| Full text | |
| Author(s): |
Total Authors: 4
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| Affiliation: | [1] Sao Paulo State Univ, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[2] Natl Inst Space Res INPE, Lab Comp Aplicada, BR-12227010 Sao Jose Dos Campos, SP - Brazil
[3] State Univ Mato Grosso do Sul UEMS, BR-79540000 Cassilandia, MS - Brazil
[4] Fed Inst Educ Sci & Technol Sao Paulo IFSP, BR-11533160 Cubatao, SP - Brazil
[5] Fed Univ Sao Paulo UNIFESP, Inst Sci & Technol, BR-12247014 Sao Jose Dos Campos, SP - Brazil
Total Affiliations: 5
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| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 504, n. 4, p. 6144-6156, JUL 2021. |
| Web of Science Citations: | 0 |
| Abstract | |
The Kepler-1647 is a binary system with two Sun-type stars (approximate to 1.22 and approximate to 0.97 M-circle dot). It has the most massive circumbinary planet (approximate to 1.52 M-lup) with the longest orbital period (approximate to 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-16476. 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. (AU) | |
| FAPESP's process: | 15/50122-0 - Dynamic phenomena in complex networks: basics and applications |
| Grantee: | Elbert Einstein Nehrer Macau |
| Support Opportunities: | Research Projects - Thematic Grants |
| FAPESP's process: | 13/07375-0 - CeMEAI - Center for Mathematical Sciences Applied to Industry |
| Grantee: | Francisco Louzada Neto |
| Support Opportunities: | Research Grants - Research, Innovation and Dissemination Centers - RIDC |
| FAPESP's process: | 16/24561-0 - On the relevance of small bodies in orbital dynamics |
| Grantee: | Othon Cabo Winter |
| Support Opportunities: | Research Projects - Thematic Grants |