The habitability of Proxima Centauri b II. Possible climates and Observability
dc.contributor.author | TURBET, Martin, | |
hal.structure.identifier | ECLIPSE 2016 | |
dc.contributor.author | LECONTE, J. | |
hal.structure.identifier | ECLIPSE 2016 | |
dc.contributor.author | SELSIS, Franck | |
hal.structure.identifier | Namur Center for Complex Systems [Namur] [NaXys] | |
dc.contributor.author | BOLMONT, Emeline, | |
hal.structure.identifier | Laboratoire de Météorologie Dynamique (UMR 8539) [LMD] | |
dc.contributor.author | FORGET, Francois, | |
hal.structure.identifier | Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona | |
dc.contributor.author | RIBAS, Ignasi, | |
hal.structure.identifier | ECLIPSE 2016 | |
dc.contributor.author | RAYMOND, Sean N. | |
dc.contributor.author | ANGLADA-ESCUDÉ, Guillem, | |
dc.date.issued | 2016-08 | |
dc.identifier.issn | 0004-6361 | |
dc.description.abstractEn | Radial velocity monitoring has found the signature of a $M \sin i = 1.3$~M$_\oplus$ planet located within the Habitable Zone of Proxima Centauri, (Anglada-Escud\'e et al. 2016). Despite a hotter past and an active host star the planet Proxima~b could have retained enough volatiles to sustain surface habitability (Ribas et al. 2016). Here we use a 3D Global Climate Model to simulate Proxima b's atmosphere and water cycle for its two likely rotation modes (1:1 and 3:2 resonances) while varying the unconstrained surface water inventory and atmospheric greenhouse effect. We find that a broad range of atmospheric compositions can allow surface liquid water. On a tidally-locked planet with a surface water inventory larger than 0.6 Earth ocean, liquid water is always present, at least in the substellar region. Liquid water covers the whole planet for CO$_2$ partial pressures $\gtrsim 1$~bar. For smaller water inventories, water can be trapped on the night side, forming either glaciers or lakes, depending on the amount of greenhouse gases. With a non-synchronous rotation, a minimum CO$_2$ pressure is required to avoid falling into a completely frozen snowball state if water is abundant. If the planet is dryer, $\sim$0.5~bar of CO$_2$ would suffice to prevent the trapping of any arbitrary small water inventory into polar ice caps. More generally, any low-obliquity planet within the classical habitable zone of its star should be in one of the climate regimes discussed here. We use our GCM to produce reflection/emission spectra and phase curves. We find that atmospheric characterization will be possible by direct imaging with forthcoming large telescopes thanks to an angular separation of $7 \lambda/D$ at 1~$\mu$m (with the E-ELT) and a contrast of $\sim 10^{-7}$. The magnitude of the planet will allow for high-resolution spectroscopy and the search for molecular signatures. | |
dc.language.iso | en | |
dc.publisher | EDP Sciences | |
dc.subject.en | Astrophysics - Earth and Planetary Astrophysics | |
dc.title.en | The habitability of Proxima Centauri b II. Possible climates and Observability | |
dc.type | Article de revue | |
dc.identifier.doi | 10.1051/0004-6361/201629577 | |
dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP] | |
dc.identifier.arxiv | 1608.06827 | |
bordeaux.journal | Astronomy and Astrophysics - A&A | |
bordeaux.page | id.A112 | |
bordeaux.volume | 596 | |
bordeaux.peerReviewed | oui | |
hal.identifier | hal-01359518 | |
hal.version | 1 | |
hal.popular | non | |
hal.audience | Internationale | |
hal.origin.link | https://hal.archives-ouvertes.fr//hal-01359518v1 | |
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