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Thermal Phase Variations of WASP-12b: Defying Predictions

Author(s): Cowan, Nicolas B; Machalek, Pavel; Croll, Bryce; Shekhtman, Louis M; Burrows, Adam S; et al

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dc.contributor.authorCowan, Nicolas B-
dc.contributor.authorMachalek, Pavel-
dc.contributor.authorCroll, Bryce-
dc.contributor.authorShekhtman, Louis M-
dc.contributor.authorBurrows, Adam S-
dc.contributor.authorDeming, Drake-
dc.contributor.authorGreene, Tom-
dc.contributor.authorHora, Joseph L-
dc.identifier.citationCowan, Nicolas B, Machalek, Pavel, Croll, Bryce, Shekhtman, Louis M, Burrows, Adam, Deming, Drake, Greene, Tom, Hora, Joseph L. (2012). Thermal Phase Variations of WASP-12b: Defying Predictions. apj, 747 (82 - 82. doi:10.1088/0004-637X/747/1/82en_US
dc.description.abstractWe report Warm Spitzer full-orbit phase observations of WASP-12b at 3.6 and 4.5μm. This extremely inflated hot Jupiter is thought to be overflowing its Roche lobe, undergoing mass loss and accretion onto its host star, and has been claimed to have a C/O ratio in excess of unity. We are able to measure the transit depths, eclipse depths, thermal and ellipsoidal phase variations at both wavelengths. The large-amplitude phase variations, combined with the planet’s previously measured dayside spectral energy distribution, are indicative of non-zero Bond albedo and very poor day–night heat redistribution. The transit depths in the mid-infrared—(Rp/R∗) 2 = 0.0123(3) and 0.0111(3) at 3.6 and 4.5μm, respectively—indicate that the atmospheric opacity is greater at 3.6 than at 4.5μm, in disagreement with model predictions, irrespective of C/O ratio. The secondary eclipse depths are consistent with previous studies: Fday/F∗ = 0.0038(4) and 0.0039(3) at 3.6 and 4.5μm, respectively. We do not detect ellipsoidal variations at 3.6μm, but our parameter uncertainties—estimated via prayer-bead Monte Carlo—keep this non-detection consistent with model predictions. At 4.5μm, on the other hand, we detect ellipsoidal variations that are much stronger than predicted. If interpreted as a geometric effect due to the planet’s elongated shape, these variations imply a 3:2 ratio for the planet’s longest:shortest axes and a relatively bright day–night terminator. If we instead presume that the 4.5μm ellipsoidal variations are due to uncorrected systematic noise and we fix the amplitude of the variations to zero, the best-fit 4.5μm transit depth becomes commensurate with the 3.6μm depth, within the uncertainties. The relative transit depths are then consistent with a solar composition and short scale height at the terminator. Assuming zero ellipsoidal variations also yields a much deeper 4.5μm eclipse depth, consistent with a solar composition and modest temperature inversion. We suggest future observations that could distinguish between these two scenarios.en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsFinal published version. This is an open access article.en_US
dc.titleThermal Phase Variations of WASP-12b: Defying Predictionsen_US
dc.typeJournal Articleen_US

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