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| Auteurs principaux: | , |
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| Format: | Preprint |
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2025
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| Accès en ligne: | https://arxiv.org/abs/2508.16532 |
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| _version_ | 1866918129110614016 |
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| author | Akiba, Ryunosuke Nimmo, Francis |
| author_facet | Akiba, Ryunosuke Nimmo, Francis |
| contents | The large Kuiper Belt object (KBO) Eris is nearly as big as Pluto and has a small moon, Dysnomia. Constraints on the system's spin and orbit characteristics were recently used to argue for a dissipative Eris, requiring a differentiated structure but not necessarily a subsurface ocean. Here, we model the thermal history of Eris coupled to its spin-orbital evolution, finding a subsurface ocean is preferred in order for Eris to be sufficiently dissipative. Spinning down Eris without an ocean is difficult, requiring a warm convecting ice shell protected by a thick insulating layer and very dissipative anelastic behavior in ice. Oceans make up 77-100% of successful thermal-orbital evolution models, depending on the parameters assumed, which increases to >98% when the Andrade $β$ parameter for ice is restricted to $β\leq3\times10^{-11}$ Pa$^{-1}$ s$^{-0.25}$. Oceans freeze over by the present day unless insulation (porosity, gas clathrates) or antifreeze are present. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_16532 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Thermal-orbital evolution of Eris Akiba, Ryunosuke Nimmo, Francis Earth and Planetary Astrophysics The large Kuiper Belt object (KBO) Eris is nearly as big as Pluto and has a small moon, Dysnomia. Constraints on the system's spin and orbit characteristics were recently used to argue for a dissipative Eris, requiring a differentiated structure but not necessarily a subsurface ocean. Here, we model the thermal history of Eris coupled to its spin-orbital evolution, finding a subsurface ocean is preferred in order for Eris to be sufficiently dissipative. Spinning down Eris without an ocean is difficult, requiring a warm convecting ice shell protected by a thick insulating layer and very dissipative anelastic behavior in ice. Oceans make up 77-100% of successful thermal-orbital evolution models, depending on the parameters assumed, which increases to >98% when the Andrade $β$ parameter for ice is restricted to $β\leq3\times10^{-11}$ Pa$^{-1}$ s$^{-0.25}$. Oceans freeze over by the present day unless insulation (porosity, gas clathrates) or antifreeze are present. |
| title | Thermal-orbital evolution of Eris |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2508.16532 |