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The Shocking Variability Of Exoplanet Transits

Published online by Cambridge University Press:  06 January 2014

J. Llama ,
A. A. Vidotto ,
M. Jardine ,
K. Wood  and
R. Fares
J. Llama
Affiliation:
SUPA. University of St Andrews. North Haugh. St Andrews. KY16 9SS. UK email: joe.llama@st-andrews.ac.uk
A. A. Vidotto
Affiliation:
SUPA. University of St Andrews. North Haugh. St Andrews. KY16 9SS. UK email: joe.llama@st-andrews.ac.uk
M. Jardine
Affiliation:
SUPA. University of St Andrews. North Haugh. St Andrews. KY16 9SS. UK email: joe.llama@st-andrews.ac.uk
K. Wood
Affiliation:
SUPA. University of St Andrews. North Haugh. St Andrews. KY16 9SS. UK email: joe.llama@st-andrews.ac.uk
R. Fares
Affiliation:
SUPA. University of St Andrews. North Haugh. St Andrews. KY16 9SS. UK email: joe.llama@st-andrews.ac.uk
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Abstract

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Asymmetries in exoplanet transits are proving to be a useful tool for furthering our understanding of magnetic activity on both stars and planets outside our Solar System. Near-UV observations of the WASP- 12 system have revealed asymmetries in the timing of the transit when compared with the optical light curve. In this paper we review a number of reported asymmetries and present work simulating near-UV transits for the hot-Jupiter hosting star HD 189733.

Keywords

stars: activitycoronaeindividual (WASP-12, HD 189733)magnetic fieldsplanetary systemswinds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 262 - 265
Copyright
Copyright © International Astronomical Union 2013 

References

Fares, R., Donati, J., & Moutou, C., et al. 2010, MNRAS 406, 409CrossRefGoogle Scholar
Fossati, L., Haswell, C., Froning, C., et al. 2010, ApJ 714, L222Google Scholar
Lai, D., Helling, C. & van den Heuvel, E. P. J. 2010, ApJ, 721, 923CrossRefGoogle Scholar
Llama, J., Jardine, M., Mackay, D. H., & Fares, R. 2012, MNRAS 422, L72CrossRefGoogle Scholar
Llama, J., Wood, K., Jardine, M., Vidotto, A. A., et al., 2011, MNRAS 416, L41CrossRefGoogle Scholar
Powell, K. G., Roe, P. L., Linde, T. J., et al. 1999, Journal of Computational Physics, 154, 284Google Scholar
Sanchis-Ojeda, R., Winn, J. N., Holman, M. J., et al. 2011, ApJ, 733, 127CrossRefGoogle Scholar
Vidotto, A. A., Jardine, M., & Helling, C. 2010, ApJ, 722, L168CrossRefGoogle Scholar
Vidotto, A. A., Jardine, M., & Helling, Ch. 2011, MNRAS, 414, 1573CrossRefGoogle Scholar
Vidotto, A. A., Llama, J., Jardine, M., et al. 2011, Astronomische Nachrichten, 332, 1055Google Scholar
Wilkin, F. P. 1996, ApJ, 459, L31CrossRefGoogle Scholar