Hi all,

Thanks to everyone who compared solar storms in ‘Protect our Planet from Solar Storms’ – we now have results to share with you!

We have used your comparisons to rank 1100 solar storms in order of how complicated, or complex they appeared.

Figure 1 shows three solar storms from the ranking. The left-hand image is a less complex storm, the middle image is an average storm, and the right-hand storm is a highly complex storm.

Figure 1: Three solar storms from across the complexity ranking.

The Sun has an ~11-year solar cycle, during which the number of sunspots (and solar storms) rises and falls. This can be seen in the bottom panel of Figure 2.

The top panel of Figure 2 shows the complexity of all 1100 solar storms plotted against the time the storm erupted from the Sun, for each of the two STEREO spacecraft. We have over-plotted yearly means, which clearly show that the average complexity of solar storms follows the sunspot cycle!

Figure 2: Top panel: complexity of solar storms over time, bottom panel: daily sunspot number.

Now we have established this, we are launching a new phase of the project – please help us compare solar storms with brightness adjusted images!

As usual, feel free to question us via the project Talk page!

Best wishes,

The Solar Stormwatch II team

Thank you very much for all your help with our solar storm research over the past year – we’ve made some good progress, thanks to you!

Some of you might have seen our project ‘Protect our Planet from Solar Storms’, which we launched back in May with the Science Museum. Here citizen scientists compared images of two solar storms, and decided which was the most complex or complicated solar storm.

Image: Screenshot of Zooniverse project ‘Protect our Planet from Solar Storms’

We have started to analyse the data from this project, and now have some interesting results, which we will share with you in the coming months (once we get them published!).

In the meantime, we would like your help…

We have used your comparisons to create a ranking of 1100 solar storms in order of complexity (see animation below). This clearly shows the characteristics of the storms seen in these images changing as they become more complex.

Animation: Subset of the solar storms which have been ranked, showing increasing complexity.

However, we have yet to work out precisely which characteristics make a solar storm “complex”. So to help us with this, we would like you to tell us what you saw as a complex solar storm; what did you look for when you decided which was the most complicated storm?

Please tell us what you see as a complex solar storm on the talk page or using this form!

Thanks again for all your help!

Hi all, thanks for all your hard work tracing storm fronts so far; we’re now over a third of the way there!

Back in September, I wrote a blog post explaining why we wanted your help with Solar Stormwatch II. Since then I’ve been using the data from Solar Stormwatch II to look at how solar storm fronts change shape and distort as they travel through the heliospheric imager field of view.

In this blog post, I explain how we combine all the storms fronts that you trace into a single consensus storm front (or two) in each image, allowing the fronts of a solar storm to be studied over the whole field of view.

Differenced images of solar storms are uploaded to Solar Stormwatch II. This image shows a solar storm from May 2010, and all the images in this post are of this same storm.

Every image of a solar storm is shown to 30 people, who each draw around the outermost and brightest fronts they see in each image. Each colour represents a different front drawing.

The points from the 30 front drawings are split into two groups. We use the coordinates of the outer front in the previous image to determine which points are likely to represent the same front. These points are shown in red, and the remaining points are shown in blue.

We first look at the red points as shown in the previous step. To combine all the points and find a consensus storm front profile, we use a process called kernel density estimation. This finds the areas of the image with the highest density of points; these areas are shown in black. The largest area corresponds to the storm front.

Using the storm front area found in the previous step, we can find the expected location of the storm front (solid red line) and calculate uncertainties from the distribution of the points in this area (dashed red lines).

The previous two steps are repeated for the second set of points shown in blue. There isn’t a second front in every image, so this stage involves a check to see whether the blue points show a storm front or not.

This method is repeated for every image of a solar storm, allowing us to examine how the shape of the storm changes throughout the field of view. The animation shows the outermost storm fronts found for this solar storm as it travels away from the Sun.

I’ve been looking at several solar storms to see how the shape of the storm front compares to the solar wind speed across the front; I hope to update you on this soon!

In the meantime, we are grateful for your continued support tracing storm fronts, and if you want to help with even more space weather research, we (the Solar Stormwatch II team) have recently released another project in collaboration with the Science Museum, see here: Protect our Planet from Solar Storms.

by Lee T. Macdonald

A solar explosion that took place in 1859, known today as the ‘Carrington Event’, is used as a benchmark for a catastrophic ‘space weather’ incident that could have serious consequences for today’s mobile phone, internet and satellite communications and also for the world’s electricity supplies. Space weather events are one of the potential catastrophes on the British government’s National Risk Register of Civil Emergencies. Funding is currently being sought for a British space-based observatory called Carrington-L5, whose purpose is to continuously monitor the Sun’s emissions and provide five-day warnings of solar storms that could damage terrestrial communications.

Who was Carrington? Also, what exactly happened in the ‘Carrington event’ of 1859?

For some years around the mid-nineteenth century, Richard Christopher Carrington (1826-1875) was one of Britain’s leading astronomers. Born into a wealthy brewing family, Carrington studied mathematics at the University of Cambridge, where he graduated in 1847. Attaining high marks in the Cambridge ‘Mathematical Tripos’ exam was in those days the standard qualification for anyone who aspired to one of the relatively few paid posts in British astronomy.

After graduation, Carrington worked for several years at the Durham University observatory. In 1852 he resigned and moved to Redhill, Surrey, where he worked as an independent astronomer, setting up a private observatory with the profits from his father’s brewing firm. Carrington initially became famous for compiling a catalogue of stars near the north celestial pole, which won him the Gold Medal of the Royal Astronomical Society.

Not long after moving to Redhill, Carrington also began systematically observing the Sun and its ever-changing dark spots. Little was then known about what sunspots were. But since the 1830s, scientists had been seriously studying the Earth’s magnetic field. Then, in 1843, the German astronomer Heinrich Schwabe discovered that the number of sunspots visible rose and fell in a cycle of about ten years. Seven years later, Edward Sabine, a British army officer who was in charge of Britain’s geomagnetic observations, found a ten-year cycle in the frequency and intensity of magnetic variations. He then noticed that this cycle coincided exactly with Schwabe’s sunspot cycle. This seemed to confirm the existence of some kind of link between sunspots and terrestrial magnetism, and led to an increased interest among astronomers in observing the Sun.

It was against this background that Carrington began regularly observing the Sun. He used a 4 ½-inch equatorially-mounted refracting telescope to project an image of the Sun onto a large sheet of glass painted white, from which he made drawings of the sunspots and measured their positions. After several years of careful observation, Carrington discovered what later came to be known as ‘Spörer’s Law’: a gradual decline in the average solar latitude of sunspots as the solar cycle progressed. He also discovered that sunspots close to the solar equator rotate around the Sun faster than those at higher latitudes. In addition, he established a system of reckoning the Sun’s rotation that is still used today.

On the morning of 1 September 1859, Carrington was making his usual daily observation of the Sun. For some days past, a large and unusually complex sunspot group had dominated the solar disc. According to his own account, at 11:18am on 1 September, Carrington noticed two dots of intensely bright light appear in the big sunspot group. These bright dots gradually faded, and disappeared altogether five minutes after Carrington first noticed them. But while they remained visible, Carrington observed them move across a large part of the sunspot group – around 35,000 miles, according to his measurements.

By good luck, another British astronomer, Richard Hodgson, was also observing the Sun at the same time that morning, and independently witnessed the same phenomenon. Both presented their results at the November 1859 meeting of the Royal Astronomical Society. By then, Carrington had learned something more exciting. One or two days after 1 September, Carrington visited King George III’s former observatory in Richmond, which was by then known as Kew Observatory and which Sabine had begun using as a principal station for his geomagnetic work. Eighteen months earlier, Sabine and others had established at Kew a programme of regular photographs of the Sun’s disc, in combination with a continuous record of the terrestrial magnetic field using a set of self-recording magnetometers.

See Carrington’s 1859 report of his observation in the Monthly Notices of the Royal Astronomical Society

As it happened, Kew Observatory had not obtained any pictures of the Sun on the day of Carrington and Hodgson’s phenomenon. However, when Carrington and an assistant at the observatory, Charles Chambers, examined the magnetometer data, they found a pronounced jump in the traces produced by the magnetometers at 11:20am on 1 September, two minutes after Carrington had first noticed the bright spots. Moreover, on the night of 2 September, a great display of the aurora was visible over much of the globe. In the northern hemisphere, it was seen as far south as Cuba. The magnetometers at Kew and elsewhere recorded wild variations. Over the same period, operators using the recently-invented electric telegraph had problems with sending and receiving messages. The event came to be known as a ‘magnetic storm’.

Ever the careful scientist, Carrington noted the coincidence in time between the magnetic disturbances and his observation of the strange phenomenon on the Sun, but expressed diffidence about making any connections between the two, quoting the old saying, ‘one swallow does not make a summer’.

What Carrington saw on 1 September 1859 is now called a ‘white-light flare’. A solar flare occurs in an active region whose magnetic field becomes so twisted and complex that it effectively ‘short-circuits’, causing a huge release of energy. Most flares require special filters to be seen from Earth, but a few are so intense that they can be seen in ordinary, ‘white’ light. Carrington and Hodgson were lucky enough to observe an exceptionally powerful flare many years before special equipment was invented for observing these phenomena.

The ‘jump’ recorded by the magnetometers at the same time as Carrington’s flare is now recognised to have been a ‘geomagnetic crochet’, caused by ultraviolet rays from the flare ionizing the Earth’s upper atmosphere and thus exciting the terrestrial magnetic field. The longer-term magnetic variations and aurorae were caused by a great wave of subatomic particles released from the Sun by the flare, now known as a ‘coronal mass ejection’ (CME). Yet the aurorae did not occur until the evening of 2 September, about eighteen hours after Carrington’s flare, because that is how long it took the particles to travel from the Sun to the Earth. The geomagnetic crotchet occurred at the same time as Carrington saw the flare, because both the visible light seen by Carrington and the ultra-violet rays that caused the magnetic jump were just different forms of electromagnetic radiation, travelling at the speed of light.

The Carrington Event had great contemporary importance in Victorian science. It heightened an already increasing interest in Sun-Earth connections, and helped stimulate astronomers to look for further connections, including possible solar influences on terrestrial weather that might be used to predict droughts and associated famines.

However, the event’s significance for the twenty-first century is that it was one of the most powerful solar explosions ever recorded. The largest flare of modern times occurred on 4 November 2003. This originated in a complex sunspot group similar to the one that caused the Carrington flare. Across much of its passage across the Sun the previous two weeks, the 2003 sunspot had been unleashing many flares and CMEs. These had not only sparked powerful aurorae: the magnetic effects caused damage to communications satellites and some airlines flying near the arctic regions had to be re-routed, due to dangerous radiation levels in the upper atmosphere. By 4 November, when the most powerful flare took place, the parent sunspot was moving off the Sun’s visible disc and the resulting CME was directed at 90 degrees to the Earth. Had it travelled directly towards the Earth, its consequences for communications systems and transport could have been devastating.

Research by scientists into the recorded magnetic effects of the 1859 Carrington flare suggests that it might well have been as powerful as the 2003 one. The explosion’s effects on the Victorian electric telegraph were as nothing to the consequences of a Carrington-type event for the communications and power supplies we rely on in the modern world. That is why the Carrington event forms a benchmark for a potentially disastrous modern-day space weather event – and why scientists and governments need to understand and monitor the Sun’s emissions, in preparation for another such event.

Thank you Stormwatchers for all your hard work drawing Storm Fronts! While you continue to help us improve space weather forecasts, here is an article on the history of space weather (which includes solar storms) written by Lee Macdonald, a science historian.

The Victorian origins of ‘space weather’

Lee Macdonald

Today we take it for granted that activity on the Sun causes colourful displays of the aurora (the ‘northern lights’ in the northern hemisphere; the ‘southern lights’ south of the equator) and, in extreme cases, power cuts and disruptions to satellite communications. We now know that the Sun triggers these phenomena through its magnetic field and the stream of subatomic particles it emits, called the ‘solar wind’ – which in turn affects Earth’s magnetic field. We call the state of the solar wind and magnetic activity in the solar system ‘space weather’. Aurorae do not just take place on Earth: they can occur on any planet that has both a magnetic field and an atmosphere. They have been photographed in the atmospheres of Jupiter, Saturn, Uranus and Neptune; more recently, spacecraft have imaged them in the skies of Mars.

We strongly associate pictures of aurorae on other planets, as well as terms like ‘space weather’ and ‘solar wind’, very much with the space age. However, the possibility of detecting aurorae on other planets – and, by implication, the existence of the Sun’s influence throughout the solar system – was first suggested by two British astronomers working in the mid-nineteenth century: Balfour Stewart (1828-1887) and Edward Sabine (1788-1883).

A correlation between aurorae and the Earth’s magnetic field had been known since the eighteenth century, when Anders Celsius (best known for the Celsius temperature scale) and Olof Hiorter noticed frequent and wild oscillations in the direction of magnetic north during an auroral display. In the 1830s, the astronomer and scientific polymath John Herschel (1792-1871) undertook a systematic study of sunspots while on a four-year observing expedition at the Cape of Good Hope in South Africa. In 1837, he noticed a peak in both sunspot and auroral activity and thought that it would be worth investigating whether a correlation between these two phenomena applied more generally. Six years later, German apothecary and astronomer Heinrich Schwabe discovered that the number of sunspots waxed and waned in a ten-year cycle. Then, in 1852, Sabine discovered a similar periodicity in the Earth’s magnetic field and noticed that it coincided exactly with Schwabe’s sunspot cycle. Herschel saw this discovery as confirmation of a link between sunspots and aurorae, and he now suggested that the ‘red clouds’ seen during a solar eclipse (now known as solar prominences) might be ‘reposing auroral masses’.

In response to Sabine’s discovery, the British Association for the Advancement of Science (BAAS) set up a solar telescope and a suite of magnetic instruments in the Association’s observatory at Kew, to further investigate this correlation. The solar telescope, known as the Kew ‘photoheliograph’, took pictures of the Sun every clear day so that sunspot activity could be compared with the magnetic readings. (See separate article and associated video on the ConSciCom web pages about Elizabeth Beckley’s role in solar photography at Kew: https://conscicom.org/2017/03/09/work-peculiarly-fitting-to-a-lady-elizabeth-beckley-and-the-early-years-of-solar-photography/)

In 1859, Balfour Stewart became superintendent of Kew Observatory. On 1 September that year, just two months after Stewart took up his post, the astronomers Richard Carrington and Richard Hodgson independently noticed a pair of bright lights appear above a large sunspot group, only to disappear a few minutes later. The timing of this explosion on the Sun, now known to have been a solar flare, coincided exactly with a jump in the traces produced by the magnetic instruments at Kew, and triggered Stewart’s interest in connections between solar activity and terrestrial magnetism.

In the early 1860s, Stewart and Sabine engaged in a lively correspondence on the nature of the newly-discovered Sun-Earth connections. In an August 1862 letter to Sabine, Stewart revived (without acknowledgement) Herschel’s 1852 assertion that the red clouds seen during eclipses might be aurorae on the Sun. In his reply to Stewart, Sabine took the speculation further, suggesting that the solar ‘aurorae’ triggered aurorae on Earth and wondered whether ‘all the planets participate in such appearances, though we may never attain to their observation’. Stewart, in turn, suggested a variety of observational evidence in favour of the red solar clouds being aurorae, including the fact that, as with sunspots, their greatest frequency coincided with periods of magnetic disturbance on Earth. As to Sabine’s suggestion that aurorae might occur on all the planets, Stewart wondered whether ‘perhaps Mr De La Rue could photograph one [of the planets] during an Aurora and ascertain this’.

Warren De La Rue (1815-1889) was then Britain’s leading pioneer of astronomical photography. He was instrumental in designing the Kew photoheliograph and was famous for his photographs of the Moon. Neither De La Rue’s nor anyone else’s photographic technology was then capable of photographing aurorae on other planets, but since 1979 spacecraft, including the Hubble Space Telescope, have photographed aurorae around the poles of Mars, Jupiter, Saturn, Uranus and Neptune (though scientists believe that Jupiter’s aurorae are due primarily to the interaction of the planet’s magnetic field with its volcanic satellite Io rather than the solar wind).

Figure 1. Aurora around the southern pole of Saturn, photographed with the Hubble Space Telescope. Image courtesy J. T. Trauger (Jet Propulsion Laboratory) and NASA.

Although Sabine and Stewart’s prediction had to wait more than a century to be vindicated, their logic was correct: something emanating from the Sun was influencing the entire solar system at the same time. We now know that this ‘solar wind’ is made up of charged subatomic particles that become tangled in planetary magnetic fields and cause their atmospheres to glow with auroral light. What, however, could these two visionaries have had in mind in 1862, when the smallest particle known to exist was the hydrogen atom?

Stewart’s work makes it clear that he believed solar emissions travelled through an invisible, all-pervading medium called the ‘ether’. In the mid-nineteenth century, with the rise of the wave theory of light, such a medium had become a popular way of explaining how light travelled through space. In the forefront of this ether physics was Stewart’s contemporary and fellow Scot, James Clerk Maxwell (1831-1879), whose electromagnetic theory described mathematically how light is an electrical and magnetic wave that propagates through this hypothetical ether. The ether was needed in the wave theory of light, because as a wave, light needed something to propagate through, just as sound requires air in which to travel.

Moreover Stewart, a staunch Christian believer, saw the ether as a convenient way of explaining the newly-discovered law of the conservation of energy without compromising the religious doctrine that the universe would one day come to an end. The ether provided a repository into which all the energy in the universe would eventually be dissipated, leaving the universe ultimately devoid of light and heat.

Stewart believed that as the planets changed their positions relative to the Sun, they moved through this ether and drew energy out of the Sun, causing magnetic effects that gave rise to sunspots and, as a consequence, aurorae. According to Stewart, the ether meant that the Sun and planets were tightly bound to one another, so that the motion of one body would have an effect on the others. Over the 1860s and 1870s, he used the solar results at Kew to develop some increasingly elaborate theories that attempted to correlate the positions of planets in their orbits with variations in sunspot activity. At the same time, he built experiments to find evidence for the ether, by measuring the heating of a disc spinning rapidly in a vacuum, eliminating friction with the air as a source of heat.

Link here:- https://www.nasa.gov/feature/goddard/comet-encke-a-solar-windsock-observed-by-nasa-s-stereo to a movie taken in 2007 by the STEREO A spacecraft, showing the tail of Comet Encke being buffeted by the solar wind – thought by Balfour Stewart and his contemporaries to be due to the ether. Image courtesy NASA/STEREO.

Both these approaches had inconclusive results. Stewart claimed to have detected heating in his spinning disc experiments, though modern scientists believe that this was due to the less-than-perfect vacuum attainable with the equipment of the mid-nineteenth century. After 1905, the ether theory gradually became discredited by Albert Einstein’s special theory of relativity. This painted a new picture of how light waves travel through space, dispensing with the notion of an ether.

However, the story of Balfour Stewart’s researches into solar-terrestrial physics has one ironic twist. In 1870, Stewart left Kew to become professor of ‘natural philosophy’ (now called physics) at Owens College in Manchester (now the University of Manchester). One of his students at Manchester was a young Joseph John (‘J. J.’) Thomson, who in 1897 would discover the electron – the first of the subatomic particles now known to make up the solar wind.

Hi! I’m Shannon. I first became involved with Stormwatch about a year ago, analysing the results of an original Solar Stormwatch activity; Track-it-back, and I’m now excited to be starting a PhD, studying space weather at the University of Reading, looking at solar storms.

Image: a solar storm or coronal mass ejection (NASA)

 So, what are solar storms, and why do we care about them?

Solar storms, also known as coronal mass ejections (CMEs), are huge clouds of solar material emitted from the Sun. These are part of the phenomenon we call ‘space weather’. If these reach the Earth, they can cause geomagnetic storms with severe consequences, such as damage to power transformers leading to wide-spread, long-term power outages. Other impacts include increased radiation exposure for astronauts and passengers on commercial flights, damage to satellites, and reduced accuracy of GPS systems.

To reduce the impacts of solar storms, we need to be able to accurately predict if and when a storm will hit the Earth. Therefore, we want to learn as much as we can about the nature and evolution of these storms.

During my PhD, I intend to work on improving solar storm forecasts, and I’m hoping that through Solar Stormwatch, we can create a dataset of tracked solar storms to help me achieve this. To this end, we have created a new Stormwatch activity; Storm Front. In Storm Front we would like you to help us track solar storms as they travel away from the Sun by tracing the outlines of storms in images from the wide-angle cameras on the STEREO spacecraft.

Image: the Storm Front interface

I will use the storm fronts that you trace to create a dataset which tracks solar storms as they move away from the Sun. The Sun constantly emits solar material out into space – the solar wind, and this dataset will allow me to study the interaction between the solar wind and these storms, and examine how the solar wind distorts the shape of solar storms. This will hopefully allow forecasts of solar storms with greater accuracy.

Image: visualisation of the solar wind (NASA)

Check back here for updates on the project, but in the meantime, feel free to ask us any questions you might have on the ‘Talk’ page… Thanks for reading, look forward to hearing from you!

Hello, I’m Luke and I work with Chris Scott (formerly Davis!) at the University of Reading as a postdoctoral research assistant. Recently I’ve been doing some work with the large amount of Trace-it data that has been generated over the last few years. We thought it was a good time to update everyone on the work we have been doing.

The short story is that we have turned the roughly 40000 time-elongation (t-e) profiles generated by Trace-it into a catalogue of CMEs seen by Heliospheric Imager (HI) instruments aboard STEREO-A (STA) and STEREO-B (STB). The Solar Stormwatch catalogue provides profiles of the CME fronts in the remarkable field-of-view (FOV) of the HI instruments. The HI FOV covers regions of the inner heliosphere not accessible to the coronagraph instruments that are more commonly used to build CME catalogues. Therefore the Solar Stormwatch catalogue should allow us to study the structure and dynamics of CME fronts in a way not previously possible using other presently available CME catalogues. This has been written up into a paper which is currently under review for publication in the journal Space Weather. So, first things first, thank you to everyone that has contributed to Solar Stormwatch. I think that we have produced a useful catalogue of CMEs, which will hopefully be of use to the wider space weather community – this wouldn’t have been possible without all of the contributors to Solar Stormwatch.

Let’s begin with a quick review of the raw data produced by Trace-it. Trace-it analysed J-maps made from HI1 and HI2 images, for both STA and STB, over 18 distinct position angles separated by 5 degrees, except for one position angle, which was centered on the ecliptic plane.

The J-maps covered a time span of January-2007 to February-2010. As of a few months ago, the Trace-it results consisted of database of 38171 t-e profiles, 22007 from STA and 16164 from STB, generated by 4599 Solar Stormwatch users.

If elongation angles and position angles are unfamiliar to anyone reading this, Figure 1 shows an image from HI1A, over which contours of constant position angle (in blue) and constant elongation angle (in red) have been overlaid, to make these coordinates clear.

Figure 1. An example of a differenced image from the HI1A camera, overlaid with contours of

constant PA (in blue) and constant elongation angle (in red). The elongation and PA contours

are in 5◦ increments. A CME is visible to the right of the image, between 5◦ and 10◦ elongation

and with maximum extent in PA between 65◦ and 135

To separate the t-e profiles into groups which represent individual CMEs we looked for periods when many t-e profiles were clustered in a short space of time. To do this, we counted how many t-e profiles began in a 7-hour window, for every hour covering the data set, and whenever the count of profiles was higher than a threshold of 22 counts we defined that as an event. This happens whenever lots of us have seen features over multiple position angles but at similar times. Figure 2 shows an example of this. Panel A) shows a STA J-map, at PA=110 degrees, overlaid with the t-e profiles generated by the Solar Stormwatchers as red dots, whilst the blue dots mark the earliest occurring point in each profile. In this instance, this position angle was tracked 11 times by 8 different Solar Stormwatchers. Panel B) shows the count of these profiles as a function of time, using the 7 hour sliding window. Note that this count is done over every position angle, whereas the J-map shows the t-e profiles at one position angle only. There is a well defined maximum in the count, which we use to define the onset of this event and identify the t-e profiles that describe it. The thresholds we picked are arbitrary but sensible, we could have used different ones and had similar results – for anyone interested in how we picked these numbers, we go into a bit more detail in the paper.

This gives us groups of t-e profiles for each CME – 113 from STA and 80 from STB. However, we had to do a bit of quality control, as it is not good enough just to have to t-e profiles that start at similar times – they could come from coincident but unrelated solar transients that are widely separated in position angle. So we used another set of rules to exclude any t-e profiles which look like they may belong to a different solar transient. This process is detailed more in the paper, but the result of it is that we have to discard 6 events that we are too unsure about, 3 each from STA and STB. This leaves us with 110 events from STA and 77 from STB.

At this point, we have defined sets of t-e profiles which we think robustly identify CMEs seen by the Solar Stormwatchers. The next step is to average these profiles along each position angle the event was observed. An example of this averaging is shown in Figure 3. The black dots show the t-e profiles generated by the Solar Stormwatchers for one event and along one PA, which includes 13 t-e profiles, generated by 9 different Solar Stormwatchers. The red-dots and red-lines show the average profile and the uncertainty in the average profile.

Figure 3. An example of an average t-e profile, for CME number 59 from STA, tracked along a PA of 110 degrees. The black dots show the individual t-e profiles and the red dots mark the consensus profile while the two red lines indicate the uncertainty in the mean time coordinates.

Now we can turn this around and overlay the average t-e profiles for each position angle back onto the original differenced images that made the J-maps they were tracked in. Figure 4 shows a movie of the evolution of an event through the HI1A field-of-view. The yellow lines mark the maximum extent of PAs that the J-maps used by Stormwatch cover, whilst the regions bounded in red mark the locations where the consensus profiles (like figure 3) suggest the CME front should be. The width of the bounded region arises from the uncertainty in the consensus profile at that position angle, so that wider regions mean we are less sure where the CME front is.

Figure 4. This movie shows a sequence of HI1A differenced images in which a CME can be seen to enter and propagate across the HI1A field-of-view. The yellow lines mark the outer limits of the position angles of the J-maps analysed by Trace-it. The red lines mark the location of the CME front, and are calculated from the averaged t-e profiles (see Figure 3) along each position angle the event was tracked.

We are in the process of making this CME catalogue available in an easily usable form so that the rest of the space weather community can get involved and hopefully start using it for some research. In November we will be taking this work to the European Space Weather Week conference in Belgium, to present this work to other researchers. In the meantime, we have some plans for some things we would like to do with the Solar Stormwatch catalogue, which we will update you with when there is more to say.

Thanks!