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dc.contributor.authorPozuelos Romero, Francisco José
dc.contributor.authorSuárez Yanes, Juan Carlos 
dc.date.accessioned2020-07-10T07:49:15Z
dc.date.available2020-07-10T07:49:15Z
dc.date.issued2020-06
dc.identifier.citationPozuelos, F. J., Suárez, J. C., de Elía, G. C., Berdiñas, Z. M., Bonfanti, A., Dugaro, A., ... & Garcia, L. J. (2020). GJ 273: On the formation, dynamical evolution and habitability of a planetary system hosted by an M dwarf at 3.75 parsec. arXiv preprint arXiv:2006.09403. [Forthcoming article: https://doi.org/10.1051/0004-6361/202038047]es_ES
dc.identifier.urihttp://hdl.handle.net/10481/62937
dc.description.abstractContext. Planets orbiting low-mass stars such as M dwarfs are now considered a cornerstone in the search for life-harbouring planets. GJ 273 is a planetary system orbiting an M dwarf only 3.75 pc away, composed of two confirmed planets, GJ 273b and GJ 273c, and two promising candidates, GJ 273d and GJ 273e. Planet GJ 273b resides in the habitable zone. Currently, due to a lack of observed planetary transits, only the minimum masses of the planets are known: Mb sin ib=2.89 M⊕, Mc sin ic=1.18 M⊕, Md sin id=10.80 M⊕, and Me sin ie=9.30 M⊕. Despite being an interesting system, the GJ 273 planetary system is still poorly studied. Aims. We aim at precisely determine the physical parameters of the individual planets, in particular to break the mass–inclination degeneracy to accurately determine the mass of the planets. Moreover, we present thorough characterisation of planet GJ 273b in terms of its potential habitability. Methods. First, we explored the planetary formation and hydration phases of GJ 273 during the first 100 Myr. Secondly, we analysed the stability of the system by considering both the two- and four-planet configurations. We then performed a comparative analysis between GJ 273 and the Solar System, and searched for regions in GJ 273 which may harbour minor bodies in stable orbits, i.e. main asteroid belt and Kuiper belt analogues. Results. From our set of dynamical studies, we obtain that the four-planet configuration of the system allows us to break the mass– inclination degeneracy. From our modelling results, the masses of the planets are unveiled as: 2:89 ≤ Mb ≤ 3:03 M⊕, 1:18 ≤ Mc ≤ 1:24 M⊕, 10:80 ≤ Md ≤ 11:35 M⊕ and 9:30 ≤ Me ≤ 9:70 M⊕. These results point to a system likely composed of an Earth-mass planet, a super-Earth and two mini-Neptunes. From planetary formation models, we determine that GJ 273b was likely an efficient water captor while GJ 273c is probably a dry planet. We found that the system may have several stable regions where minor bodies might reside. Collectively, these results are used to comprehensively discuss the habitability of GJ 273bes_ES
dc.description.sponsorshipSpanish Ministry of Science and Education Ramón y Cajal programme ESP2017-87676-2-2 RYC-2012-09913es_ES
dc.description.sponsorshipCONICYT- FONDECYT/Chile Postdoctorado 3180405es_ES
dc.description.sponsorshipMIT’s Kavli Institutees_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.rightsAtribución-NoComercial-SinDerivadas 3.0 España*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/*
dc.subjectGJ 273es_ES
dc.subjectM dwarfses_ES
dc.subjectPlanetary systemses_ES
dc.subjectPlanetary dynamicses_ES
dc.subjectTides es_ES
dc.subjectMinor-body reservoir analogueses_ES
dc.subjectHabitabilityes_ES
dc.titleGJ 273: On the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parseces_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.rights.accessRightsinfo:eu-repo/semantics/openAccesses_ES
dc.identifier.doi10.1051/0004-6361/202038047
dc.type.hasVersioninfo:eu-repo/semantics/submittedVersiones_ES


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