Supervisor
Dr Licia Ray
Description: Energetic electrons precipitating in Jupiter’s atmosphere generate some of the brightest aurora in the solar system, yet much is unknown the region in which they are accelerated. Recent data from the Juno mission has provided unprecedented knowledge of the high-latitude auroral region, yet data coverage is spatially and temporally limited by the single spacecraft. This PhD project aims to explore the behaviour of Jupiter’s acceleration region a 1D spatial, 2D phase space numerical Vlasov simulations.
The student will work with a time-dependent Vlasov code of Jupiter’s auroral acceleration region. They will investigate how the magnitude of field-aligned potential drops varies with initial density profiles, relating the outputs to Juno plasma data and auroral observations.
Students interested in this project should apply via the Lancaster University admissions system.
Funding is available on a competitive basis. To be considered for funding, submit your application by 31st January 2027.
Supervisor
Dr Licia Ray and/or Dr Sarah Badman
Description: Jupiter’s magnetosphere is the largest structure in our solar system, inflated by plasma from the moon Io. Iogenic plasma pervades the system and is coupled to Jupiter’s atmosphere via the planetary magnetic field. Recent modelling work has shown that the connection between these two regions is local time dependent, with plasma decoupled from the atmosphere at distances as small as 30 planetary radii on the nightside of the system. This PhD project will refine existing models and look for evidence of decoupling in Juno data.
The student will update the existing Jenkins et al. model to include magneto-sonic effects. They will also explore relevant Juno datasets, such as MAG and UVS, for signatures of decoupling such as magnetic field rotations and discontinuities and auroral intensity variations. We encourage interested students to be creative and consider how recent insight from Solar Orbiter and Parker Solar Probe discoveries can be adapted to the jovian system.
Students interested in this project should apply via the Lancaster University admissions system.
Funding is available on a competitive basis. To be considered for funding, submit your application by 31st January 2027.
Supervisor
Dr Maria Walch
Description
Earth’s magnetic environment, the magnetosphere is driven by the solar wind. This results in plasma convection around the whole of the magnetosphere and ionosphere, the atmosphere’s ionised top layer. We have observed this plasma convection in the ionosphere and magnetosphere for decades using spacecraft and ground-based systems like radars. We know that magnetic reconnection in the nightside magnetosphere results in auroral brightening. These brightenings are sometimes abrupt and fast growing, with specific auroral features that we group to call substorms (Akasofu, 1964). Substorms are one of the “magnetospheric modes”, the way the magnetosphere responds to solar wind driving (e.g. Pulkkinen et al., 2010). Substorms are the most frequently occurring magnetospheric mode and often precede a steady magnetospheric convection event (Walach et al., 2015). On the large, global scale, steady magnetospheric convection events and substorms start out the same but something happens during the evolution of a steady magnetospheric convection event that makes it different to substorms (Walach et al., 2017).
In recent years, we have deployed instrumentation that can measure magntosphere-ionosphere interactions at improved temporal and spatial cadence. This PhD project will aim to understand what these differences are using a large array of measurements from space and on the ground. You will investigate where in space and time differences between substorms and steady magnetospheric convection events occur using historical data. You will then investigate types of these events further and test your findings using newer, high resolution data. For this investigation, you will use new instrumentation that can measure meso-scale features (~10s-100s km scale sizes) in plasma convection, auroras and plasma densities.
A minimum of a 2:1 UK honours degree or equivalent is a requirement. It would be beneficial to have a mathematics/computer science background with an interest in space physics, or a physics background with an interest in programming. Prior programming knowledge is necessary, alongside a passion for research, and an inquisitive attitude.
Funding is available on a competitive basis. To be considered for funding, please submit your application by 31st January 2027.
Please contact Maria Walach (m.walach@lancater.ac.uk) for further information on the project.
References:
Akasofu, S. I. (1964). The development of the auroral substorm. Planetary and Space Science, 12(4), 273-282.
Pulkkinen, T. I., Palmroth, M., Koskinen, H. E., Laitinen, T. V., Goodrich, C. C., Merkin, V. G., & Lyon, J. G. (2010). Magnetospheric modes and solar wind energy coupling efficiency. Journal of Geophysical Research: Space Physics, 115(A3).
Walach, M. T., & Milan, S. E. (2015). Are steady magnetospheric convection events prolonged substorms?. Journal of Geophysical Research: Space Physics, 120(3), 1751-1758.
Walach, M. T., Milan, S. E., Murphy, K. R., Carter, J. A., Hubert, B. A., & Grocott, A. (2017). Comparative study of large‐scale auroral signatures of substorms, steady magnetospheric convection events, and sawtooth events. Journal of Geophysical Research: Space Physics, 122(6), 6357-6373.
