Skip to main content

Dynamical Constraints on the Core Mass of Hot Jupiter HAT-P-13b

Author(s): Buhler, Peter B; Knutson, Heather A; Batygin, Konstantin; Fulton, Benjamin J; Fortney, Jonathan J; et al

Download
To refer to this page use: http://arks.princeton.edu/ark:/88435/pr1jh7t
Full metadata record
DC FieldValueLanguage
dc.contributor.authorBuhler, Peter B-
dc.contributor.authorKnutson, Heather A-
dc.contributor.authorBatygin, Konstantin-
dc.contributor.authorFulton, Benjamin J-
dc.contributor.authorFortney, Jonathan J-
dc.contributor.authorBurrows, Adam S-
dc.contributor.authorWong, Ian-
dc.date.accessioned2019-04-10T19:31:32Z-
dc.date.available2019-04-10T19:31:32Z-
dc.date.issued2016-04en_US
dc.identifier.citationBuhler, Peter B, Knutson, Heather A, Batygin, Konstantin, Fulton, Benjamin J, Fortney, Jonathan J, Burrows, Adam, Wong, Ian. (2016). Dynamical Constraints on the Core Mass of Hot Jupiter HAT-P-13b. \apj, 821 (26 - 26. doi:10.3847/0004-637X/821/1/26en_US
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1jh7t-
dc.description.abstractHAT-P-13b is a Jupiter-mass transiting exoplanet that has settled onto a stable, short-period, and mildly eccentric orbit as a consequence of the action of tidal dissipation and perturbations from a second, highly eccentric, outer companion. Owingto the special orbital configuration of the HAT-P-13 system, the magnitude of HAT-P-13bʼseccentricity(eb)is in part dictated by its Love number(k2b), which is in turn a proxy for the degree of central mass concentration in its interior. Thus, the measurement ofebconstrainsk2band allows us to place otherwise elusive constraints on the mass of HAT-P-13bʼs core(Mcore,b). In this study we derive new constraints on the value of eb by observing two secondary eclipses of HAT-P-13b with the Infrared Array Camera on board the Spitzer Space Telescope.Wefit the measured secondary eclipse times simultaneously with radial velocity measurements and find that eb=0.00700±0.00100. We then use octupole-order secular perturbation theory to find the corresponding=-+k0.3120.050.08b. Applying structural evolution models, we then find, with 68% confidence, that Mcore,b is less than 25 Earth masses(M⊕). The most likely value isMcore,b=11M⊕, which is similar to the core mass theoretically required for runaway gas accretion. This is the tightest constraint to date on the core mass of a hot Jupiter. Additionally, we find that the measured secondary eclipse depths, which are in the 3.6 and 4.5μmbands, best match atmospheric model predictions with a dayside temperature inversion and relatively efficient day–night circulation.en_US
dc.language.isoen_USen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsAuthor's manuscripten_US
dc.titleDynamical Constraints on the Core Mass of Hot Jupiter HAT-P-13ben_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.3847/0004-637X/821/1/26-
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

Files in This Item:
File Description SizeFormat 
1602.03895.pdf740.83 kBAdobe PDFView/Download


Items in OAR@Princeton are protected by copyright, with all rights reserved, unless otherwise indicated.