Which solar wind properties drive large-scale plasma waves in Earth’s magnetosphere?

Earth’s radiation belts are a hazardous environment to satellites, which are at risk from the charged particles trapped in near-Earth space. The behaviour of these particles is strongly determined by a spectrum of plasma waves. Ultra-low frequency (“ULF”) plasma waves are large-scale waves with periods on the order of minutes (frequency 1-15 mHz). While these are a fascinating component of near-Earth space, they’re particularly of interest to radiation belt modelling because of their role in the energisation and transportation of radiation belt electrons, so we want to know when and where to expect these waves.

Figure 1: Earth’s radiation belts contain particles (mostly electrons and protons) that are trapped by the Earth’s magnetic field. These need to be understood in order to protect satellites, many of which orbit in the heart of this environment. Missions such as the Van Allen probes (depicted here) provide a way to measure the particle population and the plasma waves which allow for particle acceleration, loss and transport.  Credit: JHU/APL, NASA

These plasma waves are predominantly driven by perturbations of the magnetopause – the boundary between the solar wind and the area dominated by Earth’s magnetic field. A simple example would be a constant tapping on the magnetopause by solar wind pulses – each tap causes a small compression and a magnetic field oscillation (they’re coupled together) which can propagate into the magnetosphere. (Figure 2)

Figure 2: Perturbations at the magnetopause can drive waves that propagate inwards. As the wave travels through the magnetosphere, these oscillations disturb Earth’s magnetic field. We can use the fact that these magnetic disturbances travel along dipole magnetic field lines to measure ULF waves at Earth’s surface.

But can we predict when and where these waves are likely to occur? Since the solar wind is the main driver of ULF waves, we want to be able to predict their effect on electrons from observations of the oncoming solar wind, while most existing models are based on the global geomagnetic activity index, Kp. There are many reasons why this is a poor parameter to base predictions on, the two most relevant being that firstly, it’s a 3-hr averaged index, so we don’t know the value of Kp at the current time (not great for either forecasting or nowcasting) and secondly, it’s so highly derived that it is not really suitable for any kind of statistical description of ULF waves (Murphy et al., 2016).

Previous studies have used a variety of methods to parameterise ULF wave power using solar wind properties (See review in Bentley et al., 2018). It turns out that a difficult part of this question is the solar wind itself. For starters, there is a lot more data describing some conditions than others, e.g. we have far more observations of the solar wind with a speed of 400 km s-1 than 600 km s-1 , and we must account for this if we don’t want our results to be skewed towards the situations where we have more data. But a more difficult problem is the tangled nature of the solar wind properties, which are highly interdependent. (Figure 3) This is partly due to the fact that the solar wind can come from different solar sources, and each one is likely to have a consistent set of properties which then occur at the same time. But also important are the multitude of interactions within the solar wind before it reaches Earth.

Figure 3: Establishing causal relationships is particularly difficult when looking at the solar wind as many properties are highly interdependent. If a quantity D correlates with B and C, is that because they both affect D? Here, only C affects D. But B will still correlate with D because B and C are interdependent. We want to identify only causally correlated parameters.

For example, fast solar wind is generally less dense than the slow solar wind, so speed vsw will anticorrelate with proton number density, Np. But when a region of fast solar wind catches up with some slow solar wind, we will end up with a compression region (Figure 4), so the onset of high speed solar wind will also be related to sudden dense regions and corresponding oscillations of the interplanetary magnetic field (as it folds up due to the compression). If on average we see increased ULF wave power in the magnetosphere when we see high solar wind speeds, is that then due to the speed or due to properties of density or the magnetic field that happen to occur at the same time? Other examples of interdependencies include turbulence, wave interactions and the composition in certain types of solar wind. Many solar wind properties correlate with the speed, because it’s quite a good proxy for all the different types of solar wind.

Figure 4: As fast solar wind catches up with slow solar wind, this creates a compression region ahead and a rarefaction region behind. This is one example of many solar wind interactions that make it difficult to separate the effect of different solar wind properties on the magnetosphere.

Unfortunately most of the existing techniques we might use to construct a parameterisation of ULF wave power on these solar wind properties aren’t appropriate – either they require unphysical assumptions about these interdependencies or they will be difficult to use to investigate the physics behind ULF wave occurrence.

Instead we opted for something simpler – systematically examine all solar wind parameters to find out which ones are causally correlated with ULF wave power. An example of this is shown in Figure 5: take two solar wind parameters to make a grid, and in each bin show the median observed ULF wave power. This allows us to see whether power increases with one parameter when a second is held constant, across different values. This accounts for the interdependence between a pair of parameters and so by systematically comparing many of these plots, we can identify which parameters are causally correlated to power, rather than just correlated to other parameters that affect the wave power. In the example here we can see that when the interplanetary magnetic field Bz component is above zero, ULF wave power increases only with increasing solar wind speed. However, when it’s below zero, ULF power increases with both speed and with more strongly negative Bz.

Figure 5: A two-parameter plot taken from Bentley et al., 2018. We bin the ULF power observed at one station (roughly corresponding to geostationary orbit) at one frequency (2.5mHz) and observe whether it increases with increases in solar wind speed vsw and/or the component Bz of the interplanetary magnetic field. Cut-throughs at constant speed and Bz are shown in (b) and (c).

While this method is very simple, it turns out to be surprisingly powerful – there’s clearly a threshold at Bz=0 that would be averaged over by other techniques, and it also turns out to be the change in proton number density δNp rather than the number density Np that’s causally correlated with power. We can speculate on what physical processes driving the ULF waves are represented by these parameters (see Bentley et al., 2018). It’s likely that the Bz threshold is due to different physical processes that occur when Bz <0, i.e. magnetic reconnection, which I briefly described in a previous blog post.

So by using a simple and systematic method to identify the properties of the solar wind that drive magnetospheric ULF waves, we can resolve three parameters: speed vsw, magnetic field component Bz and proton number density perturbations δNp. Having identified these three parameters opens up new opportunities to model magnetospheric ULF wave power and explore the physics – just when, where and how do we see these waves? And can we quantify how much these parameters contribute – does this change in different regions of the magnetosphere?

Like much of scientific research, answering this one question has opened many more avenues of study to understand these large-scale plasma waves and their role in the dynamics of Earth’s magnetosphere.


Murphy, K. R., I. R. Mann, I. J. Rae, D. G. Sibeck, and C. E. J. Watt (2016), Accurately characterizing the importance of wave‐particle interactions in radiation belt dynamics: The pitfalls of statistical wave representations, J. Geophys. Res. Space Physics, 121, 7895–7899, doi:10.1002/2016JA022618.

Pizzo, V. (1978), A three‐dimensional model of corotating streams in the solar wind, 1. Theoretical foundations, J. Geophys. Res., 83(A12), 5563–5572, doi:10.1029/JA083iA12p05563.

Bentley S.N., C.E.J. Watt, M.J Owens, and I.J. Rae (2018), ULF wave activity in the magnetosphere: resolving solar wind interdependencies to identify driving mechanisms, Journal of Geophysical Research, 123, doi:10.1002/2017JA024740.


The Solar Stormwatch Citizen Science Project

Coronal mass ejections (CMEs), also known as solar storms, are huge clouds of solar material, made up of plasma and magnetic field, emitted from the Sun. If these storms reach the Earth, they can cause geomagnetic storms with severe consequences, such as widespread long-term power-cuts (Canon et al., 2013). Therefore, it’s important to learn as much as we can about the nature and evolution of these storms, to accurately predict if and when they will hit the Earth, and how damaging they will be if they do.

Figure 1: A coronal mass ejection leaving the Sun (Credit: NASA)

For these reasons, the Solar Stormwatch project was created; a citizen science project where volunteers identify and track CMEs in remote-sensing images of space. The original project, jointly created by the Zooniverse and the Royal Observatory Greenwich, asked participants to complete six different activities, and proved very popular. More than 16,000 citizen scientists took part, resulting in seven scientific publications. Based on the success of this, a new version has been created, Solar Stormwatch II, to continue the effort to improve CME forecasts.

Figure 2: A screenshot of the Solar Stormwatch II interface (www.solarstormwatch.com)

In Solar Stormwatch II, volunteers complete an activity called ‘Storm Front’, characterising CMEs in images from the heliospheric imagers (HI) on board NASA’s twin STEREO spacecraft in orbit around the Sun. These imagers take wide-angle images looking from the Sun out into space, and CMEs propagate outwards from the Sun through the field of view. To make the motion of each storm clearer, we show volunteers running difference images, where each image has the previous image subtracted, so only the differences remain. Figure 4 shows example plain and running-difference images for comparison. Each participant is shown three consecutive running-difference images of a CME, and draws around the storm fronts they see in each image, as shown in Figure 5.

Figure 3: An illustration of the twin STEREO spacecraft in orbit around the Sun. (Credit: NASA)
Figure 4a: An example of a running-difference image of a CME. 4b: An example image taken by the heliospheric imagers.
Figure 5: An example set of three consecutive running-difference images of a CME, with storm fronts traced in red.

This is a subjective task, and we don’t expect that everyone will draw storm fronts in exactly the same place. Even two experts might disagree, and these differences could lead to big differences in results (De Koning, 2017). Therefore, we ask 30 people to draw around every storm front, which allows us to combine the observations, find the average location of the storm front, and calculate uncertainties from the distribution of the observations. This makes the dataset more objective and robust than if one expert had created it. Figure 6a shows the average storm fronts and uncertainties found using this method for an example image.

Figure 6a: A differenced HI image with the average storm fronts and uncertainties superimposed. 6b: The average storm fronts for one CME, changing from light to dark red over time, as the CME travels through the field of view.

Typically, researchers only track CME propagation along one slice of each image (Sheeley Jr. et al., 1999); Storm Front allows the whole CME front to be analysed in an unprecedented level of detail (Barnard et al., 2017). This extra detail will allow us to examine how the shape of the CME is distorted as it propagates through the HI field of view (see Figure 6b). Savani et al. (2010) looked at one CME and found that the solar wind, the constant stream of solar material which the Sun emits into space, could explain how the CME shape was distorted; we intend to use the dataset created though Solar Stormwatch II for a statistical comparison between CME distortions and solar wind conditions.

Figure 7: Sign up at www.solarstormwatch.com

At the time of writing, over 3,000 volunteers have taken part in Solar Stormwatch II, resulting in nearly 60,000 classifications. However, only 30% of the dataset has been completed, so we still need more volunteers. If you’d like to join the effort, please visit www.solarstormwatch.com and help finish the dataset!

· Barnard et al. 2017 doi:10.1002/2017SW001609
· Canon et al. 2013 doi:1/903496/96/9
· De Koning 2017 doi: 10.3847/1538-4357/aa7a09
· Savani et al. 2010 doi:10.1088/2041-8205/714/1/L128
· Sheeley Jr. et al. 1999 doi:10.1029/1999JA900308

Oceans in Weather and Climate Course 2018

email: r.frew@pgr.reading.ac.uk

Between the 11th-16th March myself and four other PhDs and post docs attended the Ocean in Weather and Climate (OiWC) course at the Met Office, Exeter. This NERC advanced training course was aimed at PhDs, postdocs and beyond. It provided a great opportunity to spend a week meeting other Oceanography researchers at varying stages of their career, and to expand your understanding of the oceans role in climate beyond the scope of your own work.

The week kicked off with an ice breaker where we had do some ‘Scientific speed dating’, chatting to other participants about: Where are you from? What do you work on? What is your main hobby? What is the biggest question in your field of research? This set the tone for a very interactive week full of interesting discussions between all attendees and speakers alike. Course participants were accommodated at The Globe Inn situated in Topsham, a cute village-sized town full of pastel-coloured houses, cosy pubs, art galleries, and beautiful riverside walks to stretch your legs in the evenings.

The days consisted of four 1.5 hour sessions, split up by caffeine and biscuit breaks to recharge before the next session.

Topics covered in the lecture-style talks included…

  • Dynamical Theory
  • Modelling the Ocean
  • Observations
  • Ocean-atmosphere coupling
  • Air-sea fluxes
  • High Resolution Ocean modelling in coupled forecast systems
  • The Meridional Overturning Circulation
  • The Southern Ocean in climate and climatic change
  • Climate variability on diurnal, seasonal, annual, inter-annual, decadal timescales
  • Climate extremes
  • Climate sensitivity, heat uptake and sea level.
A recurring figure of the week…. taken from Helene Hewitt’s talk on high resolution ocean modelling showing ocean surface currents from HadGEM3-based global coupled models at different resolutions (eddy resolving, eddy permitting and eddy parameterised).


All the talks were very interesting and were followed by some stimulating discussion. Each session provided an overview of each topic and an indication of the current research questions in each area at the moment.

In the post lunch session, there were group practical sessions. These explored observational ARGO float data and model output. The practicals, written in iPython notebooks, were designed to let us play with some data, giving us a series of questions to trigger group discussions to deepen understanding of topics covered that morning.

The course also included some ‘softer’ evening talks, giving research career advice in a more informal manner. Most evenings were spent exploring the lovely riverside walks and restaurants/pubs of Topsham. The final evening was spent all together at the Cosy Club in Exeter, rounding off a very interesting and enjoyable week!

Describe your research using the ten-hundred most common words…

Online comic “xkcd” set a trend for explaining complicated things using only the 1000 most common words when they created this schematic of Saturn-V.  They have subsequently published more on how microwaves, plate tectonics and your computer work, using the same style.

tornado safety
Useful safety advice from xkcd

So we thought we’d jump on the bandwagon in a recent PhD group meeting, and have a go at explaining our research topics using the ten-hundred most common words. You can have a go yourselves, and tweet us with it @SocialMetwork on Twitter. Enjoy!

The Role of the Asian Summer Monsoon in European Summer Climate Variability – Jonathan Beverley

I look at how heavy rain in in-dear in summer makes rain, sun, wind and other things happen in your-up. This happens by big waves high up in the sky moving around the world. We might be able to use this to make a long know-before better and to help people live longer and not lose money.

Contribution of near-infrared bands of greenhouse gases to radiative forcing – Rachael Byrom

I study how the sun’s light warms the sky. This happens when these really tiny things in the air that we can’t see eat the sun’s light which then makes the sky warmer. I use computers to look into how this happens, especially how exactly the really tiny things eat the sun’s light and how this leads to warming. By this I mean, if I add lots of the tiny things to a pretend computer sky, all over the world, then will the sky also warm over all of the world too and by how much will it warm? This might be interesting for people who lead the world so that they can see how much of the really tiny things we should be allowed to put into the sky.

Wind profile effects on gravity wave drag and their impact on the global atmospheric circulation – Holly Turner

I look at waves in the air over high places and how they slow down the wind. When the wind gets faster the higher up you go, it changes how it slows down. I want to use this to make computer wind pictures better.

The pulsatory nature of Bagana volcano, Papua New Guinea – Rebecca Couchman-Crook

To be a doctor, I look at a fire-breathing ground thing with smoke and rocks on a hot place surrounded by water. I look at space pictures to understand the relationships between the air that smells and fire-rock bits in the air, and other stuff. It’s a very angry fire-breathing ground thing and might kill the near-by humans

Surface fluxes, temperatures and boundary layer evolutions in the building grey zone in London – Beth Saunders

I work on numbers which come out of the Met Office’s computer world. These numbers are different to what is seen and felt in real life for cities. True numbers, seen in real life, help to say how hot cities are, and how different the hot city is to areas that aren’t cities, with trees and fields, because of the city’s people, cars and houses. Numbers saying how fast the wind goes, and the wind’s direction, change in cities because of all the areas with tall houses. Finding times where the computer world numbers are bad for cities will help to make the Met Office’s computer give numbers more like the true numbers.

Cloud electrification and lightning in the evolution of convective storms – Ben Courtier

To be a doctor, I look at sudden light shocks from angry water air that happens with noise in the sky and how the angry water air changes before the light shock happens. I do this in order to better guess when the sudden light shock happens.


Can scientists improve evidence transparency in policy making?

Email: a.w.bateson@pgr.reading.ac.uk

Twitter: @a_w_bateson

Politics. Science. They are two worlds apart. One is about trying to understand and reveal the true nature of the universe using empirical evidence. The other is more invested in constructing its own reality; cherry-picking evidence which conforms to the desired perception of the universe. Ok, so this is a gross simplification. Politicians have by no means an easy task. They are expected to make huge decisions on limited evidence and understanding. Meanwhile, whilst we all like the romantic idea that the science we do is empirical and non-biased, there are frequent examples (such as the perils of the impact factor or sexism in peer review) to counter this. We do understand, however, that evidence lies at the core of what we do. A good research paper will highlight what evidence has led to a conclusion or outcome, how that evidence was collected, and any uncertainties or limitations of the evidence. This is essential for transparency and reproducibility. What if we could introduce the same tools to politics?


For effective public scrutiny of policies, transparency in how evidence is used is essential. Credit for photo: Jamie Smith, Unsplash

In October 2017 I spent multiple hours reviewing government policy documents to assess just how well they were using evidence. I was contributing to the Sense about Science publication transparency of evidence: spot check. This document is the product of a collaboration in 2015 between Sense about Science, the Institute for Government and the Alliance for Useful Evidence wherein the evidence transparency framework was proposed. This framework aims to encourage government to be transparent in their use of evidence. In November 2016, Sense about Science published the original transparency of evidence report which was a trial use of this framework applied to a random selection of ‘publicly-available policy documents’. After feedback from the departments and participants involved, the framework has been refined to produce the spot check.

The review involved a team of young scientists, including me, each assessing how a subset of around 10 of these policies is using evidence. At this stage the quality of this evidence, or whether the policy has merit based on the presented evidence, was not considered. The priority is to assess the transparency in how evidence is being used to shape policy. We scored each policy in four key areas (with a score out of 3 given for each area):

  • Diagnosis: The policymakers should outline all they know about a particular issue including its causes, impacts and scale with supporting evidence. Any uncertainties or weaknesses in the evidence base should be highlighted.
  • Proposal: The policy should outline the chosen intervention with a clear statement of why this approach has been selected as well as any negatives. It should also be made clear why other approaches have not been used, and if the chosen intervention has not been fully decided on how the Government intends to make that decision. Once again the strengths and weaknesses of the evidence base should be acknowledged and discussed.
  • Implementation: If the method for implementing the proposal has not been made, what evidence will be used to make that decision? If it has, why has this approach been selected over alternatives, and what negatives exist? As previously, supporting evidence should be provided and assessed for its quality.
  • Testing and Evaluation: Will there be a pilot / trial of the policy and if not why not? How will the impacts and outcomes of the policy be assessed? The testing methods and criteria for success should be made clear, with an accompanying timetable.

For full details of this framework refer to Appendix 1 of the transparency of evidence: spot check publication. Whilst the framework is fairly explicit, it was nevertheless challenging as a reviewer to provide a fair assessment of each policy. The policies ranged in content from cyber-security to packaging waste; some were a few pages long, some closer to 100 pages; some were still at the consultation stage and others were ready to implement. Furthermore, sometimes values and pragmatism are as important in policy making as the available evidence. Policies based on such values can still be scored highly provided it is explicit and justified why these values have taken priority over any available contradictory evidence.

The findings discussed within the report are consistent with what I found when reviewing the policies. In particular, whilst inclusion of supporting evidence has improved since the original assessment, an approach of “info-dumping” seems to have been adopted whereby evidence is provided without being explicit about why it is relevant or it has been used. Similarly often references are cited without it being clear why. Many policies also failed to make the chain of reasoning from diagnosis to testing and evaluation of a policy clear. These complaints should not be unfamiliar to scientists! Finally, very few documents discussed how policies would be tested and evaluated. I am hoping by this point it should be clear why we as scientists can have a positive input. The same skills we use to produce high quality research and papers can be used to produce transparent and testable policies.

We have established why a scheme to engage young researchers in assessing and improving use of evidence in policy making has value, however perhaps you may still be wondering why we should care? Linking back to the theme of this blog, in the next few years we are going to see a raft of policies worldwide designed to combat climate change in response to the Paris Agreement. As the people providing the evidence, climate scientists will have a role in scrutinising these policies and ensuring they will achieve the predicted outcomes. For this to happen, transparency of evidence is essential. Furthermore, we all exist as citizens outside of our research, and as citizens we should want the ability to properly hold government and other policy makers accountable.

Nicaragua Diary: San Francisco Libre

This year the Department of Meteorology are participating and organising several events to raise money for the David Grimes Trust, a part of Reading San Francisco Libre Association. The David Grimes Trust was set-up after the passing away of Dr. David Grimes, a Reader in African Meteorology and an integral part of our department. His works include leading the TAMSAT group from the mid-1990s and supporting a new generation of African scientists. More details about David Grimes and the Reading San Francisco Libre can be found at http://www.met.reading.ac.uk/david/ and http://www.sanfranciscolibre.org/.

Events taking place include a departmental bake sale and a Meteorology Gatsby Ball. 20 members of the department are also running the Reading Half Marathon, and you can support them by donating at https://mydonate.bt.com/fundraisers/metdeptreadinghalf2018 .

This week’s blog post comes from Nick Byrne, a recent PhD graduate from the department, who’s written a two-day diary for us on his experiences in Nicaragua visiting San Francisco Libre.

Day 1

05:30 – Days in Nicaragua begin early! In San Francisco Libre (and in ‘el campo’ in general) everyone is up from as early as 04.00. Animals are tended to and tortillas are prepared from scratch, perhaps also along with a dish of ‘gallo pinto’ and some coffee.

School in San Francisco Libre

In the big towns life begins a little later. I’m staying in Esteli, a city in the northern highlands which is over 100km from SFL. My ‘expreso’ bus to Managua leaves at 06.45 and I only have time for a banana before I have to dash out the door.

08:00 – The bus drops me at the side of the highway near San Benito where I need to catch a regular bus to SFL. I get some travel advice from a friendly owner of a nearby ‘pulperia’, who tells me that the bus should arrive in about an hour. Regular buses in Nicaragua (or ‘chicken buses’ to tourists) are often retired American schoolbuses that have been redecorated in colourful ways. Anything and everything can be sold on them, and a couple of fresh Nicaraguan ‘picos’ can be very welcome if you missed breakfast.

11:00 – The bus arrives in SFL! I get off outside the house of a German NGO where 4 young volunteers are spending the year. I meet two of them, Flo and Clara, before being introduced to local resident and president of APREDEN (Association for the Recovery and Development of the Environment in Nicaragua), Jimmy Zamora. I give Jimmy a small gift of art supplies from Reading which he tells me will be very popular with the children of SFL. We chat briefly with the volunteers at the house and then hop on Jimmy’s bike for a ride to the local ‘comedor’ where we get some food and a delicious melon ‘fresco’.

12:00 – Over lunch we talk about some recent projects in SFL such as the plant nursery and beekeeping programs in ‘La Guayabita’, and the education programs in the library and the school. Between working on the various projects and coordinating activities with the German NGO, Jimmy is effectively on duty 24/7. Like many Nicaraguans, participating in his church community and singing in the choir at weekends is his release from the challenges that work brings. We also talk a little about his visit to England and his love of The Beatles, and we even manage a brief discussion on how residents perceive climate change in SFL.

13:00 – After lunch we spend the afternoon visiting various projects and activities in SFL. These include the harbour and canal network to the capital Managua, the semi-developed volcanic bath and spa facility for tourists, and also to the many communities surrounding the lake that were devastated by flooding after hurricane Mitch and from heavy rains in recent years. A recurrent theme is that even in difficult conditions, SFL is not lacking in creative solutions to the various problems that arise. The primary challenge is finding funding to get a project started. I’m told that the average daily wage for an agricultural worker in Nicaragua is around $5 a day, and so even a few dollars can have a huge impact on the daily quality of life.

Perhaps the project which Jimmy and colleagues are most proud of is the work at ‘La Guayabita’. This is a nursery for plants and trees as well as housing the location of the beekeeping project in SFL. There is a close connection between both of these projects as the bees help pollinate the nursery, while a diverse ecological system is crucial for a successful beekeeping program. When the beekeeping program initially started, all that the community had was the technical expertise of a few residents. Over time, and with the help of various fundraising efforts (including from the David Grimes Trust in Reading), the necessary materials were purchased and now the program is actually generating money for the community.

Plants at La Guayabita

The nursery itself has a striking visual impact as deforestation has been a problem in SFL over recent decades. Plants from the nursery are being used to redevelop recently bought land and this major project is currently in the early stages of development. Jimmy’s colleagues describe it best by calling ‘La Guayabita’ the lungs of SFL.

17:00 – Saturday evening is a chance to unwind a little. A karaoke competition has been organised in the central park and many children and families are present to enjoy the atmosphere. Jimmy is hosting the event and there is a wide range of genres. Songs range from recent hits such as ‘Chambea’ and ‘Casate Conmigo’ to crowdpleasers like ‘Me Gusta Tu Vieja’ (which I’m told is a Mexican joke about ‘your mum’!). Jimmy closes the event with a ranchera called ‘La Ley De La Vida’ before the prizes are presented. Everyone goes home around 21.00 after a very enjoyable evening.

Day 2

5:30 – I wake with the roosters and have breakfast with the German volunteers. We talk about their experience, from the initial shock of their first few weeks, to their determination to make the most of their year-long stay, to them now being an integral part of community life. They are well-known amongst the children of SFL, who like to chat and play whenever they pass the house. After breakfast I meet Jimmy again, and we go to visit the school and library education projects.

9:00 – The selection of books and educational materials in the library is impressive, and both the school and the library have been colourfully decorated with many art projects from the school children along with flowers and trees from the surrounding gardens. The library also contains materials for a weather station funded by the David Grimes Trust, along with English teaching materials donated by Caversham resident Russell Maddicks during a recent visit. Jimmy tells me that the project that they are currently working on in the library is to raise money for a sound system so that regular dance classes and audio lessons can be held. This is likely to cost a couple of hundred dollars and so it may be sometime before the project is finally completed.

11:00 – Suddenly it is 11.00 and we realise that it is time for me to leave. I say some quick goodbyes and then hop on Jimmy’s bike for the hour drive down the ’41’ from where I will catch my bus back to Esteli. I’m very grateful to Jimmy for taking the time to drive me personally, and this kindness is a typical example of what I have experienced from everyone in SFL during my short visit. It’s been a fantastic experience to meet a community I’ve read so much about since I came to Reading; after getting to know someone as committed to community work as Jimmy, it is much easier to understand how fundraising efforts in Reading can be translated into real community impacts thousands of miles away in SFL. I tell Jimmy that I hope to be able to visit again on my way home to Ireland in a couple of weeks, and he informs me that I should be just in time to sample some freshly harvested honey!

Thank you to Jimmy Zamora and volunteers for providing photos.

Baroclinic and Barotropic Annular Modes of Variability

Email: l.boljka@pgr.reading.ac.uk

Modes of variability are climatological features that have global effects on regional climate and weather. They are identified through spatial structures and the timeseries associated with them (so-called EOF/PC analysis, which finds the largest variability of a given atmospheric field). Examples of modes of variability include El Niño Southern Oscillation, Madden-Julian Oscillation, North Atlantic Oscillation, Annular modes, etc. The latter are named after the “annulus” (a region bounded by two concentric circles) as they occur in the Earth’s midlatitudes (a band of atmosphere bounded by the polar and tropical regions, Fig. 1), and are the most important modes of midlatitude variability, generally representing 20-30% of the variability in a field.

Figure 1: Southern Hemisphere midlatitudes (red concentric circles) as annulus, region where annular modes have the largest impacts. Source.

We know two types of annular modes: baroclinic (based on eddy kinetic energy, a proxy for eddy activity and an indicator of storm-track intensity) and barotropic (based on zonal mean zonal wind, representing the north-south shifts of the jet stream) (Fig. 2). The latter are usually referred to as Southern (SAM or Antarctic Oscillation) or Northern (NAM or Arctic Oscillation) Annular Mode (depending on the hemisphere), have generally quasi-barotropic (uniform) vertical structure, and impact the temperature variations, sea-ice distribution, and storm paths in both hemispheres with timescales of about 10 days. The former are referred to as BAM (baroclinic annular mode) and exhibit strong vertical structure associated with strong vertical wind shear (baroclinicity), and their impacts are yet to be determined (e.g. Thompson and Barnes 2014, Marshall et al. 2017). These two modes of variability are linked to the key processes of the midlatitude tropospheric dynamics that are involved in the growth (baroclinic processes) and decay (barotropic processes) of midlatitude storms. The growth stage of the midlatitude storms is conventionally associated with increase in eddy kinetic energy (EKE) and the decay stage with decrease in EKE.

Figure 2: Barotropic annular mode (right), based on zonal wind (contours), associated with eddy momentum flux (shading); Baroclinic annular mode (left), based on eddy kinetic energy (contours), associated with eddy heat flux (shading). Source: Thompson and Woodworth (2014).

However, recent observational studies (e.g. Thompson and Woodworth 2014) have suggested decoupling of baroclinic and barotropic components of atmospheric variability in the Southern Hemisphere (i.e. no correlation between the BAM and SAM) and a simpler formulation of the EKE budget that only depends on eddy heat fluxes and BAM (Thompson et al. 2017). Using cross-spectrum analysis, we empirically test the validity of the suggested relationship between EKE and heat flux at different timescales (Boljka et al. 2018). Two different relationships are identified in Fig. 3: 1) a regime where EKE and eddy heat flux relationship holds well (periods longer than 10 days; intermediate timescale); and 2) a regime where this relationship breaks down (periods shorter than 10 days; synoptic timescale). For the relationship to hold (by construction), the imaginary part of the cross-spectrum must follow the angular frequency line and the real part must be constant. This is only true at the intermediate timescales. Hence, the suggested decoupling of baroclinic and barotropic components found in Thompson and Woodworth (2014) only works at intermediate timescales. This is consistent with our theoretical model (Boljka and Shepherd 2018), which predicts decoupling under synoptic temporal and spatial averaging. At synoptic timescales, processes such as barotropic momentum fluxes (closely related to the latitudinal shifts in the jet stream) contribute to the variability in EKE. This is consistent with the dynamics of storms that occur on timescales shorter than 10 days (e.g. Simmons and Hoskins 1978). This is further discussed in Boljka et al. (2018).

Figure 3: Imaginary (black solid line) and Real (grey solid line) parts of cross-spectrum between EKE and eddy heat flux. Black dashed line shows the angular frequency (if the tested relationship holds, the imaginary part of cross-spectrum follows this line), the red line distinguishes between the two frequency regimes discussed in text. Source: Boljka et al. (2018).


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Boljka, L., T. G. Shepherd, and M. Blackburn, 2018: On the coupling between barotropic and baroclinic modes of extratropical atmospheric variability. J. Atmos. Sci., in review.

Marshall, G. J., D. W. J. Thompson, and M. R. van den Broeke, 2017: The signature of Southern Hemisphere atmospheric circulation patterns in Antarctic precipitation. Geophys. Res. Lett., 44, 11,580–11,589.

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Thompson, D. W. J., B. R. Crow, and E. A. Barnes, 2017: Intraseasonal periodicity in the Southern Hemisphere circulation on regional spatial scales. J. Atmos. Sci., 74, 865–877.

Thompson, D. W. J., and J. D. Woodworth, 2014: Barotropic and baroclinic annular variability in the Southern Hemisphere. J. Atmos. Sci., 71, 1480–1493.