Magnetosphere, Ionosphere and Solar-Terrestrial

Latest news

Winners of Rishbeth Prizes 2023

We are pleased to announce that following Spring MIST 2023 the Rishbeth Prizes this year are awarded to Sophie Maguire (University of Birmingham) and Rachel Black (University of Exeter).

Sophie wins the prize for the best MIST student talk which was entitled “Large-scale plasma structures and scintillation in the high-latitude ionosphere”. Rachel wins the best MIST poster prize, for a poster entitled “Investigating different methods of chorus wave identification within the radiation belts”. Congratulations to both Sophie and Rachel!

As prize winners, Sophie and Rachel will be invited to write articles for Astronomy & Geophysics, which we look forward to reading.

MIST Council extends their thanks to the University of Birmingham for hosting the Spring MIST meeting 2023, and to the Royal Astronomical Society for their generous and continued support of the Rishbeth Prizes.

Nominations for MIST Council

We are pleased to open nominations for MIST Council. There are two positions available (detailed below), and elected candidates would join Beatriz Sanchez-Cano, Jasmine Kaur Sandhu, Andy Smith, Maria-Theresia Walach, and Emma Woodfield on Council. The nomination deadline is Friday 26 May.

Council positions open for nomination

  • MIST Councillor - a three year term (2023 - 2026). Everyone is eligible.
  • MIST Student Representative - a one year term (2023 - 2024). Only PhD students are eligible. See below for further details.

About being on MIST Council

If you would like to find out more about being on Council and what it can involve, please feel free to email any of us (email contacts below) with any of your informal enquiries! You can also find out more about MIST activities at mist.ac.uk.

Rosie Hodnett (current MIST Student Representative) has summarised their experience on MIST Council below:
"I have really enjoyed being the PhD representative on the MIST council and would like to encourage other PhD students to nominate themselves for the position. Some of the activities that I have been involved in include leading the organisation of Autumn MIST, leading the online seminar series and I have had the opportunity to chair sessions at conferences. These are examples of what you could expect to take part in whilst being on MIST council, but the council will welcome any other ideas you have. If anyone has any questions, please email me at This email address is being protected from spambots. You need JavaScript enabled to view it..”

How to nominate

If you would like to stand for election or you are nominating someone else (with their agreement!) please email This email address is being protected from spambots. You need JavaScript enabled to view it. by Friday 26 May. If there is a surplus of nominations for a role, then an online vote will be carried out with the community. Please include the following details in the nomination:
  • Name
  • Position (Councillor/Student Rep.)
  • Nomination Statement (150 words max including a bit about the nominee and your reasons for nominating. This will be circulated to the community in the event of a vote.)
MIST Council contact details

Rosie Hodnett - This email address is being protected from spambots. You need JavaScript enabled to view it.
Mathew Owens - This email address is being protected from spambots. You need JavaScript enabled to view it.
Beatriz Sanchez-Cano - This email address is being protected from spambots. You need JavaScript enabled to view it.
Jasmine Kaur Sandhu - This email address is being protected from spambots. You need JavaScript enabled to view it.
Andy Smith - This email address is being protected from spambots. You need JavaScript enabled to view it.
Maria-Theresia Walach - This email address is being protected from spambots. You need JavaScript enabled to view it.
Emma Woodfield - This email address is being protected from spambots. You need JavaScript enabled to view it.
MIST Council email - This email address is being protected from spambots. You need JavaScript enabled to view it.

RAS Awards

The Royal Astronomical Society announced their award recipients last week, and MIST Council would like to congratulate all that received an award. In particular, we would like to highlight the following members of the MIST Community, whose work has been recognised:
  • Professor Nick Achilleos (University College London) - Chapman Medal
  • Dr Oliver Allanson (University of Birmingham) - Fowler Award
  • Dr Ravindra Desai (University of Warwick) - Winton Award & RAS Higher Education Award
  • Professor Marina Galand (Imperial College London) - James Dungey Lecture

New MIST Council 2021-

There have been some recent ingoings and outgoings at MIST Council - please see below our current composition!:

  • Oliver Allanson, Exeter (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2024 -- Chair
  • Beatriz Sánchez-Cano, Leicester (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2024
  • Mathew Owens, Reading (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2023
  • Jasmine Sandhu, Northumbria (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2023 -- Vice-Chair
  • Maria-Theresia Walach, Lancaster (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2022
  • Sarah Badman, Lancaster (This email address is being protected from spambots. You need JavaScript enabled to view it.), to 2022
    (co-opted in 2021 in lieu of outgoing councillor Greg Hunt)

Charter amendment and MIST Council elections open

Nominations for MIST Council open today and run through to 8 August 2021! Please feel free to put yourself forward for election – the voting will open shortly after the deadline and run through to the end of August. The positions available are:

  • 2 members of MIST Council
  • 1 student representative (pending the amendment below passing)

Please email nominations to This email address is being protected from spambots. You need JavaScript enabled to view it. by 8 August 2021. Thank you!

Charter amendment

We also move to amend the following articles of the MIST Charter as demonstrated below. Bold type indicates additions and struck text indicates deletions. Please respond to the email on the MIST mailing list before 8 August 2021 if you would like to object to the amendment; MIST Charter provides that it will pass if less than 10% of the mailing list opposes its passing. 

4.1  MIST council is the collective term for the officers of MIST and consists of six individuals and one student representative from the MIST community.

5.1 Members of MIST council serve terms of three years, except for the student representative who serves a term of one year.

5.2 Elections will be announced at the Spring MIST meeting and voting must begin within two months of the Spring MIST meeting. Two slots on MIST council will be open in a given normal election year, alongside the student representative.

5.10 Candidates for student representative must not have submitted their PhD thesis at the time that nominations close.

Nuggets of MIST science, summarising recent papers from the UK MIST community in a bitesize format.

If you would like to submit a nugget, please fill in the following form: https://forms.gle/Pn3mL73kHLn4VEZ66 and we will arrange a slot for you in the schedule. Nuggets should be 100–300 words long and include a figure/animation. Please get in touch!
If you have any issues with the form, please contact This email address is being protected from spambots. You need JavaScript enabled to view it.. 

Average Ionospheric Electric Field Morphologies During Geomagnetic Storm Phases

By Maria-Theresia Walach (Lancaster University)

Geomagnetic storms are a global electrodynamic phenomenon, during which the ring current is loaded with energy. The coupled magnetospheric/ionospheric system responds during a geomagnetic storm and the dynamics of the system can be monitored using measurements of the high-latitude ionosphere. Ordering data from the Super Dual Auroral Radar Network (SuperDARN) by geomagnetic storm phase, we produce convection maps for a geomagnetic storm, which allow us to discern changes that occur in association with the development of the storm phases. We utilize principal component analysis to identify and quantify the primary electric potential morphologies during geomagnetic storms. Along with information on the size of the patterns, the first six eigenvectors provide over ∼80% of the variability in the morphology, providing us with a robust analysis tool to quantify the main changes in the patterns. Studying the first six eigenvectors and their eigenvalues shows that the primary changes in the morphologies with respect to storm phase are the convection potential enhancing and the dayside throat rotating from pointing toward the early afternoon sector to being more sunward aligned during the main phase of the storm. We find that the ionospheric electric potential increases through the main phase and then decreases once the recovery phase begins. Furthermore, we find that a two‐cell convection pattern is dominant throughout and that the dusk cell is overall stronger than the dawn cell.

The figure shows the mean electrostatic potential, followed by the first six eigenvectors. These show the most common components that can be used to make up the ionospheric convection patterns during geomagnetic storms.

 Multipanel plot showing the first six components and mean electrostatic potential

Figure Caption: Ionospheric electric field component patterns showing the mean for geomagnetic storms (top left), followed by the patterns corresponding to the first six eigenvectors of the Principal Component Analysis. Each pattern is centered on the geomagnetic pole, with 12:00 magnetic local time pointing toward the top of the page, and dusk toward the left. Lines of geomagnetic latitudes are indicated from 40° to 90° by the dashed gray circles.

Animation showing convection patterns from SuperDARN data for geomagnetic storm main phase

Animation Caption: Average convection patterns from SuperDARN data for geomagnetic storm main phase

Please see the paper for full details: Walach, M.‐T.,  Grocott, A., &  Milan, S. E. (2021).  Average ionospheric electric field morphologies during geomagnetic storm phases. Journal of Geophysical Research: Space Physics,  126, e2020JA028512. https://doi.org/10.1029/2020JA028512

Network community structure of substorms using SuperMAG magnetometers

By Lauren Orr (University of Warwick)

Geomagnetic substorms are a global magnetospheric reconfiguration, during which energy is abruptly transported to the ionosphere. Central to this are the auroral electrojets, large-scale ionospheric currents that are part of a larger three-dimensional system, the substorm current wedge. Many, often conflicting, magnetospheric reconfiguration scenarios have been proposed to describe the substorm current wedge evolution and structure. We have used well-established network science techniques to analyze data from >100 ground-based magnetometers operated by the SuperMAG collaboration1.  We translated this data into a time-varying directed network, based on canonical cross-correlation of the vector magnetic field perturbations measured at each magnetometer pair2,3 and performed community detection on the network4. Communities are locally dense but globally sparse groups of connections in the network, identifying emerging coherent patterns in the current system as the substorm evolves. Analysis of 41 substorms exhibit robust structural change from many small, uncorrelated current systems before substorm onset, to a large spatially-extended coherent system, between 10-20 minutes after onset. We interpret this as strong indication that the auroral electrojet system during substorm expansions is inherently a large-scale phenomenon and is not solely due to many meso-scale wedgelets.

Panels showing the evolution of the community structure during substorms. The top panels show temporal variations in the communities and connections. Panels on the bottom show snapshots at times of interest.

Figure 1: The community structure of a substorm on the 16/03/1997. The abscissa of all panels is normalized time, where t'=0 is onset (dashed green line) and t'=30 (dashed purple line) is the time of maximum auroral bulge expansion. Panels 1-2 plots individual communities as circles where the size of the circle reflects the  number of connections within the community. The ordinate plots the mean MLT/MLAT of the community, and the color indicates the proportion of connections with each time lag, |τc|. The dashed lines overplotted are the edges of the auroral bulge (MLT) and the onset location (MLAT), found from auroral images. Panel 3 shows snapshots of the community structure at time points t’=0 (onset), t’=10 and t’=20, overplotted on maps provided by SuperMAG1. There is a clear shift from many, small uncorrelated communities before onset to one large correlated system half way through the expansion phase.

Please see the paper for full details:

Orr, L., Chapman, S.C., Gjerloev, J.W. et al. Network community structure of substorms using SuperMAG magnetometers. Nat Commun 12, 1842 (2021). https://doi.org/10.1038/s41467-021-22112-4

The Cushion Region and Dayside Magnetodisc Structure at Saturn

By Ned Staniland (Imperial College London)

The moons Enceladus and Io are internal plasma sources for the magnetospheres of Saturn and Jupiter, respectively. This, coupled with their rapid rotation rates (~10 h), radially stretches the magnetic field from a dipole to a magnetodisc. However, this structure can break down at large distances where the magnetic field can no longer contain the equatorial plasma. This quasi-dipolar layer between the current sheet outer edge and magnetopause is known as the “cushion region.” This has previously been observed at Jupiter, predominantly at dawn, but not at Saturn (Went et al., 2011). It is suggested to be populated by mass-depleted flux tubes following magnetotail reconnection.

We present the first evidence of a cushion region forming at Saturn. From the complete Cassini orbital dataset, only five examples are identified, showing this phenomenon to be rare, with four at local time dusk and one pre‐noon. The dusk cushion observed could be due to asymmetric heating of plasma in the Saturn system (Kaminker et al., 2017), as well as the changing magnetic field configuration through dusk where the field is less confined by the magnetopause, resulting in disc instabilities (Kivelson and Southwood, 2005).

These results highlight a key difference between the rotationally driven magnetospheres of Saturn and Jupiter. The rare cushion region examples found and evidence of patchy reconnection at Saturn (Delamere et al., 2015) compared to the persistent cushion region at Jupiter (Went et al., 2011) and statistical x-line across the Jovian tail (Vogt et al., 2010) shows that the mass transport and loss mechanisms differ between these systems. Whilst the Saturn system is often described as being between Jupiter and the Earth in terms of dynamics and structure, these results suggest that this is perhaps an oversimplified description.

An example of a cushion region is shown on the left, where the magnetic field observations indicate a transition from magnetodisc-like to quasi-dipolar. A schematic is included on the right where regions are colour-coded to indicate the expected locations of disc-like and dipolar-like fields.

Figure: The left plot shows an example of a cushion region at Saturn. The top panel shows magnetic field data. The second panel showing the relative contributions of the radial (green) and meridional (blue) components to the total field. The third panel shows the angle between the observed field and a dipole. For this example, the field is disc-like in the middle magnetosphere, but the structure breaks down in the outer magnetosphere (highlighted by the background colours). The right plot shows the average dayside magnetic field configuration. The field is more disc-like in the dawn sector whilst there is a quasi-dipolar region in the outer magnetosphere at dusk.

Please see the full paper for details:

Staniland, N. R., Dougherty, M. K., Masters, A., & Achilleos, N. (2021). The cushion region and dayside magnetodisc structure at Saturn. Geophysical Research Letters, 48, e2020GL091796. https://doi.org/10.1029/2020GL091796

Particle-In-Cell Simulations of the Cassini Spacecraft's Interaction with Saturn's Ionosphere during the Grand Finale

By Zeqi Zhang (Imperial College London)

Cassini's Grand Finale at Saturn was the first time the giant planet’s atmosphere had been sampled in-situ. The ionosphere, and indeed the Saturn system as a whole, provided a uniquely different environment compared to the terrestrial planets and also Jupiter, with populations of charged dust grains influencing the plasma dynamics.  When passing through Saturn’s ionosphere, Cassini observed an ionosphere dominated by ice and dust particles which continually rain inward from Saturn’s vast ring system and soak up free electrons, thus producing a dusty complex plasma.  Understanding how incident plasma currents charge a spacecraft relative to its surrounding environment is important for interpreting the surrounding plasma conditions and on-board plasma measurements.  In this article, we describe three dimensional Particle-In-Cell simulations of the Cassini spacecraft’s interaction with plasmas representative of Saturn's ionosphere during the Grand Finale.

The global simulations revealed complex interaction features such as a highly structured wake containing spacecraft-scale vortices and electron wings, a Langmuir wave analogue of Alfvén wings, which propagated at small angles to the magnetic field and upstream into the pristine plasma ahead of Cassini. The results explain how a large negatively charged plasma component combined with a large negative to positive ion mass ratio is able to drive the spacecraft to the observed positive potentials, a previously unexplained phenomenon observed during end-of-mission.  Despite the high electron depletions, the electron properties are found as a significant controlling factor for the spacecraft potential together with the magnetic field orientation which induces a potential gradient directed across Cassini's asymmetric body. This study reveals the global spacecraft interaction experienced by Cassini during the Grand Finale in a plasma environment dominated by a class of physics quite different to those considered in the classical view of spacecraft charging.

Figure shows a schematic of the Cassini spacecraft configuration in the simulation. Bottom panels show the electron, ion, and negative ion density spatial distributions.

Figure 1. The upper schematic shows the simulation configuration for Cassini during Grand Finale Rev 292 ingress at 2500 km Saturn altitude. The lower panels shows the electron (left-hand panel), ion (centre panel) and negative ion (right-hand panel) densities in the Y-Z plane through Cassini’s main body. The plasma wake is longer for the larger species and electron wing structures are visible in the electron density which propagate at small angles to the ambient magnetic field.

Please see the paper for full details:

Zhang, Z., Desai, R.T., Miyake, Y., Usui, H., Shebanits, O., (2021). Particle-In-Cell Simulations of the Cassini Spacecraft’s Interaction with Saturn’s Ionosphere during the Grand Finale. Monthly Notices of the Royal Astronomical Society, Volume 504, Issue 1, pp 964 - 973, https://doi.org/10.1093/mnras/stab750.

Magnetic topology of actively evolving and passively convecting structures in the turbulent solar wind

By Bogdan Hnat (University of Warwick)

Plasma turbulence and magnetic reconnection are fundamental to the transfer of energy and momentum between field and flow and are ubiquitous in laboratory and in space plasmas. Both processes generate coherent structures, which modify the energy transfer between different scales. The precise energy balance depends on the relative prevalence of specific topological structures, their rate of evolution and their ability to carry currents. 

Multi-point satellite observations of the high Mach number solar wind offer a unique opportunity to directly probe the properties of the coherent structures inherent in plasma turbulence and reconnection. We use topological invariants, nQ and nR, of the magnetic field gradient tensor to classify the topology of magnetic structures and to quantify the prevalence of actively evolving and passively advective structures and their contribution to Ohmic heating. We established that at least 25% of all samples are passively advected by the solar wind. The passive structures are dominated by plasmoids which carry a significant current density. Actively evolving structures are primarily quasi-2D flux ropes and 3D X-points. Magnetic configurations that actively evolve and carry a significant current, give a lower bound on the fraction of structures that can dissipate and heat the plasma to be ~35% of the total population. These are dominated by quasi-2D flux rope topology. Magnetic X-points constitute ~40% of all evolving structures, but only 1/5 of these carry a significant current.

 Probability density distributions are shown for passive structures on the left and active structures on the right. Shaded regions correspond to the topology of the structure.

Figure 1. Conditional joint probability density for (a) force-free magnetic field, passively advecting configurations; (b) actively evolving magnetic structures. Rectangular blue shaded region with nQ>0 corresponds to quasi-2D flux ropes (O-points). Green shaded region, nQ<0 corresponds to hyperbolic 3D X-point magnetic topologies and unshaded regions represent plasmoids. Magenta line separates regions of hyperbolic and elliptic magnetic field lines.

Please see the paper for full details:

Hnat, B., Chapman, S. C., & Watkins, N. W. (2021). Magnetic Topology of Actively Evolving and Passively Convecting Structures in the Turbulent Solar Wind, Phys. Rev. Lett. 126, 125101. https://doi.org/10.1103/PhysRevLett.126.125101