Service of rapid magnetic variations, an update

Rapid magnetic variations on Earth are intimately linked with solar activity and this is one of the main topics in Space Weather research. Modelling and forecasting these phenomena are vital in our technological society. The Service of Rapid Magnetic Variations provides lists of these remarkable magnetic events in a continuous way in what constitutes a long geophysical series that began in the late 19th century. Although the aim of this Service remains unchanged, methods have changed with time. Here, we describe the recent evolution of the Service, its database and the latest works carried out to improve the products delivered to the scientific society.


| INTRODUCTION
The geomagnetic field exhibits variations due to different phenomena. It has regular variations (the clearest example is the daily variation) and irregular variations (such as geomagnetic storms), considered in this sense as magnetic disturbances. Often, the latter have a sudden onset, so we call them rapid sudden commencements and they form part of what we call rapid magnetic variations. Other rapid variations that have aroused interest in the scientific community are geomagnetic bays -now known as sub-storms -, geomagnetic pulsations or solar flare effects. The study of rapid variations has been difficult, especially when it comes down to establishing a definition of the phenomenon and, overall, producing a physical explanation. Given this interest, many years ago, the IAGA (International Association of Geomagnetism and Aeronomy) created a specific committee for a deep study of these phenomena. This committee eventually became a stable service known as the Service of Rapid Magnetic Variations, SRMV, to be run by the Ebro Observatory. One of the main activities of this Service has been the detection of magnetic events such as Storm Sudden Commencements (SSC) and Solar Flare Effects (Sfe) and the preparation of lists that are published annually by the International Association of Geomagnetism and Aeronomy (IAGA). An introduction to this Service and its evolution can be found in Curto et al. (2007). That paper provided a complete explanation of the evolution of the Service, contextualizing it in the historical evolution of the scientific interest in RMV. As an example, the paper includes the reasons behind the change of nomenclature from Storm Sudden Commencements (SSC) to Sudden Commencements (SC) to help to generalize the concept. In the term SC, events with a sudden commencement followed or not by a geomagnetic storm are included. In this paper, we will refer to the phenomena as SC. Now, with our paper, we aim to show the latest updates of the SRMV database and the actions taken to improve the Service.

| Recognitions
With our nowadays technological-dependant society, there is an increased necessity to have a thorough understanding of the physical processes of the near-Earth environment, beyond that of theoretical studies. Most of the anthropogenic infrastructures, at Earth surface and at satellite altitude, may be affected by rapid magnetic variations inducing, respectively, geomagnetically induced currents (GIC) or surface charging. Implications for the socio-economic world are numerous. Threats, brought by rapid magnetic variations, are now considered by private companies as well as by governments, for transport of fluids, energy network, communications, satellite operations, etc.
In this context, many space weather studies take advantage of the SRMV historical data products in order to get benchmarks for their modelling, simulation and forecasting services. Society, as a whole, benefits from the availability of the SRMV lists that constitute continuous series of events. It has to be noted that, in recent scientific papers, authors acknowledge utility and high quality of SRMV data products (e.g. Camporeale et al., 2018;Saiz et al., 2021;Smith et al., 2019).
These lists are valued by the scientific community. On the Ebro web page (http://www.obseb re.es/en/rapid) alone, there are around 1,500 queries per year (1,000 of them from international institutions). But the number of downloads can achieve tens of thousands (Table 1).
IAGA has continued to support the Service and, in addition to other previous adopted resolutions (Curto et al., 2007), their latest resolutions have again backed the Ebro Observatory. By recognizing the utility of the work done, they have urged the observatory to continue with this task. Thus, at the Sopron (2009) and Montreal (2019) Scientific Assemblies, it was recommended that the lists of rapid variations and, in particular, those of the Sfe be continued, given their usefulness as a reference for many geophysical works (Appendix A in this paper).

| Staff
Ever since the creation of the first committee for rapid magnetic variations and its subsequent evolution to become the current service known as the SRMV, at the Ebro Observatory we have been committed to this endeavour by dedicating some of our staff to this task. Table 2 lists the scientific personnel devoted to the service.
Father Romañá initiated the Service of Rapid Magnetic Variations and led the service for 16 years. Following that, Father Cardús headed the service for three decades. More recently, Father/Doctor Alberca succeeded Father Cardús in 2000 as chair of the service and, finally, Dr. J.J. Curto took over this responsibility in 2018.
In addition to the day-to-day work in the Service, they have attended national and international scientific workshops and assemblies to report on the activities of the SRMV and to validate the new proposals aiming to improve some aspects of the tasks they carry out.

| SRMV as a part of the ISGI
Since its creation, the Ebro Observatory has housed the international SRMV, responsible for creating and publishing lists of rapid magnetic variations. As already mentioned, this task was entrusted to the Observatory by the IAGA and is part of the International Service of Geomagnetic Indices (ISGI). ISGI, through the ISGI Collaborating Institutes, has the responsibility of carrying out the derivation, publication and dissemination of magnetic indices (IAGA, Resolution No. 9, 1989), and ensuring the homogeneity of the data series.

| Evolution in the dynamics of the service. Traditional method
The work involved in evaluating each case was very laborious in the past and increased further during years of maximum solar activity as the number of SC and Sfe events usually follows the solar cycle ( Figure 1). In years of maximum solar activity, the number of alerts received, and the work required to process them, can increase by a factor of 6 compared to years of minimum solar activity. For both phenomena, SC and Sfe, the traditional detection method started by analysing the movements of the curves on the magnetograms (Figure 2). Those variations suspected to be an Sfe or an SC were reported in a list of events called preliminary report (Figure 3) constructed by the scientist responsible for each observatory of the network distributed through the world.
These lists, on paper, were sent monthly (by regular courier) to the SRMV with potential events to be considered as SC or an Sfe.
The SRMV created a combined list in a summary, known as checking lists, which were sent back (again by regular courier) to the observatories for a second review. The observers went back to their magnetograms and qualified the reports using a letter code: • A very clear movement; • B fair, ordinary movement; • C very poor movement; • D movement not observed, although records are satisfactory; • E movement cannot be observed due to heavy disturbance; • X record missing. • 3 = the observed movement is certainly an Sfe; • 2 = the observed movement is probably an Sfe; • 1 = the observed movement is probably not an Sfe; • 0 = the observed movement certainly is not an Sfe.
The same procedure was carried out for SC. The reviewed/qualified lists were then returned once more to the SRMV by regular courier (Figure 4).
Once the information of all these secondary reports had been gathered by the SRMV, new tables were composed (Table 3).
For each case of Sfe and SC, to determine the region where the phenomenon was observable, global maps showing the light and dark zones were constructed ( Figure 5).
Additional solar and ionospheric data directly measured at the Ebro Observatory or from catalogues were compiled to confirm or discard them. Then, with all these inputs based on data, the final judgement was made and the event was classified.
For Sfe, as well as the true events that were classified as certain, those presenting some features compatible with Sfe while simultaneously presenting other more questionable characteristics were classified as doubtful, and those that clearly did not represent real solar-flare effects were classified as rejected. Over time, only certain Sfe were reported in the lists because many studies only focused on unmistakable events.
For SCs, the final task was to give the amplitudes, onset time and the duration of the events. The SRMV asked (via regular courier) the five official low-latitude observatories (and the five supplementary ones) to provide a copy of their magnetograms for each event. An example of an SC event is shown in Figure 6 where the H-component of the geomagnetic field for the five lowlatitude observatories is plotted. The event occurred on the 5th May 2018 at 10:25 UT. It had a duration of around 5 min and an amplitude up to 15 nT for each of the five low-latitude observatories (more details at http://www. obseb re.es/en/rapid). This event was followed by a decreasing of the magnetic field, a magnetic storm, so the event was classified as an SSC.
Sensitivities and base lines to interpret the measurements correctly were also requested ( Figure 7).
The xerocopies, photographic copies and microfilms also arrived by regular mail and, finally, the amplitudes of the variations at each observatory were measured. Their means were incorporated into the events' lists (for more detail, see Section 2.2.1.). These lists did not appear until 1 year after the events were produced (Curto, 2020). The editorial work behind the production of the IAGA bulletins by ISGI often delayed the availability of these lists by even more years. Finally, these paper bulletins were distributed worldwide, once again by post.
Nowadays, the method has been simplified and the electronic mean used for exchanges and dissemination speed up the whole process. Thus, the lists elaborated by the collaborating observatories are received promptly -once the month is over -via e-mail and a second round of forwarding the checking lists back to the observatories is no longer carried out. In the past, the SRMV did not have direct access to the magnetograms but now, taking advantage of the new facilities in data access provided by the INTERMAGNET network, they are available almost in real time. So, provisional lists are updated during the next month and definitive lists can be consulted once the year has come to an end ( Figure 8).

| Collaborating observatories
The SRMV data products and outputs rely on the huge amount of work carried out at magnetic observatories, by observers directly, or by involved scientists, who dedicate part of their working time to report on events. All together, F I G U R E 2 Magnetogram corresponding to the magnetic declination at Ebro for the 8th July 1992. At 9:44, the crochet-like movement was reported as a very clear solar flare effects (Sfe) by the observer who reported it in the corresponding preliminary list of that month they form the fundamental network of primary data suppliers. They send alerts when they detect, in the magnetograms of their observatories, a movement that may be suspected to be a rapid magnetic variation. However, the number of worldwide collaborating observatories has declined with time (Table 4) due to the increasing process of automatization and reduction in the observatory's staff. Moreover, although all observatories report SC, only some of them report Sfe (20% fewer).
Nowadays (2021), some observatories have re-joined the network and the group of collaborating institutions is composed of 19 observatories which are governed by 11 agencies (Table 5). Unfortunately, their distribution is uneven (they are grouped in fewer zones such as Europe and the extreme east of Asia, so they do not cover properly the world surface).
Recently, the Bureau Central de Magnétisme Terrestre (BCMT) that gathered all magnetic observatories managed by French institutes (http://www.bcmt.fr, hosted by IPG, Paris, France) provide alerts from a network composed of nine observatories (CLF, TAM, PHU, MBO, KOU, PPT, DLT, IMP and LZH) by mean of an automatic SC detection algorithm.

| Criteria
Given the difficult morphology of these events, even experienced observers at the collaborating observatories produce reports with alerts that cannot be classified as SC or Sfe in the end. For example, in the 2017-2018 period, although 356 alerts were received and processed by the SRMV, 51% of them were false positives. And even with this big number of alerts, there were 13% false negatives. Sometimes, events listed from neighbour stations do not match. So, each alert must be dully checked by the F I G U R E 3 Preliminary list from Niemegk observatory in June 1988. sudden commencements (SC) and solar flare effects (Sfe) candidates' events were reported monthly SRMV in a thorough and complete way, which is very time-consuming.
Thus, it would be desirable to have a manual with examples and advice to help observers. In the past, an atlas was initiated but not finished (IAGA, 1959;Romañá, 1959) and now once again this idea of elaborating an atlas is under consideration because it could help to unify criteria and produce more homogeneous lists.

| A new challenge: automatic detection
Another way to save time is to design algorithms that can automatically detect, trace and scale the rapid variations instead of requiring manual procedures by observatory personnel. Such algorithms will be more objective in their assessment. They will have objective rules in their programming or clear pattern recognition processes after a training on the clearest events.

| Sudden commencements automatic detection
Sudden commencements (SC) are produced by an increase in the pressure of the solar wind and they present a global imprint. This characteristic encouraged many researchers to create an SC automatic detection algorithm (Ghamry et al., 2013;Hafez & Ghamry, 2011;Joselyn, 2011;Shinohara et al., 2005;Takano et al., 1999). The SRMV also developed an SC automatic detection method (Segarra & Curto, 2013). The main difference between this method and the first method mentioned above arises in the final objective of creating event lists in a quick and reliable way but with one restriction -to be as consistent as possible with the manual method so as to maintain continuity with the historical list and full homogeneity of the data sets.
The difficulties in creating a new detection method consistent with the manual detection method arise in the various definition of the phenomena. In 1973, Mayaud introduced a lot of changes and improvements in the SC definition and its identification criteria. In fact, his new F I G U R E 5 Synoptic map with symbols located in the position of the observatories with the variations they observed for an solar flare effects (Sfe) event (July 8, 1992 09:44). The drawing is oversimplified but one can deduce that abscissa represents longitude and ordinate represents latitude. Central vertical line represents midday. The basic information for this map is located in Table 2. In the case analyzed here, the most significant variations reported are located in the daytime hemisphere as would be expected corresponds for an Sfe F I G U R E 6 An example of sudden commencements (SC) occurred the 5th May 2018 at 10:25. The figure shows the H-component of the magnetic field for the five low-latitude observatories, Honolulu, San Juan, M'Bour, Alibag and Kanoya definition is still used nowadays: 'sudden commencements followed by a magnetic storm or by an increase in activity lasting at least one hour'. This definition is a morphological definition and the concept of 'change of activity' has to be interpreted by each observer and remains highly subjective.
Another important difficulty belongs to the physics of the phenomena showing different morphology depending on the longitude and local time of each observatory (Araki, 1994). For that reason, the SRMV focused its attention on data from low-latitude observatories where the morphology of SC is comparable to a step-like function. To cover the Earth with a good longitudinal distribution, a set of five low-latitude observatories was chosen, but over time these selected observatories have changed. When the SRMV was first housed at the Ebro Observatory, the five low-latitude observatories were Honolulu (HON), Fuquene (FUQ), M'Bour (MBO), Alibag (ABG) and Port Moresby (PMG). Following the closure of some of them, nowadays the five low-latitude observatories are Honolulu (HON), San Juan (SJG), Guimar (GUI), Alibag (ABG) and Kanoya (KNY) and their respective substitutes in specific cases of an absence of data are Apia (API), Kourou (KOU), Tamanrasset (TAM), Hyderabad (HYB) and Guam (GUA). Figure 9 shows a map with the location of these observatories. Notice that in regions such as the Pacific or Africa, the scarcity of observatories can make data selection difficult in the case where some of the observatories mentioned experience a failure in their data collection.
In accordance with the decision taken in the XXIV IUGG General Assembly at Perugia in 2007, some changes have been introduced in order to make the SC definition less ambiguous. That is, an event is considered to be an SC if the rate of change of a sudden increase in the magnetic field is equal or larger than 3 nT/min for at least three of five low-latitude observatories. The SC are differentiated as either storm sudden commencement (SSC) or sudden impulse (SI). SSC are those SC followed by an increase in magnetic activity within the next 48 hr, with Dst index reaching the threshold of -50nT (or lower) or with Kp index reaching the threshold of 5o (or higher). The SC that do not observe the aforementioned magnetic activity are classified as SI.

F I G U R E 7 Letter from ABG observatory providing base lines and sensitivities necessary to measure amplitudes of the events for year 1976
These criteria were tested in advance in order to ensure that the new lists are coherent with the oldest lists. The objective criteria enabled the SRMV to develop an automatic method to detect SC based on neural networks (Segarra & Curto, 2013). Neural networks have the ability to learn from cases and we try this methodology with the aim of transferring the experience of the Service to the algorithm. The architecture of the network consists of three layers: one for the inputs, one hidden and another for the outputs (Figure 10).
The morphological definition of Mayaud has been taken into consideration in the selection of the inputs. Then, the inputs are date, slope, change level in X and Y components and change of rhythm. Instead of amplitude, we worked with the change of levels to avoid uncertainty introduced by the presence of possible preliminary reverse impulses (PRI). The change of levels was calculated as the difference ahead and behind the SC onset time, for a magnetic field averaged over 10 min. The change of rhythm was calculated with the difference in the standard F I G U R E 8 Workflows for the traditional method (left) and method used nowadays (right). The whole process has speeded up using internet facilities including email and real-time web services deviation of the derivative ahead and behind the SC, averaged for 60 min. The output is a logical YES/NO equivalent to a true/not true event. One neural network was developed for each one of the five low-latitude observatories. The criteria to consider an event fully detected is that at least three of five observatories' neural networks reported a YES for the particular event.
The neural network has been working since 2017 acting as a preliminary internal list of SC. The Service staff also make a comparison between the results of the F I G U R E 9 Map with the five lowlatitude observatories used to determine sudden commencements (SC) amplitude. Green dots represent the location of the original ones. Red squares represent the location of the observatories used currently. Blue triangles are those used as alternative to the main ones when their magnetograms are not available network methodology and the cases reported by the observatories' collaborators. And finally, each month a preliminary list of SC events is published at http://www.obseb re.es/en/rapid. The experience of working with the neural network has proved really successful and compatible with the cases reported by collaborators. Discrepancies emerge for cases that are even difficult to detect manually. These are what we call limit cases: close to the minimum slope required, with too slow a slope to be considered sudden or with a really small amplitude. In any case, neural network methodology represents a valid alternative for the future if we see a greater decline in the number of collaborating observatories.

| Sfe automatic detection
As mentioned above, the reduced number of observatories reporting rapid variations means the network does not obtain all the necessary observational data for appropriate analysis from around the world. This problem is even more dramatic in the case of Sfe events detection because of their limited extension (only in the illuminated area) and having fewer observatories reporting them. Historically, there have been fewer attempts to achieve automatic detection of Sfe than with SC because they do not have a definite pattern -Sfe rarely appear with a perfect crochet shape -and, additionally, they usually only have small amplitudes which, being similar to other magnetic perturbations, makes it difficult to separate them from this natural noise (Curto, 2020).
However, some progress has recently been achieved. Two attempts using different strategies should be mentioned. One strategy, called the Morphological Model, takes advantage of one of the Sfe characteristics: they usually have a rapid rise followed by a smooth decay allowing us to create morphological models for each magnetic component. Then, the definite Sfe time interval can be identified by setting conditions on various parameters such as the correlations of the measured data with the models or model similarities among components (Curto et al., 2022). The other strategy, called the Geometrical Model, is based on some properties of Sfe ionospheric electric currents, such as their spherical symmetry around the vortex. Here, the algorithm calculates the derivative of the data in order to avoid contamination of the daily variation Sq, and, by means of trigonometric formulas, computes the magnetic radial component relative to the Sfe current vortex (the focus), and finally, with these data, creates an Sfe index (Curto et al., 2017;Curto et al., 2022). Again, to ensure homogeneity of both, manual and automatic detection lists, careful checking was performed computing ROC curves and Youden index in each case.
A more complex approach could be to continuously monitor the ionospheric electric currents producing the Sfe using SECS methodology as in Curto et al. (2018). This powerful technique is still being tested but promises to give a comprehensive visual representation of the origin of the Sfe magnetic signatures.

| Proxies
Given the uncertainty in SC and Sfe determination based only on the observation of the magnetograms, over the years that we have been working in this field, other proxies have been consulted through the Service to gain confirmations. Previously, solar Hα and F 10 were used to contrast Sfe alerts with solar activity events. Also, ionospheric proxies such as some sudden ionospheric F I G U R E 1 0 Neural network architecture for sudden commencements (SC) detection (Segarra & Curto, 2013) F I G U R E 1 1 (a) One of the storage racks where the historical files are preserved; and (b) some bundle files containing the documentation on paper used to compile the rapid magnetic variations' events of 1 year disturbances (atmospherics, absorption in D layer) were used. However, they provided a limited spatial and temporal resolution. Later, as satellites came into use, the availability of X-ray intensities allowed us to confirm more directly the presence of a flare. Nowadays, with the advent of new technologies (especially with the deployment of GNSS satellite constellations), we are able to scan the ionosphere with wide coverage and in quasi-real time. Hence, the creation of an ionospheric activity index related to the presence of solar flares as confirmation of Sfe (Curto et al., 2019. Direct monitoring of the solar wind by satellites at the Lagrange point also makes the task of confirming SCs easier.

DELIVERY. THE SRMV DATABASE
Historical yearly files with preliminary reports, checking lists, maps, magnetograms, etc., and, in general, all the documentation used to analyse each event are stored by the SRMV (Figure 11a).
The methodology and the support materials used by the SRMV have changed with time. In the beginning of the Service, all the documentation was entirely in paper format, and very often on hand-written documents (Figure 11b).
The SRMV database in paper format covers the period 1957-2001. It includes all monthly preliminary reports by the collaborating observatories, the preliminary checking lists created by the SRMV as a summary of them, the answers of the observatories to the checking lists with their assessment of each candidate, synoptic maps elaborated by the SRMV for each event and the copies on paper (xerocopies, photocopies and microfilms) of the five low-latitude observatories' (and their substitutes) magnetograms. Also, letters from those observatories, with the sensitivities and baselines of their magnetograms, in order to measure the amplitude and the duration of the SC events. Additionally, there are plenty of handmade auxiliary tables created by the staff of SRMV to cope with all this huge amount of information. All these materials on paper are kept in bulky files in the SRMV database.
Some paper copies of magnetograms, used by Mayaud (1973) to create the first part of the SC list from 1868 to 1967, are stored in France at ISGI headquarters.
In more recent years, from 2002 to nowadays, this work has dramatically changed, hand in hand with changes in technology. Paper documents are no longer collected and all the information is stored in digital files in plain text files or in spreadsheet files.

| New tables of SC amplitudes
From the outset of data collection, SC tables from the five low-latitude observatories have been published showing an average of the duration and amplitude of the event. However, as the understanding of SC has evolved, it is clear nowadays that the average of the five low-latitude observatories makes little physical sense. So, since 2005, the Service has published the duration and the amplitude of each of the five low-latitude observatories.
Recently, the Service has also been working to recover the individual amplitudes and durations of the five low-latitude observatories from the Service database. In Appendix B, an example is shown: the list of SC for 1987. The old list has been revised and expanded with the individual values of amplitudes and rise times.

| Dissemination
The final annual lists of rapid variations are compiled by the SRMV and published in the IAGA bulletins on paper by the ISGI. A yearly list with classifications of SC and Sfe has been developed. Ever since the start of our work, SSC and Sfe data have appeared on separate lists.
The bulletins published annually by the IAGA refer to the global magnetic activity indices as well as the rapid variations in the magnetic field, in particular, the SC and Sfe (IAGA, 1954(IAGA, -1990. IAGA bulletins are not published in paper any more by the ISGI. But, digital lists can be found through its official website (http://isgi.unist ra.fr/data_downl oad.php). Available files format is a simple tabular text, a format similar to IAGA 2002 format used for magnetic observatory data.
With the idea of providing a quick list to researchers who need to analyse recent episodes, ever since 2015, a presentation of the preliminary data of the rapid magnetic variations has also been displayed on the Ebro website (http://www.obseb re.es/en/rapid) with a similar format as that of the definitive ones, but without having the verification task done. The name of the archives with the preliminary data of every year is similar to one of the definitive data, but with a final 'p' instead of the 'd' associated with the definitive ones.
All the SRMV data products and outputs are licensed under a Creative Commons Attribution Non-Commercial 4.0 International License (CC BY-NC 4.0). Their use, in or, for commercial purpose is subject to formal agreement of the data owner, namely the SRMV. That licence is thus considering the restriction and compliance with primary data that are the magnetic observatory magnetograms while allowing a licence as open as possible.
In an effort to promote the use of indices and remarkable events (rapid magnetic variations), the Ebro Observatory and ISGI actively participate in the EPOS H2020 project. EPOS goal is to establish a comprehensive multidisciplinary research platform for the Earth sciences in Europe by establishing a long-term plan to facilitate the integrated use of data, models and facilities. Legal solutions were adopted securing a common and shared data policy, the open access and the transparent use of data, and guaranteeing mutual respect of the intellectual property rights. Metadata standard formats were defined and Application Programming Interfaces (API), acting as software intermediaries, were implemented to allow applications in computers to talk between each -others.
Digital Object Identifiers (DOI) are nowadays the universal mean to reference any digital resources on long term. Once a DOI is minted on a particular resource, for example, a growing time series of events; the time series itself cannot be changed or corrected. Only new values may be appended to the end. If an historical value needs to be corrected, then the DOI has to be changed as the underlying resource will change. Each DOI is materialized by a landing page that permanently expose the referred resource. The DOI allow to find the landing page through redirection operated by the https://www.doi. org/organization. Our aim is to have our RMV growing datasets to be attached to a DOI, so everyone can just reference this dataset by using the DOI for even better reproducibility. The first steps in this sense are currently being taken.
Finally, due to the changes in the data sets over the years, the formats have changed. This makes the data less reasonably usable for researchers. So, creating a single homogeneous format that would cover all the changes is now under consideration.

| CONCLUSIONS
The SRMV is a dynamic service that has carried out the task endorsed by the IAGA in its founding mandate. However, the SRMV does not only continue to compile the annual lists in what is now a century-long series but it fosters new actions such as promoting the knowledge of these phenomena, creating normative proposals or focusing the interest of the scientific community on this field.
Over recent years, new challenges have emerged. For instance, difficulties in the task of elaborating alerts show the necessity of providing a comprehensive manual to guide observers who produce these alerts. Algorithms for automatic detections have been tested to complement manual work done by the collaborating observers. Also, the SRMV boosted the use of more precise proxies to determine whether candidates are true SC or Sfe events. Finally, new ways of dissemination have been adopted to provide easy access to the Remarkable Events (Rapid Magnetic Variations) lists and make the researchers' work easier.
Summarizing, the SRMV carries on its work improving determination methods, and the quality of the data sets produced.