Earth-Mass Planets in Tandem Disks
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arXiv
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| author | Nimura, Tokuhiro Ebisuzaki, Toshikazu |
| author_facet | Nimura, Tokuhiro Ebisuzaki, Toshikazu |
| contents | This paper presents a new terrestrial planet formation theory demonstrating that Earth-mass planets form naturally in tandem protosolar disks. Our model builds upon tandem planet formation theory (Ebisuzaki and Imaeda 2017; Imaeda and Ebisuzaki 2017a,b, 2018), incorporating magneto-rotational instability (MRI) suppression (Balbus and Hawley 1991; Hawley and Balbus 1991), porous particle aggregation (Okuzumi et al. 2012; Kataoka et al. 2013), and standard planet formation mechanisms (e.g., Safronov 1969; Hayashi et al. 1985). In a tandem proto-solar disk, planets form at two distinct locations: the inner and outer edges of the MRI-suppressed region, where solid particles accumulate. The inner edge produces rocky planets, while the outer edge forms gas giants. When planetesimals reach Earth-sized mass at the inner MRI edge, they migrate outward due to gas disk torque. For a protosolar disk accretion rate of M_dot = 10^-7.08 solar masses per year (Case D), the total solid mass at the inner MRI edge reaches 1.99 Earth masses, producing two Earth-mass planets. This result closely matches the solar system's terrestrial planet distribution (Earth and Venus), which comprises 92% of total terrestrial planet mass, providing strong support for our formation mechanism. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_13269 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Earth-Mass Planets in Tandem Disks Nimura, Tokuhiro Ebisuzaki, Toshikazu Earth and Planetary Astrophysics This paper presents a new terrestrial planet formation theory demonstrating that Earth-mass planets form naturally in tandem protosolar disks. Our model builds upon tandem planet formation theory (Ebisuzaki and Imaeda 2017; Imaeda and Ebisuzaki 2017a,b, 2018), incorporating magneto-rotational instability (MRI) suppression (Balbus and Hawley 1991; Hawley and Balbus 1991), porous particle aggregation (Okuzumi et al. 2012; Kataoka et al. 2013), and standard planet formation mechanisms (e.g., Safronov 1969; Hayashi et al. 1985). In a tandem proto-solar disk, planets form at two distinct locations: the inner and outer edges of the MRI-suppressed region, where solid particles accumulate. The inner edge produces rocky planets, while the outer edge forms gas giants. When planetesimals reach Earth-sized mass at the inner MRI edge, they migrate outward due to gas disk torque. For a protosolar disk accretion rate of M_dot = 10^-7.08 solar masses per year (Case D), the total solid mass at the inner MRI edge reaches 1.99 Earth masses, producing two Earth-mass planets. This result closely matches the solar system's terrestrial planet distribution (Earth and Venus), which comprises 92% of total terrestrial planet mass, providing strong support for our formation mechanism. |
| title | Earth-Mass Planets in Tandem Disks |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2508.13269 |