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dc.contributor.authorBlecic, Jasmina
dc.contributor.authorHarrington, Joseph
dc.contributor.authorMadhusudhan, Nikku
dc.contributor.authorStevenson, Kevin B.
dc.contributor.authorHardy, Ryan A.
dc.contributor.authorCubillos, Patricio E.
dc.contributor.authorHardin, Matthew
dc.contributor.authorBowman, Oliver
dc.contributor.authorNymeyer, Sarah
dc.contributor.authorAnderson, David R.
dc.contributor.authorHellier, Coel
dc.contributor.authorSmith, Alexis M. S.
dc.contributor.authorCollier Cameron, Andrew
dc.date.accessioned2014-09-02T09:01:01Z
dc.date.available2014-09-02T09:01:01Z
dc.date.issued2014-02-01
dc.identifier.citationBlecic , J , Harrington , J , Madhusudhan , N , Stevenson , K B , Hardy , R A , Cubillos , P E , Hardin , M , Bowman , O , Nymeyer , S , Anderson , D R , Hellier , C , Smith , A M S & Collier Cameron , A 2014 , ' Spitzer observations of the thermal emission from WASP-43b ' , Astrophysical Journal , vol. 781 , no. 2 , 116 . https://doi.org/10.1088/0004-637X/781/2/116en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 109776123
dc.identifier.otherPURE UUID: b9c0aead-bea0-452f-aa49-53c2d2da2755
dc.identifier.otherBibCode: 2014ApJ...781..116B
dc.identifier.otherScopus: 84892706654
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531418
dc.identifier.otherWOS: 000331171200060
dc.identifier.urihttp://hdl.handle.net/10023/5314
dc.descriptionSupport for this work was provided by NASA through an award issued by JPL/Caltech; through the Science Mission Directorate's Planetary Atmospheres Program, grant NNX12AI69G; Astrophysics Data Analysis Program, grant NNX13AF38G; and by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX12AL83H. N.M. acknowledges support from the Yale Center for Astronomy and Astrophysics through the YCAA postdoctoral Fellowship.en
dc.description.abstractWASP-43b is one of the closest-orbiting hot Jupiters, with a semimajor axis of a = 0.01526 ± 0.00018 AU and a period of only 0.81 days.However, it orbits one of the coolest stars with a hot Jupiter (T* = 4520 ± 120 K), giving the planet a modest equilibrium temperature of Teq = 1440 ± 40 K,assuming zero Bond albedo and uniform planetary energy redistribution.The eclipse depths and brightness temperatures from our jointly fit model are 0.347% ± 0.013% and 1670 ± 23 K at 3.6 μm and0.382% ± 0.015% and 1514 ± 25 K at 4.5 μm. The eclipse timings improved the estimate of the orbital period, P, by a factor of three (P = 0.81347436 ± 1.4 × 10-7 days) and put an upper limit on the eccentricity (e =0.010+0.010-0.007). We use our Spitzer eclipse depths along with four previously reported ground-based photometric observations in the near-infrared to constrain the atmospheric properties of WASP-43b. The data rule out a strong thermal inversion in the dayside atmosphere of WASP-43b. Model atmospheres with no thermal inversions and fiducial oxygen-rich compositions are able to explain all the available data.However, a wide range of metallicities and C/O ratios can explain the data. The data suggest low day-night energy redistribution in the planet, consistent with previous studies, with a nominal upper limit of about 35% for the fraction of energy incident on the dayside that is redistributed to the nightside.
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectEclipsesen
dc.subjectPlanets and satellites: atmospheresen
dc.subjectPlanets and satellites: individual: WASP-43ben
dc.subjectTechniques: photometricen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSpitzer observations of the thermal emission from WASP-43ben
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/781/2/116
dc.description.statusPeer revieweden


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