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Stellar rotation period inference with Gaussian processes

Published online by Cambridge University Press:  27 October 2016

Ruth Angus ,
Susanne Aigrain  and
Daniel Foreman-Mackey
Ruth Angus
Affiliation:
Subdepartment of Astrophysics, University of Oxford, Oxford, UKruth.angus@astro.ox.ac.uk, suzanne.aigrain@astro.ox.ac.uk
Susanne Aigrain
Affiliation:
Subdepartment of Astrophysics, University of Oxford, Oxford, UKruth.angus@astro.ox.ac.uk, suzanne.aigrain@astro.ox.ac.uk
Daniel Foreman-Mackey
Affiliation:
Sagan Fellow, Department of Astronomy, University of Washington, Seattle email: danfm@uw.edu
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The light curves of spotted, rotating stars are often non-sinusoidal and Quasi-Periodic (QP) and a strictly periodic sinusoid is therefore not a representative generative model. Ideally, a physical model of the stellar surface would be conditioned on the data, however the parameters of such models can be highly degenerate.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29A: Astronomy in Focus , August 2015 , pp. 191 - 192
Copyright
Copyright © International Astronomical Union 2016 

References

McQuillan, A., Mazeh, T., & Aigrain, S., 2014, ApJ, 211, 24 Google Scholar
Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J., 2013, PASP, 125, 306 CrossRefGoogle Scholar
Foreman-Mackey, D. 2015, https://github.com/dfm/george.Google Scholar