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.. 

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  

Electron Bulk Heating At Saturn’s Magnetopause

By Matthew Cheng (University College London)

The magnetopause (MP) boundary is formed by the solar wind plasma flow interacting with a planetary magnetic field. Magnetic reconnection is an important process at this boundary as it energises plasma via release of magnetic energy. This process can lead to an “open” magnetosphere allowing solar wind and magnetosheath particles to directly enter the magnetosphere. At Saturn, the nature of MP reconnection remains unclear. Masters et al. (2012) hypothesised that viable reconnection under a large difference in plasma β across the MP also requires a high magnetic shear (i.e. magnetic fields either side of the boundary close to anti-parallel).

We used electron bulk heating (i.e. the scalar temperature change) at magnetopause crossings to test hypotheses about reconnection at open magnetopause locations, and the influence of magnetic shear and plasma β. The bulk temperature was determined using three different methods, related to properties of the observed energy distribution (including methods from Lewis et al. 2008). We compared the observed heating of magnetosheath electrons with the prediction based on reconnection, using the semi-empirical relationship proposed by Phan et al. (2013) which relates the degree of bulk electron heating to the inflow Alfven speed. Figure 1 shows that Δβ-magnetic shear parameter space discriminates well between events with evidence of energisation (right) and those without (left). Based on the magnetic shear measured locally by the spacecraft either side of the MP, we find 81% of events with no energisation were situated in the ‘reconnection suppressed’ regime, and up to 68% of events with energization lay in the ‘reconnection possible’ regime. These findings support the hypotheses that magnetic shear and plasma β play a role in the viability of magnetic reconnection.

Plots showing magnetic shear as a function of delta-beta, showing where events lie in this parameter space. Regions where reconnection is possible and reconnection is suppressed are marked. Two cases are shown: with and without energisation. The plots show the points lying in the suppressed reconnection when there is not energisation. More points lie in the possible reconnection region when there is energisation.

Figure 1. Assessment of diamagnetic suppression of reconnection, overlaid with electron heating ΔTe. The left and right panels show events without and with evidence of energization respectively.

Please see the paper for full details:

Cheng, I., Achilleos, N., Masters, A., Lewis, G., Kane, M., & Guio, P. (2021). Electron Bulk Heating at Saturn’s Magnetopause. Journal of Geophysical Research: Space Physics, 126, e2020JA028800. https://doi.org/10.1029/2020JA028800

Comparing electron precipitation fluxes calculated from pitch angle diffusion coefficients to LEO satellite observations

By Jade Reidy (British Antarctic Survey)

Trapped radiation belt particles can be pitch angle scattered into the loss cone by resonant wave-particle interactions and atmospheric collisions. This high-energy electron input into our atmosphere can affect the atmospheric chemistry and is a significant loss mechanism of particles from the radiation belts, which themselves pose a threat to satellites. Reidy et al (2021) calculates the precipitating flux that would be measured inside the field of view of an electron detector on board a low earth orbiting satellite (POES) using wave particle theory and compares to in-situ data. These calculations depend on diffusion coefficients for whistler mode chorus waves, plasmaspheric hiss waves and atmospheric collisions. The diffusion coefficients used in Reidy et al (2021) were derived for use in the British Antarctic Survey Radiation Belt Model (BAS-RBM). The analysis presented in this paper is a direct test of the how well the diffusion coefficients used in the BAS‐RBM are able to quantify the precipitating flux and therefore a first step toward testing the loss due to precipitation within the BAS‐RBM itself.

Figure 1 shows a global plot of the linear correlation between the calculated precipitating flux and that measured by the POES T0 >30 keV electron channel between 26–30 March 2013. Our results show the best correlation on the dawnside for L* > 5; this agreement is consistent with chorus waves being the dominant scattering mechanism in this MLT and L-shell zone, suggesting that chorus-driven scattering is well represented in the BAS-RBM. However, we consistently underestimate the precipitating flux on the duskside, suggesting we are likely missing some diffusion here; potential causes of this underestimate are discussed in the paper. Reidy et al (2021) also demonstrates the potential of using wave particle theory to reconstruct the total precipitating flux over the entire loss cone, some of which is missed by the POES detector due to its limited field of view, finding that the total precipitating flux can exceed that measured by POES by a factor of 10.

A figure showing the correlation between calculated and precipitating flux as a function of space.

Figure 1: Linear correlation coefficient between calculated and measured precipitating flux in bins of 3 hour MLT and 0.5 L*, where noon is to the top and dawn to the right. The correlation is only shown where the confidence level is over 95%.

Please see the paper for full details:

Reidy, J. A., Horne, R. B., Glauert, S. A., Clilverd, M. A., Meredith, N. P., Woodfield, E. E., et al. (2021). Comparing electron precipitation fluxes calculated from pitch angle diffusion coefficients to LEO satellite observations. Journal of Geophysical Research: Space Physics, 126, e2020JA028410. https://doi.org/10.1029/2020JA028410

Simultaneous Observation of an Auroral Dawn Storm with the Hubble Space Telescope and Juno

By Ben Swithenbank-Harris (University of Leicester)

Jupiter’s dawn storms are bright enhancements of the dawn flank of the main auroral emission, and produce the most powerful auroral events in the Solar System. These events have been observed numerous times with the Hubble Space Telescope (HST), and more recently by the Juno spacecraft, but their exact origins and related magnetospheric dynamics are not fully understood. For example, although consistent observations of this phenomena near local dawn suggested a relationship with the impinging solar wind, previous studies have shown no correlation between storm occurrence and solar wind conditions. Additionally, prior to the arrival of the Juno spacecraft at Jupiter in July 2016, auroral observations of dawn storms had not been supported by magnetospheric data from spacecraft in the dawn magnetosphere.

In this work, we present the first simultaneous magnetospheric in situ and auroral observations of the onset of a dawn storm. Magnetometer readings reveal brief reversals in the azimuthal magnetic field and decreases in the radial and total field magnitudes around the time of storm onset (Figure 1a-d). Furthermore, concurrent JADE (Figure 1e-h) and JEDI (Figure 1k-n) particle measurements reveal an increase in high energy particle populations and acceleration of magnetospheric protons towards corotational speeds, as well as long-lived hot plasma populations which persist in the outer magnetosphere beyond the expected lifetime of the enhanced auroral emissions. Ultimately, we associate this dawn storm with significant plasma heating and acceleration following reconnection at earlier local times.

Multi-panel plot showing time series of Juno observations.

Figure 1: Overview of the Juno in situ data, showing (1a-d) the radial, north-south, azimuthal and total magnetic field strength (nT) in cylindrical polar coordinates, (1e-h) the JADE ion time-of-flight energy spectra, electron and proton temperatures (K), number densities (cm-3) and proton azimuthal velocities (km s-1), (1i-j) Waves high frequency and electric field continuum emissions, (1k-n) JEDI particle spectra showing the total particle and proton energies (k-l) and the proton and heavy ion pitch angle distributions (m-n), (1o) and the expected spacecraft distance from the centre of the current sheet (RJ), calculated using the method of Khurana (1992). The light grey shaded regions show the times of HST observations, with the dawn storm interval denoted by the yellow shaded region. The darker grey shading denotes a magnetopause crossing, and the three dotted vertical lines mark the times of several successive reversals in the azimuthal magnetic field.

Please see the paper for full details:

Swithenbank‐Harris, B.G., Nichols, J.D., Allegrini, F., Bagenal, F., Bonfond, B., Bunce, E.J., et al. (2021). Simultaneous Observation of an Auroral Dawn Storm with the Hubble Space Telescope and Juno. Journal of Geophysical Research: Space Physics, 126, e2020JA028717. https://doi.org/10.1029/2020JA028717