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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Planet formation in a triple stellar system: implications of the third star's orbital inclination

Texto completo
Domingos, R. C. [1, 2] ; Winter, O. C. [1] ; Izidoro, A. [3, 2, 4]
Número total de Autores: 3
Afiliação do(s) autor(es):
[1] Univ Estadual Paulista, UNESP, Sao Joao Da Boa Vista, SP - Brazil
[2] Univ Estadual Paulista, UNESP, BR-12516410 Guaratingueta, SP - Brazil
[3] Minist Educ Brazil, CAPES Fdn, BR-70040020 Brasilia, DF - Brazil
[4] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange, F-06304 Nice 4 - France
Número total de Afiliações: 4
Tipo de documento: Artigo Científico
Fonte: International Journal of Astrobiology; v. 14, n. 2, SI, p. 153-163, APR 2015.
Citações Web of Science: 1

Planets have been revealed both in binary and triple stellar systems. Although there have been several studies of the late stages of planet formation in binary stars this process does not appear to have been studied in triple stellar systems. To understand how the late stage of planetary accretion is affected by a third companion, in this work we have numerically investigated the formation of planets in a hypothetical triple stellar system. The system is composed by an inner binary formed by two half-solar-mass components orbited by a solar-mass star. In our experiments, lunar and Mars-sized planetary embryos are distributed around the centre of mass of the inner binary system. Our main goal is to analyse how the formation of planets evolves depending on the orbital configuration of the massive distant companion. We have performed an extensive number of numerical simulations considering different orbital configurations for the third star. All simulations were numerically integrated for at least 10(7) years. The results show that when the protoplanetary disc and the stars are initially on coplanar orbits, one or two planets are quickly formed between 6 and 8AU. In general such planets have also small eccentricities with values about 10(-2). On the other hand, when the third star is considered initially on inclined orbits (even tiny values), there tends to occur a significant increase in the inclination of bodies of protoplanetary disc, which prevents the collisions between these objects and their growth. As a result, in this latter case we do not evidence the formation of planets during the timescale of our integrations but note the existence of several leftover objects that can survive for longer than 10Myr, moving in orbits with semi-major axes ranging between similar to 6 and 8AU. Thus, our results do not rule out the planet formation in this kind of stellar arrangements at all, but they indicate that, if planetary bodies keep stable orbits, the late stage of planet formation in systems with a highly inclined third star can be a very long process and many of these triple hierarchical systems might not have had time to form planets and planetary systems. They could be harbouring only debris discs, fragments or planetesimals. (AU)

Processo FAPESP: 08/08679-4 - Estabilidade de discos e formação planetária ao redor de sistemas binários
Beneficiário:Rita de Cássia Domingos
Modalidade de apoio: Bolsas no Brasil - Pós-Doutorado
Processo FAPESP: 11/08171-3 - Dinâmica orbital de pequenos corpos
Beneficiário:Othon Cabo Winter
Modalidade de apoio: Auxílio à Pesquisa - Temático