Brothwell, RD, Watson, CA, Hebrard, G, Triaud, AHMJ, Cegla, HM, Santerne, A, Hebrard, E, Anderson, DR, Pollacco, D, Simpson, EK, Bouchy, F, Brown, DJA, Chew, YGM, Cameron, AC, Armstrong, DJ, Barros, SCC, Bento, J, Bochinski, J, Burwitz, V, Busuttil, R, Delrez, L, Doyle, AP, Faedi, F, Fumel, A, Gillon, M, Haswell, CA, Hellier, C, Jehin, E, Kolb, U, Lendl, M, Liebig, C, Maxted, PFL ORCID: https://orcid.org/0000-0003-3794-1317, McCormac, J, Miller, GRM, Norton, AJ, Pepe, F, Queloz, D, Rodriguez, J, Segransan, D, Skillen, I, Smalley, B ORCID: https://orcid.org/0000-0002-3456-087X, Stassun, KG, Udry, S, West, RG and Wheatley, PJ (2014) A window on exoplanet dynamical histories: Rossiter-McLaughlin observations of WASP-13b and WASP-32b. Monthly Notices of the Royal Astronomical Society, 440 (4). 3392 -3401.

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Abstract

We present Rossiter–McLaughlin observations of WASP-13b and WASP-32b and determine the sky-projected angle between the normal of the planetary orbit and the stellar rotation axis (λ). WASP-13b and WASP-32b both have prograde orbits and are consistent with alignment with measured sky-projected angles of λ=8∘+13−12 and λ=−2∘+17−19, respectively. Both WASP-13 and WASP-32 have Teff < 6250 K, and therefore, these systems support the general trend that aligned planetary systems are preferentially found orbiting cool host stars. A Lomb–Scargle periodogram analysis was carried out on archival SuperWASP data for both systems. A statistically significant stellar rotation period detection (above 99.9 per cent confidence) was identified for the WASP-32 system with Prot = 11.6 ± 1.0 days. This rotation period is in agreement with the predicted stellar rotation period calculated from the stellar radius, R*, and vsin i if a stellar inclination of i* = 90° is assumed. With the determined rotation period, the true 3D angle between the stellar rotation axis and the planetary orbit, ψ, was found to be ψ = 11° ± 14°. We conclude with a discussion on the alignment of systems around cool host stars with Teff < 6150 K by calculating the tidal dissipation time-scale. We find that systems with short tidal dissipation time-scales are preferentially aligned and systems with long tidal dissipation time-scales have a broad range of obliquities.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: techniques, photometric, radial velocities, stars, individual, WASP-13, WASP-32, planetary systems
Subjects: Q Science > QB Astronomy
Divisions: Faculty of Natural Sciences > School of Physical and Geographical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 03 Nov 2016 11:17
Last Modified: 20 May 2019 10:58
URI: http://eprints.keele.ac.uk/id/eprint/2418

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