Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation
This paper deals with the formation and evolution of Mars’ moons, Phobos and Deimos, assuming the dislocation of a larger progenitor as the origin of these moons. The study by R. Hyodo et al. argues that under somewhat simplistic modeling, the postdislocation orbits of Phobos and Deimos inevitably c...
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| Format: | Article |
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IOP Publishing
2025-01-01
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| Series: | The Planetary Science Journal |
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| Online Access: | https://doi.org/10.3847/PSJ/adcab2 |
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| author | Ryan Dahoumane Kévin Baillié Valéry Lainey |
| author_facet | Ryan Dahoumane Kévin Baillié Valéry Lainey |
| author_sort | Ryan Dahoumane |
| collection | DOAJ |
| description | This paper deals with the formation and evolution of Mars’ moons, Phobos and Deimos, assuming the dislocation of a larger progenitor as the origin of these moons. The study by R. Hyodo et al. argues that under somewhat simplistic modeling, the postdislocation orbits of Phobos and Deimos inevitably collide within 10,000 yr, leading to their mutual annihilation. These findings are based on ${ \mathcal N }$ -body simulations, accounting for Mars’ J _2 and J _4 gravitational perturbations and mutual perturbations between the moons. In this paper, we challenge these findings by extending their work. We incorporate important perturbations such as solar perturbations, Mars’ axial precession and nutation, and its deformation along three axes. We also extend some of the hypotheses made by R. Hyodo et al. concerning the initial distribution of Phobos and Deimos after the dislocation. Our analysis reveals that including these additional perturbations, as well as the possibility of having more than two fragments after the dislocation, does not alter the ultimate fate of Phobos and Deimos. The moons still converge towards collision within comparable timescales, supporting R. Hyodo et al.'s conclusions that the dislocation hypothesis under the dynamical scenario developed by A. Bagheri et al. has, in the best conditions, about a 10% chance of surviving after the first 100,000 yr following their formation. |
| format | Article |
| id | doaj-art-99a27ded9c3647d7bb0fd9476cbfe75c |
| institution | Kabale University |
| issn | 2632-3338 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Planetary Science Journal |
| spelling | doaj-art-99a27ded9c3647d7bb0fd9476cbfe75c2025-08-20T03:47:33ZengIOP PublishingThe Planetary Science Journal2632-33382025-01-016511810.3847/PSJ/adcab2Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential DislocationRyan Dahoumane0https://orcid.org/0009-0005-8382-8181Kévin Baillié1Valéry Lainey2LTE, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Lille, LNE,CNRS , 61 Avenue de l’Observatoire, 75014 Paris, France ; ryan.dahoumane@obspm.frLTE, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Lille, LNE,CNRS , 61 Avenue de l’Observatoire, 75014 Paris, France ; ryan.dahoumane@obspm.frLTE, Observatoire de Paris, Université PSL, Sorbonne Université, Université de Lille, LNE,CNRS , 61 Avenue de l’Observatoire, 75014 Paris, France ; ryan.dahoumane@obspm.frThis paper deals with the formation and evolution of Mars’ moons, Phobos and Deimos, assuming the dislocation of a larger progenitor as the origin of these moons. The study by R. Hyodo et al. argues that under somewhat simplistic modeling, the postdislocation orbits of Phobos and Deimos inevitably collide within 10,000 yr, leading to their mutual annihilation. These findings are based on ${ \mathcal N }$ -body simulations, accounting for Mars’ J _2 and J _4 gravitational perturbations and mutual perturbations between the moons. In this paper, we challenge these findings by extending their work. We incorporate important perturbations such as solar perturbations, Mars’ axial precession and nutation, and its deformation along three axes. We also extend some of the hypotheses made by R. Hyodo et al. concerning the initial distribution of Phobos and Deimos after the dislocation. Our analysis reveals that including these additional perturbations, as well as the possibility of having more than two fragments after the dislocation, does not alter the ultimate fate of Phobos and Deimos. The moons still converge towards collision within comparable timescales, supporting R. Hyodo et al.'s conclusions that the dislocation hypothesis under the dynamical scenario developed by A. Bagheri et al. has, in the best conditions, about a 10% chance of surviving after the first 100,000 yr following their formation.https://doi.org/10.3847/PSJ/adcab2Celestial mechanicsMartian satellitesN-body simulationsNatural satellite formationPlanetary system formation |
| spellingShingle | Ryan Dahoumane Kévin Baillié Valéry Lainey Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation The Planetary Science Journal Celestial mechanics Martian satellites N-body simulations Natural satellite formation Planetary system formation |
| title | Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation |
| title_full | Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation |
| title_fullStr | Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation |
| title_full_unstemmed | Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation |
| title_short | Origin of Phobos and Deimos: Orbital Evolution Shortly after Formation from a Potential Dislocation |
| title_sort | origin of phobos and deimos orbital evolution shortly after formation from a potential dislocation |
| topic | Celestial mechanics Martian satellites N-body simulations Natural satellite formation Planetary system formation |
| url | https://doi.org/10.3847/PSJ/adcab2 |
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