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Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1

hal.structure.identifierNamur Center for Complex Systems [Namur] [NaXys]
dc.contributor.authorBOLMONT, Emeline,
hal.structure.identifierECLIPSE 2017
dc.contributor.authorSELSIS, Franck
dc.contributor.authorOWEN, James E.,
hal.structure.identifierDpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona
dc.contributor.authorRIBAS, Ignasi,
hal.structure.identifierECLIPSE 2017
dc.contributor.authorRAYMOND, Sean N.
hal.structure.identifierECLIPSE 2017
dc.contributor.authorLECONTE, J.
hal.structure.identifierEnvironnement Méditerranéen et Modélisation des Agro-Hydrosystèmes [EMMAH]
dc.contributor.authorGILLON, Michael,
dc.date.issued2017
dc.identifier.issn0035-8711
dc.description.abstractEnUltracool dwarfs (UCD) encompass the population of extremely low mass stars (later than M6-type) and brown dwarfs. Because UCDs cool monotonically, their habitable zone (HZ) sweeps inward in time. Assuming they possess water, planets found in the HZ of UCDs have experienced a runaway greenhouse phase too hot for liquid water prior to entering the HZ. It has been proposed that such planets are desiccated by this hot early phase and enter the HZ as dry, inhospitable worlds. Here we model the water loss during this pre-HZ hot phase taking into account recent upper limits on the XUV emission of UCDs and using 1D radiation-hydrodynamic simulations. We address the whole range of UCDs but also focus on the planets b, c and d recently found around the $0.08~M_\odot$ dwarf TRAPPIST-1. Despite assumptions maximizing the FUV-photolysis of water and the XUV-driven escape of hydrogen, we find that planets can retain significant amounts of water in the HZ of UCDs, with a sweet spot in the $0.04$-$0.06~M_\odot$ range. With our assumptions, TRAPPIST-1b and c can lose as much as 4 Earth Ocean but planet d - which may be inside the HZ depending on its actual period - may have kept enough water to remain habitable depending on its initial content. TRAPPIST-1 planets are key targets for atmospheric characterization and could provide strong constraints on the water erosion around UCDs.
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.title.enWater loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1
dc.typeArticle de revue
dc.identifier.doi10.1093/mnras/stw2578
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1605.00616
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page3728-3741
bordeaux.volume464
bordeaux.issue3
bordeaux.peerReviewedoui
hal.identifierhal-01359535
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01359535v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Monthly%20Notices%20of%20the%20Royal%20Astronomical%20Society&rft.date=2017&rft.volume=464&rft.issue=3&rft.spage=3728-3741&rft.epage=3728-3741&rft.eissn=0035-8711&rft.issn=0035-8711&rft.au=BOLMONT,%20Emeline,&SELSIS,%20Franck&OWEN,%20James%20E.,&RIBAS,%20Ignasi,&RAYMOND,%20Sean%20N.&rft.genre=article


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