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Constraining the oblateness of Kepler planets

Zhu, Wei; Huang, Chelsea X.; Zhou, Guyin (George); Lin, D. N. C.

Description

We use Kepler short-cadence light curves to constrain the oblateness of planet candidates in the Kepler sample. The transits of rapidly rotating planets that are deformed in shape will lead to distortions in the ingress and egress of their light curves. We report the first tentative detection of an oblate planet outside the solar system, measuring an oblateness of for the 18 MJ mass brown dwarf Kepler 39b (KOI 423.01). We also provide constraints on the oblateness of the planets (candidates)...[Show more]

dc.contributor.authorZhu, Wei
dc.contributor.authorHuang, Chelsea X.
dc.contributor.authorZhou, Guyin (George)
dc.contributor.authorLin, D. N. C.
dc.date.accessioned2015-12-13T22:34:15Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/76041
dc.description.abstractWe use Kepler short-cadence light curves to constrain the oblateness of planet candidates in the Kepler sample. The transits of rapidly rotating planets that are deformed in shape will lead to distortions in the ingress and egress of their light curves. We report the first tentative detection of an oblate planet outside the solar system, measuring an oblateness of for the 18 MJ mass brown dwarf Kepler 39b (KOI 423.01). We also provide constraints on the oblateness of the planets (candidates) HAT-P-7b, KOI 686.01, and KOI 197.01 to be <0.067, <0.251, and <0.186, respectively. Using the Q′ values from Jupiter and Saturn, we expect tidal synchronization for the spins of HAT-P-7b, KOI 686.01, and KOI 197.01, and for their rotational oblateness signatures to be undetectable in the current data. The potentially large oblateness of KOI 423.01 (Kepler 39b) suggests that the Q′ value of the brown dwarf needs to be two orders of magnitude larger than that of the solar system gas giants to avoid being tidally spun down.
dc.publisherIOP Publishing
dc.sourceAstrophysical Journal, The
dc.titleConstraining the oblateness of Kepler planets
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume796
dc.date.issued2014
local.identifier.absfor030600 - PHYSICAL CHEMISTRY (INCL. STRUCTURAL)
local.identifier.ariespublicationU3488905xPUB4951
local.type.statusPublished Version
local.contributor.affiliationZhu, Wei, The Ohio State University
local.contributor.affiliationHuang, Chelsea X., Princeton University
local.contributor.affiliationZhou, Guyin (George), College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationLin, D.N.C., University of California
local.description.embargo2037-12-31
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage1
local.bibliographicCitation.lastpage18
local.identifier.doi10.1088/0004-637X/796/1/67
dc.date.updated2015-12-11T09:19:24Z
local.identifier.scopusID2-s2.0-84910097273
local.identifier.thomsonID000344550300067
CollectionsANU Research Publications

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