. Thus, the interaction of even a small planet (of the order of Earth’s mass) with a planetesimal disk can lead to the formation of dust particles observed in outer debris disks.