@Article{BarbosaWintAmarMaca:2021:FoEaPl,
               author = "Barbosa, Gerson de Oliveira and Winter, O. C. and Amarante, A. and 
                         Macau, Elbert Einstein Nehrer",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Universidade Estadual Paulista (UNESP)} and {Universidade 
                         Estadual Paulista (UNESP)} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)}",
                title = "Formation of Earth-sized planets within the Kepler-1647 system 
                         habitable zone",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2021",
               volume = "504",
               number = "4",
                pages = "6144--6156",
                month = "July",
             keywords = "Binaries: close, Planets and satellites: formation.",
             abstract = "The 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.",
                  doi = "10.1093/mnras/stab1165",
                  url = "http://dx.doi.org/10.1093/mnras/stab1165",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "barbosa-formation.pdf",
        urlaccessdate = "09 maio 2024"
}