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|a Winn, Joshua Nathan
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|a Massachusetts Institute of Technology. Department of Physics
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|a MIT Kavli Institute for Astrophysics and Space Research
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|a Winn, Joshua Nathan
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|a Winn, Joshua Nathan
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|a Albrecht, Simon H.
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|a Johnson, John Asher
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|a Howard, Andrew W.
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|a Marcy, Geoffrey W.
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|a Bakos, Gaspar A.
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|a Hartman, Joel D.
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|a Torres, Guillermo
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|a Albrecht, Simon H.
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|a Narita, Norio
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|a The HAT-P-13 Exoplanetary System: Evidence for Spin-Orbit Alignment and a Third Companion
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|b Institute of Physics,
|c 2011-04-07T19:55:46Z.
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|z Get fulltext
|u http://hdl.handle.net/1721.1/62161
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|a We present new radial velocity (RV) measurements of HAT-P-13, a star with two previously known companions: a transiting giant planet "b" with an orbital period of 3 days and a more massive object "c" on a 1.2 yr, highly eccentric orbit. For this system, dynamical considerations would lead to constraints on planet b's interior structure, if it could be shown that the orbits are coplanar and apsidally locked. By modeling the Rossiter-McLaughlin effect, we show that planet b's orbital angular momentum vector and the stellar spin vector are well aligned on the sky ([lambda] = 1.9 ± 8.6 deg). The refined orbital solution favors a slightly eccentric orbit for planet b (e = 0.0133 ± 0.0041), although it is not clear whether it is apsidally locked with c's orbit ([DELTA][omega]= 36[superscript +27] [subscript -36]deg). We find a long-term trend in the star's RV and interpret it as evidence for an additional body "d," which may be another planet or a low-mass star. Predictions are given for the next few inferior conjunctions of c, when transits may happen.
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|a Massachusetts Institute of Technology (Class of 1942)
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|a United States. National Aeronautics and Space Administration (Origins program, award NNX09AD36G)
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|a National Science Foundation (U.S.) (Grant No. NSF PHY05-51164)
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|a W. M. Keck Foundation
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|a en_US
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|a Article
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|t Astrophysical Journal
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