dc.contributor.author | Winn, Joshua N. | |
dc.contributor.author | Dai, Fei | |
dc.date.accessioned | 2017-11-20T20:16:04Z | |
dc.date.available | 2017-11-20T20:16:04Z | |
dc.date.issued | 2017-04 | |
dc.date.submitted | 2017-03 | |
dc.identifier.issn | 1538-3881 | |
dc.identifier.issn | 0004-6256 | |
dc.identifier.uri | http://hdl.handle.net/1721.1/112255 | |
dc.description.abstract | Observations of nine transits of WASP-107 during the K2 mission reveal three separate occasions when the planet crossed in front of a starspot. The data confirm the stellar rotation period to be 17 days - approximately three times the planet's orbital period - and suggest that large spots persist for at least one full rotation. If the star had a low obliquity, at least two additional spot crossings should have been observed. They were not observed, giving evidence for a high obliquity. We use a simple geometric model to show that the obliquity is likely in the range 40°-140°, i.e., both spin-orbit alignment and anti-alignment can be ruled out. WASP-107 thereby joins the small collection of relatively low-mass stars with a high obliquity. Most such stars have been observed to have low obliquities; all of the exceptions, including WASP-107, involve planets with relatively wide orbits ("warm Jupiters," with a[subscript min]/R∗ ≳ 8). This demonstrates a connection between stellar obliquity and planet properties, in contradiction to some theories for obliquity excitation. | en_US |
dc.publisher | American Astronomical Society | en_US |
dc.relation.isversionof | http://dx.doi.org/10.3847/1538-3881/AA65D1 | en_US |
dc.rights | Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. | en_US |
dc.source | IOP Publishing | en_US |
dc.title | The Oblique Orbit of WASP-107b from K2 Photometry | en_US |
dc.type | Article | en_US |
dc.identifier.citation | Dai, Fei, and Joshua N. Winn. “The Oblique Orbit of WASP-107b from K2 Photometry.” The Astronomical Journal, vol. 153, no. 5, Apr. 2017, p. 205. © 2017 The American Astronomical Society | en_US |
dc.contributor.department | Massachusetts Institute of Technology. Department of Physics | en_US |
dc.contributor.department | MIT Kavli Institute for Astrophysics and Space Research | en_US |
dc.contributor.mitauthor | Dai, Fei | |
dc.relation.journal | The Astronomical Journal | en_US |
dc.eprint.version | Final published version | en_US |
dc.type.uri | http://purl.org/eprint/type/JournalArticle | en_US |
eprint.status | http://purl.org/eprint/status/PeerReviewed | en_US |
dc.date.updated | 2017-10-19T13:45:11Z | |
dspace.orderedauthors | Dai, Fei; Winn, Joshua N. | en_US |
dspace.embargo.terms | N | en_US |
dc.identifier.orcid | https://orcid.org/0000-0002-8958-0683 | |
mit.license | PUBLISHER_POLICY | en_US |