Issue |
A&A
Volume 523, November-December 2010
|
|
---|---|---|
Article Number | A52 | |
Number of page(s) | 7 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201015052 | |
Published online | 16 November 2010 |
The Doppler shadow of WASP-3b
A tomographic analysis of Rossiter-McLaughlin observations
1
School of Physics & Astronomy, University of St
Andrews,
North Haugh, St Andrews,
Fife
KY16 9SS,
UK
e-mail: gm228@st-andrews.ac.uk
2
Astrophysics Research Centre, School of Mathematics &
Physics, Queen’s University, University Road, Belfast
BT7 1NN,
UK
3
Department of Physics, University of Oxford,
Denys Wilkinson Building, Keble
Road, Oxford
OX1 3RH,
UK
4
Observatoire de l’Université de Genève,
Chemin des Maillettes
51, 1290
Sauverny,
Switzerland
5
Institut d’Astrophysique de Paris, UMR7095 CNRS, Université Pierre
& Marie Curie, 98bis Bd
Arago, 75014
Paris,
France
6
Laboratoire d’Astrophysique de Marseille,
BP 8,
13376
Marseille, Cedex 12,
France
7
Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700
Santa Cruz de la Palma, Tenerife, Spain
Received:
26
May
2010
Accepted:
16
August
2010
Context. Hot-Jupiter planets must form at large separations from their host stars where the temperatures are cool enough for their cores to condense. They then migrate inwards to their current observed orbital separations. Different theories of how this migration occurs lead to varying distributions of orbital eccentricity and the alignment between the rotation axis of the star and the orbital axis of the planet.
Aims. The spin-orbit alignment of a transiting system is revealed via the Rossiter-McLaughlin effect, which is the anomaly present in the radial velocity measurements of the rotating star during transit due to the planet blocking some of the starlight. In this paper we aim to measure the spin-orbit alignment of the WASP-3 system via a new way of analysing the Rossiter-McLaughlin observations.
Methods. We apply a new tomographic method for analysing the time variable asymmetry of stellar line profiles caused by the Rossiter-McLaughlin effect. This new method eliminates the systematic error inherent in previous methods used to analyse the effect.
Results. We find a value for the projected stellar spin rate of
v sin i = 13.9 ± 0.03 km s-1 which is in
agreement with previous measurements but has a much higher precision. The system is found
to be well aligned, with ° which
favours an evolutionary history for WASP-3b involving migration through tidal interactions
with a protoplanetary disc. From comparison with isochrones we put an upper limit on the
age of the star of 2 Gyr.
Key words: planetary systems / line: profiles / techniques: spectroscopic / eclipses / stars: individual: WASP-3b
© ESO, 2010
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