Planetary dynamics

I am interested in understanding the dynamics of planetary systems, such as the (non-)circularity of planetary orbits and the (mis)alignment of the host stars rotation angle as compared to the planetary orbits (the obliquity), as well as mutual alignments of planets in multiplanet systems. Such measurements provide insight into the formation mechanisms of planetary systems.

For short period massive planets, orbital eccentricities can be routinely measured using radial velocity observations, while observing the Doppler shift during a planetary transit can constrain the star-planet obliquity (known as the Rossiter-McLaughlin effect).

I focus on small planets on longer-period orbits, for which such radial velocity observations are not possible. Studying stellar pulsations can provide the inclination of stars independent of the size of the planet, while knowing mass and radius of the planet can provide the orbital eccentricity by careful analysis of the planetary transit.

Image by Simon Albrecht, illustrating a misaligned orbit where the exoplanet HAT-P-7b orbits over the pole of its host star.

Exoplanet validation

An important part of exoplanet research is making sure that detected exoplanet candidates consist of genuine planets, i.e. to rule out any false positives.

When space missions (e.g. Kepler) observe a very tiny dip in brightness (of only a few hundred parts per million), we hope the cause is a transiting exoplanet moving in front of the star, blocking a tiny fraction of starlight. Binary stars can eclipse one another and also cause transits, but those eclipses are typically much deeper.

However, there are many stars in the sky. Sometimes several are in the same line of sight, so faint background stars can contaminate observations. If a faint binary star contaminates the bright star we observe, a deep binary star eclipse might be heavily diluted and look like a planetary transit. What we believe we see is a planetary transit, but instead we are observing a binary star in the background. These are false positives.

False positives can be ruled using follow-up measurements and additional observations, e.g. radial velocity follow-up or multi-colour photometry. High-resolution images from ground-based telescopes can spatially separate stars and reveal contaminant stars. I am particularly interested in using the shape of transits to rule out false positives, as well as combining optical and infrared photometry.

Phase curves

For close-in (large) exoplanets, the temperature and reflective properties can be measured by observing the combined brightness of the star and planet throughout one or more entire periods, as the planet changes phase. Measuring such a phase curve is comparable to looking at phases from the moon.

Analyzing phase curves, as well as secondary eclipses when the planet disappears behind its star, we can estimate the temperature of the planet's permanent dayside as well as its permanent nightside. Furthermore, the reflective properties (albedo) of the planet can be measured. The relative contribution of the planet's own heat and the reflection of light from the star depends on the wavelength, making it crucial to use multi-color observations.

Phase curves thereby provide information on the planet's atmosphere, including the presence of possible clouds.

Image credit: Josh Winn. Illustration of the observed light throughout the different phases of a tidally locked, close-in exoplanet.


Illustration of a pulsating red giant, by Pieter Degroote.


Understanding exoplanets requires understanding the host stars around which they orbit. Asteroseismology is the study of stellar pulsations and is an extremely useful tool to gain a detailed understanding of planet host stars.

Using asteroseismology, we can obtain precise stellar parameters, such as the mass, radius and age of the star. In some cases, asteroseismology can even be used to measure the stellar inclination angle and rotation period.