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Formation of Earth-sized planets within the Kepler-1647 system habitable zone

dc.contributor.authorBarbosa, G. O. [UNESP]
dc.contributor.authorWinter, O. C. [UNESP]
dc.contributor.authorAmarante, A. [UNESP]
dc.contributor.authorMacau, E. E.N.
dc.contributor.institutionNational Institute for Space Research (INPE)
dc.contributor.institutionUniversidade Estadual Paulista (UNESP)
dc.contributor.institutionUniversidade Estadual de Mato Grosso do Sul (UEMS)
dc.contributor.institutionScience and Technology of São Paulo (IFSP)
dc.contributor.institutionUniversidade de São Paulo (USP)
dc.date.accessioned2022-05-01T05:29:33Z
dc.date.available2022-05-01T05:29:33Z
dc.date.issued2021-07-01
dc.description.abstractThe Kepler-1647 is a binary system with two Sun-type stars (≈1.22 and ≈0.97 M⊙). It has the most massive circumbinary planet (≈1.52 MJup) with the longest orbital period (≈1107.6 d) detected by the Kepler probe and is located within the habitable zone (HZ) of the system. In this work, we investigated the ability to form and house an Earth-sized planet within its HZ. First, we computed the limits of its HZ and performed numerical stability tests within that region. We found that HZ has three subregions that show stability, one internal, one co-orbital, and external to the host planet Kepler-1647b. Within the limits of these three regions, we performed numerical simulations of planetary formation. In the regions inner and outer to the planet, we used two different density profiles to explore different conditions of formation. In the co-orbital region, we used eight different values of total disc mass. We showed that many resonances are located within regions causing much of the disc material to be ejected before a planet is formed. Thus, the system might have two asteroid belts with Kirkwood gaps, similar to the Solar system's main belt of asteroids. The co-orbital region proved to be extremely sensitive, not allowing the planet formation, but showing that this binary system has the capacity to have Trojan bodies. Finally, we looked for regions of stability for an Earth-sized moon. We found that there is stability for a moon with this mass up to 0.4 Hill's radius from the host planet.en
dc.description.affiliationLaboratório de Computação Aplicada National Institute for Space Research (INPE)
dc.description.affiliationGrupo de Dinâmica Orbital e Planetologia São Paulo State University (UNESP)
dc.description.affiliationState University of Mato Grosso Do sul (UEMS)
dc.description.affiliationFederal Institute of Education Science and Technology of São Paulo (IFSP)
dc.description.affiliationFederal University of São Paulo (UNIFESP) Institute for Science and Technology
dc.description.affiliationUnespGrupo de Dinâmica Orbital e Planetologia São Paulo State University (UNESP)
dc.description.sponsorshipConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.description.sponsorshipIdCNPq: 305210/2018-1
dc.format.extent6144-6156
dc.identifierhttp://dx.doi.org/10.1093/mnras/stab1165
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, v. 504, n. 4, p. 6144-6156, 2021.
dc.identifier.doi10.1093/mnras/stab1165
dc.identifier.issn1365-2966
dc.identifier.issn0035-8711
dc.identifier.scopus2-s2.0-85108620219
dc.identifier.urihttp://hdl.handle.net/11449/233191
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.sourceScopus
dc.subjectBinaries: close
dc.subjectPlanets and satellites: formation
dc.titleFormation of Earth-sized planets within the Kepler-1647 system habitable zoneen
dc.typeArtigo
unesp.departmentMatemática - FEGpt

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