My peer-reviewed publications
I started working on circumbinary planets in 2012 during my honours year, at which point only half of the presently-known circumbinary planets were published. Below are my peer-reviewed publications in chronological order with a short description. There are links to the ADS database to obtain the published version and also freely-available PDFs posted to arXiv
2018
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"Populations of planets in multiple star systems," Martin, D. V., 2018, invited review chapter in "Handbook of Exoplanets," editors Deeg, H. J & Belmonte, J. A. (arXiv)
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In this review article I summarise observational and theoretical efforts to date regarding planets in multiple star systems. This includes both circumbinary planets and circumstellar planets in wider binaries.
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2017
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The WASP planet survey is looking for transiting hot Jupiters - giant planets orbiting very close to their host star. Hot Jupiters are similar in size to M dwarf stars, and hence from transits alone it is hard to know the difference. Radial velocity follow-up breaks the degeneracy by measuring the mass, which is very different in the two cases. Many people would throw away the M dwarf's as false positives but Amaury Triaud used them to form the EBLM program. This is a wonderful comparison sample with the hot Jupiters, and also have implications on the formation and evolution of close binaries and tidal interactions. This is the first major data release of spectroscopic orbits, which will be roughly doubled next year.
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In the EBLM program one target was particularly sexy: EBLM J0555-57. It has a mass 85 times that of Jupiter, which is similar to the TRAPPIST-1 host star, but a radius only as big as Jupiter. It is only just above the hydrogen burning limit. It is one of the densest non-stellar remnants known and the smallest star ever measured (or, as Fox News called it, the "wimpiest").
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It turns out that a lot of the ideas regarding the transit probability of circumbinary planets can also be applied to circumstellar planets in binaries, where the planet only orbits one of the two stars. If the binary is close, say an AU apart, then the planetary orbit will precess on a timescale that is relevant to long surveys like Kepler. This makes its transit signature come and go and probably harder to detect, which may explain why none have been found so far. I then applied the same theory to exomoons, which also have never been observed, and showed them to exhibit similar characteristics.
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Because circumbinary planets transit a moving binary target, and move through orbits that are themselves varying over time, your chance of observing a transit becomes inherently time-dependent. In this second paper on circumbinary transit probabilities I calculate when exactly the planet and binary orbits overlap, and apply this to re-observations of known planets. From this I calculated that Kepler has missed perhaps up to 75% of circumbinary planets that will later transit. This was picked up on by the New Scientist and a French science podcast.
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2016
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Kozai-Lidov cycles are synonymous with misaligned triple systems, but what about misaligned circumbinary planets? It turns out that the Kozai-Lidov effect is not applicable to circumbinary planets because it requires the outer orbit to have a lot of angular momentum, and circumbinary planets are just too small. Amaury and I had suspect this for a while but finally published clear proof of it, as well as some interesting intermediate cases where the outer orbit has similar angular momentum to the inner.
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2015
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All of the circumbinary planets had been found around eclipsing binaries, and most eclipsing binaries have very tight periods, less than a few days. It therefore seemed surprising that only wider binaries (periods greater than seven days) were known to host planets. With Tsevi Mazeh and Daniel Fabrycky we showed that this dearth of planets around the tightest binaries was compatible with a popular theory of tight binary formation by Kozai-Lidov cycles under the influence of a distant stellar companion. It was nice to use an observable (or in this case, non-observable) from exoplanets to advance our understanding of star formation.
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As early as my honours thesis in 2012, Amaury Triaud and I suspected that circumbinary planets were more likely to planets than planets around single stars. In this paper I sat down, tried to remember my undergraduate mathematics training and derived the analytic probability of circumbinary planets transiting, proving our suspicions. Amaury and I interpreted this to show the benefit of circumbinary planets and argued their importance in the broader astrophysical context.
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Transits generally probe circumbinary planets that are close to their host star. Astrometry, in particular that with high precision of the recently-launched GAIA satellite, can probe circumbinary planets on wider orbits. With Johannes Sahlmann and Amaury Triaud we predicted up to hundreds of future discoveries of wide circumbinary gas giants and circumbinary brown dwarfs, discoveries that will no doubt revolutionise the field.
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2014
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All planets had been discovered around eclipsing binaries, but most binaries do not eclipse. With Amaury Triaud we posed a very simple question: can you find planets transiting non-eclipsing binaries? The answer is yes, if the planet and binary orbits are misaligned. We predicted many should be detectable within the Kepler data. We also analysed the observed trends of circumbinary planets and showed which ones are meaningful and posed explanations for them.
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Using the earlier results of the 2013 paper on circumbinary transit timing variations, Dave Armstrong led a study to show that the abundance of circumbinary gas giants was surprisingly calculated to be at least as abundant as gas giants around single stars. I synthesised various distributions of circumbinary planets and simulated their transit timings. This tested the detection capabilities of the algorithm. A prediction of our work was that if many misaligned circumbinary planets exist that have presently elluded detection, then the underlying abundance would be even higher than that around single stars. A tantilising possibility indeed...
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2013
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Dave Armstrong was already working to write an algorithm to automatically detect and constrain the abundance of transiting circumbinary planets. The transits are more complex than those around single stars because the stars are themselves moving and the planet's orbit is not static. Together we derived analytic limits on the transit timing variations.
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