Imperial College London


Faculty of Natural SciencesDepartment of Physics

Senior Lecturer in Exoplanet Physics



+44 (0)20 7594 5785james.owen CV




Blackett LaboratorySouth Kensington Campus





My personal webpage.

I'm a theoretical astrophysicist in the Astrophysics group. I hold a senior Royal Society University Research Fellowship. Previously I was a Hubble Fellow at the Institute for Advanced Study in Princeton and a CITA fellow in Toronto. My primary interests include planet formation, extra-solar planets and accretion disc physics.

The discovery of extra-solar planets (exoplanets) has been a staggering advance in astronomy in the last two decades. We have now know that the diversity of planetary systems is far my diverse than we could have even dreamed about. My current interests are understanding how close-in super-earth/mini-neptunes formed and evolve. The origin of these planets which orbit their stars with periods from hours to several months is one of the most interesting puzzles to have arisen from NASA's Kepler mission. The fact that these planets reside so close to their stars also means their atmospheres are subject to intense irradiation, orders of magnitude above what our solar system planets experience. This irradiation drives vigorous atmospheric escape, "evaporating" planets over there long lifetime. By understanding how exoplanet atmosphere's escape we can build a picture of what the planets looked like in the past, gaining insights into how they formed. 

At the earliest phases of the planet formation process, forming planets are embedded in a thin rotating gas disc which surrounds the young star. This planet-forming disc (or protoplanetary disc) provides the environment in which planets grow and migrate. In the last few years we have been able to take images of these discs at unprecedented resolution, resolving scales smaller than the size of the Earth's orbit. These images have revealed a smorgasbord of structures, which may or may not be linked to forming planets residing in these discs. A complete understanding of what creates these structures is missing and linking them to the properties of planets remains elusive. By using a combination of analytic theory to study hydrodynamic instabilities and simulations I hope to build a picture of how these structures we see in discs relate to and to not planet formation. We are just seeing the tip of the iceberg with these new images. The community has only studied a small fraction of the nearby protoplanetary discs, over the next 5 years the number will grow considerably. 



Damasso M, Rodrigues J, Castro-González A, et al., 2023, A compact multi-planet system transiting HIP 29442 (TOI-469) discovered by TESS and ESPRESSO. Radial velocities lead to the detection of transits with low signal-to-noise ratio, Astronomy and Astrophysics: a European Journal, Vol:679, ISSN:0004-6361

Rab C, Weber ML, Picogna G, et al., 2023, High-resolution [O i] line spectral mapping of TW Hya consistent with X-ray-driven photoevaporation, Letters of the Astrophysical Journal, Vol:955, ISSN:2041-8205

Nayakshin S, Owen JE, Elbakyan V, 2023, Extreme evaporation of planets in hot thermally unstable protoplanetary discs: the case of FU Ori, Monthly Notices of the Royal Astronomical Society, Vol:523, ISSN:0035-8711, Pages:385-403

Kotorashvili K, Blackman EG, Owen JE, 2023, Why the observed spin evolution of older-than-solar-like stars might not require a dynamo mode change, Monthly Notices of the Royal Astronomical Society, Vol:522, ISSN:0035-8711, Pages:1583-1590

Rogers JGG, Schlichting HEE, Owen JEE, 2023, Conclusive evidence for a population of water worlds around M dwarfs remains elusive, Letters of the Astrophysical Journal, Vol:947, ISSN:2041-8205

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