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The Oblique orbit of the Super-Neptune HAT-P-11b

Winn, Joshua N. and Johnson, John Asher and Howard, Andrew W. and Marcy, Geoffrey W. and Isaacson, Howard and Shporer, Avi and Bakos, Gáspár Á. and Hartman, Joel D. and Albrecht, Simon (2010) The Oblique orbit of the Super-Neptune HAT-P-11b. Astrophysical Journal Letters, 723 (2). L223-L227. ISSN 2041-8205.

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We find the orbit of the Neptune-sized exoplanet HAT-P-11b to be highly inclined relative to the equatorial plane of its host star. This conclusion is based on spectroscopic observations of two transits, which allowed the Rossiter–McLaughlin effect to be detected with an amplitude of 1.5m s^(−1). The sky-projected obliquity is 103^(+26) _(−10) deg. This is the smallest exoplanet for which spin–orbit alignment has been measured. The result favors a migration scenario involving few-body interactions followed by tidal dissipation. This finding also conforms with the pattern that the systems with the weakest tidal interactions have the widest spread in obliquities.We predict that the high obliquity of HAT-P-11 will be manifest in transit light curves from the Kepler spacecraft: starspot-crossing anomalies will recur at most once per stellar rotation period, rather than once per orbital period as they would for a well-aligned system.

Item Type:Article
Related URLs:
URLURL TypeDescription
Winn, Joshua N.0000-0002-4265-047X
Johnson, John Asher0000-0001-9808-7172
Howard, Andrew W.0000-0001-8638-0320
Marcy, Geoffrey W.0000-0002-2909-0113
Isaacson, Howard0000-0002-0531-1073
Shporer, Avi0000-0002-1836-3120
Bakos, Gáspár Á.0000-0001-7204-6727
Hartman, Joel D.0000-0001-8732-6166
Additional Information:© 2010 American Astronomical Society. Received 2010 September 7; accepted 2010 September 27; published 2010 October 20. We thank Norio Narita and Teruyuki Hirano for sharing their results prior to publication, and Dan Fabrycky and Scott Gaudi for helpful discussions. We acknowledge the support from the MIT Class of 1942, NASA grants NNX09AD36G (to J.N.W.) and NNX08AF23G (G.B.), and NSF grant AST- 0702843 (G.B.). The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA, and was made possible by the generous financial support of the W. M. Keck Foundation. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
NSF Astronomy and Astrophysics FellowshipAST-0702843
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:planetary systems – planets and satellites: formation – planet–star interactions – stars: rotation
Issue or Number:2
Classification Code:PACS: 97.82.-j; 95.30.Ky; 97.20.Jg; 97.10.Wn; 95.10.Gi; 97.10.Kc
Record Number:CaltechAUTHORS:20110106-144941893
Persistent URL:
Official Citation:Joshua N. Winn et al. 2010 ApJ 723 L223 doi: 10.1088/2041-8205/723/2/L223
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21635
Deposited By: Benjamin Perez
Deposited On:06 Jan 2011 23:20
Last Modified:09 Mar 2020 13:18

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