期刊
ASTRONOMICAL JOURNAL
卷 163, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-3881/ac365f
关键词
-
资金
- Technologies for Exo-Planetary Science (TEPS) PhD Fellowship [NSERC: CREATE 4826]
- Natural Sciences and Engineering Research Council of Canada (NSERC) [NSERC: PGSD 534218-2019]
- NASA
- McGill Space Institute Graduate Fellowship
- Natural Sciences and Engineering Research Council of Canada [NSERC: PGSD 519511-2018]
- Fonds de recherche du Quebec-Nature et technologies through the Centre de recherche en astrophysique du Quebec
The study presents Spitzer full-orbit phase observations of the eccentric hot Jupiter XO-3b, measuring eclipse depths at 3.6 and 4.5 micrometers. Results show no evidence of previously reported dayside temperature inversion. By employing energy balance and atmospheric models, the study deduced the zonal wind speed, pressure, and other characteristics of XO-3b, comparing observations with 1D and 3D models to analyze its inflated radius and internal heating requirements.
We report Spitzer full-orbit phase observations of the eccentric hot Jupiter XO-3b at 3.6 and 4.5 mu m. Our new eclipse depth measurements of 1770 +/- 180 ppm at 3.6 mu m and 1610 +/- 70 ppm at 4.5 mu m show no evidence of the previously reported dayside temperature inversion. We also empirically derive the mass and radius of XO-3b and its host star using Gaia DR3's parallax measurement and find a planetary mass M-p = 11.79 +/- 0.98 M-Jup and radius R-p = 1.295 +/- 0.066 R-Jup. We compare our Spitzer observations with multiple atmospheric models to constrain the radiative and advective properties of XO-3b. While the decorrelated 4.5 mu m observations are pristine, the 3.6 mu m phase curve remains polluted with detector systematics due to larger amplitude intrapixel sensitivity variations in this channel. We focus our analysis on the more reliable 4.5 mu m phase curve and fit an energy balance model with solid body rotation to estimate the zonal wind speed and the pressure of the bottom of the mixed layer. Our energy balance model fit suggests an eastward equatorial wind speed of 3.13(-0.83)(+0.26) km s(-1), an atmospheric mixed layer down to 2.40(-0.16)(+0.92) bars, and a Bond albedo of 0.106(-0.106)(+0.008).( )We assume that the wind speed and mixed layer depth are constant throughout the orbit. We compare our observations with 1D planet-averaged model predictions at apoapse and periapse and 3D general circulation model predictions for X0-3b. We also investigate the inflated radius of XO-3b and find that it would require an unusually large amount of internal heating to explain the observed planetary radius.
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