dc.contributor.author | Drummond, B | |
dc.contributor.author | Mayne, NJ | |
dc.contributor.author | Baraffe, I | |
dc.contributor.author | Tremblin, P | |
dc.contributor.author | Manners, J | |
dc.contributor.author | Amundsen, D | |
dc.contributor.author | Goyal, J | |
dc.contributor.author | Acreman, D | |
dc.date.accessioned | 2018-01-04T14:45:44Z | |
dc.date.issued | 2018-01-03 | |
dc.description.abstract | In this work we have performed a series of simulations of the atmosphere of GJ 1214b assuming different metallicities
using the Met Office Unified Model (UM). The UM is a general circulation model (GCM) that solves the deep, nonhydrostatic
equations of motion and uses a flexible and accurate radiative transfer scheme, based on the two-stream
and correlated-k approximations, to calculate the heating rates. In this work we consistently couple a well-tested
Gibbs energy minimisation scheme to solve for the chemical equilibrium abundances locally in each grid cell for a
general set of elemental abundances, further improving the flexibility and accuracy of the model. As the metallicity
of the atmosphere is increased we find significant changes in the dynamical and thermal structure, with subsequent
implications for the simulated phase curve. The trends that we find are qualitatively consistent with previous works,
though with quantitative differences. We investigate in detail the effect of increasing the metallicity by splitting the
mechanism into constituents, involving the mean molecular weight, the heat capacity and the opacities. We find the
opacity effect to be the dominant mechanism in altering the circulation and thermal structure. This result highlights
the importance of accurately computing the opacities and radiative transfer in 3D GCMs. | en_GB |
dc.description.sponsorship | This work is partly supported by the European
Research Council under the European Community’s Seventh
Framework Programme (FP7/2007-2013 Grant Agreement No.
247060-PEPS and grant No. 320478-TOFU). BD acknowledges funding
from the European Research Council (ERC) under the European
Unions Seventh Framework Programme (FP7/2007-2013) / ERC
grant agreement no. 336792 and thanks the University of Exeter for
support through a PhD studentship. DSA acknowledges support from
the NASA Astrobiology Program through the Nexus for Exoplanet
System Science. NJM and JG’s contributions were in part funded by
a Leverhulme Trust Research Project Grant, and in part by a University
of Exeter College of Engineering, Mathematics and Physical
Sciences studentship. This work used the DiRAC Complexity system,
operated by the University of Leicester IT Services, which forms
part of the STFC DiRAC HPC Facility. This equipment is funded
by BIS National E-Infrastructure capital grant ST/K000373/1 and
STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of
the National E-Infrastructure. This work also used the University of
Exeter Supercomputer, a DiRAC Facility jointly funded by STFC,
the Large Facilities Capital Fund of BIS and the University of Exeter.
Material produced using Met Office Software. | en_GB |
dc.identifier.citation | Published online 03-01-2018 | en_GB |
dc.identifier.doi | 10.1051/0004-6361/201732010 | |
dc.identifier.uri | http://hdl.handle.net/10871/30831 | |
dc.language.iso | en | en_GB |
dc.publisher | EDP Sciences for European Southern Observatory (ESO) | en_GB |
dc.relation.url | http://hdl.handle.net/10871/32593 | |
dc.rights | ©ESO 2018 | |
dc.subject | planets and satellites: atmospheres | en_GB |
dc.subject | planets and satellites: composition | en_GB |
dc.title | The effect of metallicity on the atmospheres of exoplanets with fully coupled 3D hydrodynamics, equilibrium chemistry, and radiative transfer (article) | en_GB |
dc.type | Article | en_GB |
dc.identifier.issn | 0004-6361 | |
dc.description | This is the author accepted manuscript. The final version is available from EDP Sciences for European Southern Observatory (ESO) via the DOI in this record. | en_GB |
dc.description | The dataset associated with this article is located in ORE at: http://hdl.handle.net/10871/32593 | |
dc.identifier.journal | Astronomy and Astrophysics | en_GB |