P1 – International Coordination Efforts for Improving Space Weather Science and Services
Talks
P1 Tue 5/11 11:30-13:00, room Auditorium
Chairs: Jesse Andries, Masha Kuznetsova, Joaquim Costa
Author(s): Sharafat Gadimova
United Nations Office for Outer Space Affairs
Abstract: Extreme natural events serve as a warning that the development of technological systems, including space technologies, has reached a point where exposure of such systems to adverse factors of space weather may have catastrophic impacts and result in immense losses. Therefore, there is a clear need to foster more synergy and promote the convergence of common interests in space weather among all stakeholders.
As space weather is intrinsically international in its scope of impact, expertise, monitoring and forecasting capabilities developed by multiple nations and stakeholders would benefit from improved coordination. This is especially relevant for filling key measurement gaps, securing the long -term continuity of critical measurements, advancing global forecasting and modelling capabilities, identifying potential risks and developing practices and guidelines to mitigate the impact of space weather phenomena, including on long -term observation of climate change and risk events.
The International Space Weather Initiative has proved to provide a framework for collaboration among teams of scientists, serving as an example of remarkable international work in instrument operation, data collection and analysis and the publication of scientific results. The Initiative has established a platform for a bottom-up approach in order to produce space weather-literate communities, in particular in developing countries, work together as a network for sharing ideas, information and data, and develop joint projects.
Author(s): Clezio De Nardin, ALL4Space Team (in alphabetical order on the annex file)
National Institute for Space Research (INPE), Sao Jose dos Campos (SP), Brazil; Argentina, Brazil, Chile, Mexico and Peru
Abstract: Introduction: To enhance the significance of space weather events in the context of UN long-term sustainability guidelines, considering that space usage relies primarily on knowledge rather than regulations alone, we appraise the following points to be emphasized in the international agenda.
Global Impact of Space Weather: We share the international concern regarding space weather and its potential threats to ground- and space-based infrastructures. In this regard, Latin America is carrying actions to decimate such conscienceless that involve public outreach, training schools, scientific workshops, and courses given in the Latin American regional training centers of WMO.
Global Cooperation: Predicting and mitigating space weather impacts requires a global approach through international cooperation and coordination. In this regard, we are carrying out a series of technical working meetings (e.g. São Jose dos Campos in Nov. 2022, Ushuaia in Oct. 2023, and Monterrey in Apr. 2024) to create a Latin American Regional Center for Space Weather Monitoring and Forecasting in harmony with a training center and the definition of the headquarter of a Latin American Society for similar purpose.
Recognition of National and International Initiatives: We acknowledge and appreciate ongoing national and international activities, such as the new 5-years program for the SCOSTEP, a thematic body of the ISC. We also highlight the International Space Weather Coordination Forum held in Geneva, on November 17th, 2023, in partnership with the WMO, the ISES, and the COSPAR. In this regard, representatives of the INPE, the UBA, and the UNAM actively engaged in the forum and signatories of the Statement of Intent resulting from the meeting which says that we shall “…develop or contribute to mechanisms promoting international cooperation and/or coordination […] through an International Agency Space Weather Coordination Group (IASWCG)…”.
Role of Expert Groups and Committees: We also acknowledge the contributions of expert groups and committees, such as the Expert Group on Space Weather of the Scientific and Technical Subcommittee. We highlight the importance of their discussions in advancing the understanding of space weather and fostering collaboration. Thus, the authors supported all international discussion forums to standardize and exchange best practices for space weather science and services. We have also been working to include the local space weather expert groups in the ISES.
Structure and Mechanism Development: We acknowledge that setting up an international coordination group for space weather, in collaboration with COSPAR, ICAO, WMO, and ISES, requires careful consideration of its structure and working mechanism. Nevertheless, the establishment of an International Agency Space Weather Coordination Group (IASWCG) has the potential to foster all international initiatives and accelerate the process of building the necessary infrastructure to shield society against space weather hazards.
In conclusion, by underscoring the global impact, the necessity for collective action, and the ongoing initiatives, this approach seeks to emphasize the importance of space weather events within the framework of long-term sustainability (LTS) guidelines, recognizing the need for collaborative efforts on an international scale.
Author(s): Mamoru Ishii, Sergio Dasso
NICT / ISEE Nagoya Univ.; Laboratorio Argentino de Meteorologia del esPacio (LAMP)
Abstract: The International Space Environment Service (ISES) is a collaborative network of organizations providing space weather services around the globe. Its mission is to improve, coordinate, and deliver operational space weather services. ISES is organized and operated for the benefit of the international space weather user community.
ISES currently includes 21 regional warning centers, four associate warning centers, and one collaborative expert center. It is a Network Member of the World Data System (WDS) of the International Science Council (ISC; formerly ICSU) and collaborates with WMO and other international organizations.
ISES has been the primary organization engaged in the international coordination of space weather services since 1962. Its members share data and forecasts and provide space weather services to users in their regions. ISES provides a broad range of services, including forecasts, warnings, and alerts of solar, magnetospheric, and ionospheric conditions; space environment data; customer-focused event analyses; and long-range predictions of the solar cycle.
As a principal body of space weather operational organization, ISES cooperates to promote the coordination of space weather related organizations with WMO and COSPAR. WMO-ISES-COSPAR are leading efforts in coordination and cooperation of space weather research and operations and held a first meeting of the International Space Weather Coordination Forum on November 17, 2023, at WMO headquarters, Geneva.
Author(s): Tiera Laitinen, Yana Maneva, Krista Hammond, Kirsti Kauristie
Finnish Meteorological Institute; STCE; UK Met Office; Finnish Meteorological Institute
Abstract: Within WMO, the Expert Team on Space Weather (ET-SWx) lead the activities of transitioning space weather into operations as well as stakeholder engagement activities. The Executive Council of WMO adopted the Four-Year Plan for WMO activities related to space weather (2024−2027) in its recent meeting (June 10−14, 2024). Besides concrete implementation tasks to integrate appropriate recommendations and standards for the SWx discipline within the WMO frameworks, the Plan includes actions for improved global coordination of space weather activities in consultation and collaboration with other relevant actors and international organizations.
Obviously, the International Civil Aviation Organization (ICAO), with its arrangement of four global SWx centers, is a major stakeholder of this coordination effort. In the presentation we will give a review of the Four-Year Plan priority activities and objectives for enhancing SWx capabilities in collaboration with intergovernmental organizations. The Plan will be discussed from the viewpoint of the PECASUS consortium, which is one of the ICAO SWx centers. As PECASUS has been operational already for more than four years under the strict ICAO regulations, the consortium has gathered valuable experience in several aspects addressed in the ET-SWx Four-Year Plan. With this background we will identify areas where ICAO SWx services can be improved to match with the WMO recommendations, and areas where existing WMO guidelines might require future iterations to better address the diverse needs of multinational 24/7 SWx service provision.
Author(s): Manuela Temmer, Camilla Scolini, Ian G. Richardson, Stephan G. Heinemann, Evangleos Paouris, Angeklos Vourlidas, Mario M. Bisi
Institute of Physics, University of Graz, Austria; Royal Observatory of Belgium, Belgium; Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; University of Helsinki; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA; RAL Space, United Kingdom Research and Innovation, UK
Abstract: The COSPAR iSWAT (international Space Weather Action Teams) initiative is a global hub for collaborations addressing challenges across the field of space weather. We present the COSPAR Space Weather Roadmap update for the iSWAT clusters H1+H2 covering interplanetary space and its characteristics, with focus on large-scale corotating and transient structures impacting Earth. We review the physical background of different solar wind streams together with coronal mass ejections and the considerable efforts that have been made to model these phenomena. We outline the limitations coming from observations with rather large uncertainties, making reliable predictions of the structures impacting Earth difficult. Moreover, in the wake of the upcoming solar cycle 25, the increased complexity of interplanetary space with enhanced solar activity poses a challenge to models. The current paper presents the efforts and progress achieved in recent years, identifies open questions, and gives an outlook for the next 5-10 years.
Author(s): Veronique Delouille, Freek Verstringe, Yana Maneva, Lukas Vinoelst, Dimitrios Millas, Daria Shukhobodskaia, Senthamizh Pavai V., Jasmina Magdalenic, Luciano Rodriguez, Judith de Patoul, Baptiste Cecconi, Stéphane Erard, M. Leila Mays, Chui Wiegand, Christine Verbeke
Royal Observatory of Belgium; Royal Observatory of Belgium; Royal Observatory of Belgium; Royal Observatory of Belgium; Royal Observatory of Belgium; Royal Observatory of Belgium; Royal Observatory of Belgium; KULeuven; Royal Observatory of Belgium; Royal Observatory of Belgium; Observatoire de Paris; Observatoire de Paris; NASA/Goddard Space Flight Center; NASA/Goddard Space Flight Center; KULeuven, NASA/Goddard Space Flight Center
Abstract: Adopting international standards for metadata description, access protocol, and file format sets a dataset to a high degree of FAIR-ness, that is, the capacity to find, access, interoperate, and re-use the data. It therefore allows smooth integration and scientific re-use of data by the community, leading to enhanced knowledge and further discovery and innovation.
Over the past decade, several standards have become increasingly common in the solar physics community: Heliophysics Data Application Programmer’s Interface (HAPI) for serving time series; the SOLARNET recommendations for FITS metadata description; the Table Access Protocol (TAP) and its version for solar system science (EPN-TAP) for accessing various types dataset (image, catalog, spectra, etc,…). Along with EPN-TAP comes EPNCore, a standard required for describing in an uniform way the metadata associated with an EPN-TAP service. A commonly accepted data model for describing solar events as well as a chain of events is however still missing.
We report here on work performed at the Royal Observatory of Belgium to implement those standards and the necessary collaborations towards this goal. First, the collaboration with Observatoire de Paris allows us to set up EPN-TAP services and to build data models for describing solar events. Second, going one step further than individual event characterization, we report on our current effort with the Community Coordinated Modeling Center (CCMC) to describe in a common way chains of events erupting on the Sun and propagating towards the Earth.
Panelists: Sharafat Gadimova, Clezio De Nardin, Mamoru Ishii, Tiera Laitinen, Manuela Temmer, Veronique Delouille
Posters
Posters I Display Tue 5/11 – Wed 6/11, room C1A – Aeminium
Authors in attendance: Tue 5/11 10:15–11:30, 15:15-16:15; Wed 6/11 10:15–11:30
Author(s): Jiankui Shi, Guojun Wang, Zheng Wang, Xiao Wang, Maosheng He, Bodo Reinisch, Ivan Galkin
National Space Science Center, Chinese Academy of Sciences; National Space Science Center, Chinese Academy of Sciences; National Space Science Center, Chinese Academy of Sciences; National Space Science Center, Chinese Academy of Sciences; National Space Science Center, Chinese Academy of Sciences; Space Science Laboratory, U-Mass, Lowell; Space Science Laboratory, U-Mass, Lowell
Abstract: Ionospheric Scintillation is well known as space weather phenomenon which can seriously affect radio propagation. At low latitude, the ionospheric scintillation has been considered as result of Equatorial Plasma Bubble (EPB) caused by R-T instability after sunset. With Digisonde and GPS receiver located at some low latitude stations, we found a new type of Spread-F (SF) named Strong Range SF (SSF) having high correlation to the scintillation. So, with Digisonde, there will be more means to monitor and predict ionospheric scintillations and can enhance the predictive accuracy. According to the URSI handbook, the ionospheric irregularity SF observed wherever (any latitude) are divided into four types, i. e, frequency SF, range SF, mixed SF, and branch SF. Using the data of Digisonde at low latitude stations Hainan (109.1°E, dip.19.5°N), Vanimo (141.3°E, dip.11°S), and Acsension IS (345.6°E, dip. 2.3°S), we investigated the types of SF. The results showed that branch SF has never observed in the low latitude stations. However, SSF drawn from the range SF has often taken place. In the Digisonde ionogram, the SSF has characteristics that diffuse echoes extend from low to high frequency and make the ionospheric foF2 could not be definable. The important results were that, only the SSF often took place from 1800 to 2300 LT and had a maximum occurrence in the period of 2000 to 2200 LT which was just the period of peak occurrence of low latitude scintillation. While the other types of SF were not. The SSF had maximum occurrence in Equinoxes and Summer, which was the same as the scintillations. Furthermore, the results showed that the SSF had close correlation to scintillation over these low latitude stations. We also found that the SSF were never observed at high latitude station. Alfonsi verified it using the Didisonde and GPS receiver data from Tucumán station (294.6°E, dip. 15.5°S). We also verified it with the data from other 6 low latitude stations. We analyzed Cosmic satellite in-situ date on EPBs. It showed when the Cosmic flied over the low latitude station Hainan or Vanimo, the EPBs could be clearly observed by the Cosmic, while SSF and scintillations could be observed in the ground station concurrently. Since the ionospheric scintillation at low latitude is caused by the EPBs, therefore, the SSF should also be results from the EPBs. In the science, we suggest that, at low latitude, the ionospheric SF be divided into four types, i.e., frequency SF, mixed SF, range SF and strong range SF, which is different from that described in the URSI’s Handbook. Since the low latitude scintillations has closer correlation with SSF, for space weather application, we suggest combine the Digisonde and GPS receiver at low latitude together to monitor and predict ionospheric scintillations. We call for cooperation using monitor data to investigate on the SSF and the Scintillation for that at low latitude. This will provide more means to monitor and predict the scintillation at low latitude and to enhance the predictive accuracy.
Author(s): Eric Guyader, Matteo Sgammini, Kjell Ove Orderud, Matias Krogh Boge, Kjell Arne Aarmo
European Commission – DG DEFIS; Joint Research Center; Space Norway; HEOSAT; Norwegian Space Agency
Abstract: The Arctic Satellite Broadband Mission (ASBM) is composed of 2 satellites placed in highly elliptical orbits, specifically a Three-Apogee (TAP) orbit at 63° inclination, with an orbital period of 16 hours, and crossing altitudes between 8,700 and 43,000 km over Northern hemisphere. While the primary mission of ASBM is to provide broadband telecommunication services over the Arctic area, a payload for space radiation monitoring has been fitted on-board one of the satellites.
The radiation monitoring unit, called NORM (Norwegian Radiation Monitor) will have an expected lifetime of 5 years and will document the radiation environment at the covered altitudes. This will contribute to increasing the understanding of what phenomena might affect radiation levels at these altitudes along the orbit path.
The satellites will be launched mid July 2024, onboard a Space X launch vehicle from the South California space base ‘Vandenberg’. The NORM instrument will be switched-on already at separation stage, so that it collects data during the orbit raising phase, recording radiation at specific altitudes (i.e. Mcllwain coordinates) that will never be crossed again during its nominal mission.
During the ASBM mission, NORM will be exposed to the trapped radiation belts and partially the environment outside the Earth’s magnetosphere e.g. cosmic rays and solar particle events – providing a unique insight into various domains of space physics. The data will represent a continuous flux of information about kinetic energy of electrons and protons impinging on the space vehicle.
The European Union has teamed up with the Norwegian Space Authorities to acquire the data from the NORM mission. A contract is in place where data will be continuously recorded by the mission control in Norway and delivered to the European Union’s Joint Research Centre, Ispra. The European Union develops and operates space infrastructures such as Galileo, EGNOS, Copernicus, Space Surveillance and Tracking and later IRISS. For all these programmes, the data coming from NORM will be useful for design, operations, and diagnosis. In addition, access to the data will be facilitated for the scientific community to contribute to the broader understanding of Sun-Earth interaction and of the effects of space weather on Earth’s magnetosphere, ionosphere, and other space-based technologies.
Interested parties will be invited to submit request for data access from dedicated platforms set up by the Norwegian Space authorities and the European Union authorities.
Finally, the European Union wants to procure up-to-date analytical tools for processing and exploiting the data coming from NORM. An invitation to tender will be published in 2024.
Author(s): Xiao-Xin Zhang, Tonghui Wang, Fei He, Jingtian Lv, Qiugang Zong, Huishan Fu
National Satellite Meteorological Center; National Satellite Meteorological Center; Institute of Geology and Geophysics; National Satellite Meteorological Center; Peking University; Beihang University
Abstract: The Earth’s magnetosphere is formed by the interaction between the solar wind and the Earth’s magnetic field. There are various regions of fields, plasmas, and currents inside the magnetosphere such as the plasmasphere, the ring current, and radiation belts. The highly dynamic conditions of the magnetosphere create the variable space weather. The magnetospheric system includes complicated current systems. Herein, by using the magnetic field data from Van Allen Probes, we analyzed the distribution characteristics of the electromagnetic environment in the inner magnetosphere on different Dst* index and magnetic local time. Our results show that for the response of different current systems, the dawn-dusk and noon-midnight asymmetry distribution of the residual magnetic field δB increases with Dst* index. When Dst* < −60 nT, a “banana”-shaped geomagnetic field negative disturbance peak region appears in the sector from midnight to dusk. Then, we obtained the azimuthal current density and found the asymmetric internal eastward and external westward ring current. Through the vector analysis of three-dimensional current density, the current density vector distribution in the magnetic equatorial plane is completely displayed for the first time, which directly proves the existence of banana current near r = 3.0–4.0 RE during strong geomagnetic storms.
Author(s): Knut Stanley Jacobsen, Sarah Schultz Beeck, Petri Koskimaa, Liisa Juusola
Norwegian Mapping Authority; Technical University of Denmark; Finnish Meteorological Institute; Finnish Meteorological Institute
Abstract: We present a case study of scintillation during two severe (G4) storms in 2023.
The study is based on data from networks of scintillation receivers in Greenland, Iceland, Faroe Islands, Norway and Finland.
This combined network provides coverage of a large part of the Arctic, allowing a large-scale picture of the
spatial distribution of scintillation and how this changes in time during the two events.
Certain key spectral properties of the scintillation are shown and discussed.
The impact of the disturbances on satellite-based positioning is shown using data from a selection of geodetic receivers in the region.
Properties extracted from magnetometer measurements are investigated in relation to the occurrence of scintillation.
Correlations between ROTI and phase scintillation values are investigated to evaluate how well ROTI works as a proxy for phase scintillation.
This case study serves to demonstrate the advantage of cooperation between different scintillation measurement networks operated by different institutions, using the new scintillation file format BiScEF.
Author(s): André Csillaghy, Javier Busons, Manuel Prieto, Christian Monstein
FHNW University of Applied Sciences Northwestern Switzerland; Universidad de Alcalá, Spain; Universidad de Alcalá, Spain; Monstein Radio Astronomy Support, Switzerland
Abstract: The e-Callisto network is the only ground-based observatory capable of monitoring the Sun 24/7 in the radio frequencies between 45 MHz and 870 MHz, and any other range by using a frequency converter. It has more than 80 operational observing stations, with a core of typically more than 10 providing reliable and complementary measurements at (almost) adequately distributed longitudes and latitudes. To fulfill its role as a space weather monitoring instrument, e-Callisto is currently planning a significant upgrade to meet the expectations of the various interested communities. In this talk, we will present our progress in a joint pilot project to define a reference instrument that can be used as a starting point for the development, operation, maintenance and continuous upgrade of a long-term monitoring facility. We will emphasise the potential to cover the complementary objectives of science, monitoring (including support to space instruments) and education. We believe that our efforts are well aligned with the WMO recommendations, although this does not (yet) solve the long-term funding aspect of such a distributed installation.
Author(s): Alberto Pellizzoni
INAF-Osservatorio Astronomico di Cagliari
Abstract: Solaris is a scientific and technological project aimed at the development of a smart Solar monitoring system at high radio frequencies based on innovative single-dish imaging techniques, recently approved as a permanent observatory in Antarctica. It combines the implementation of dedicated and interchangeable high-frequency receivers on existing small single-dish radio telescope systems (2.6m class) available in our laboratories, in the Alps and in Antarctica, to be adapted for Solar observations. Operations in Antarctica will offer unique observing conditions (very low sky opacity and long Solar exposures) and unprecedented Solar monitoring in radio W-band (70-120 GHz). This will be achieved through state-of-the-art single-dish imaging techniques at radio frequencies, that allows us to map the entire Solar disk in less than 30 min with spatial resolution of a few arcminutes. This opens for the identification and spectral analysis of Active Regions before, after and during the occurrence of Solar flares.
These system features will allow Solaris to explore cutting-edge aspects of Solar Physics (e.g. chromosphere dynamic monitoring) and Space Weather applications (e.g. flare forecast). Solaris can perform continuous Solar imaging observations nearly 20h/day during Antarctic summer with optimal sky opacity. In perspective our system could be implemented also in the northern hemisphere to offer Solar monitoring for the whole year.
We intend to offer to the scientific community a very competitive tool in the challenging multi-disciplinary framework of Solar Physics and Space Weather science. The Solaris observatory will be the only Solar facility offering continuous monitoring at 100 GHz, and it will be able to collect and disseminate data in synergy with the existing national and international network of Space Weather facilities.
Author(s): Giuliana de Toma, Joan Burkepile, Sarah Gibson, Enrico Landi, Steven Tomczyk
NCAR/HAO; NCAR/HAO; NCAR/HAO; University of Michigan; Solar Scientific LLC
Abstract: The Mauna Loa Solar Observatory (MLSO) is in the Big Island of Hawaii on the flank of the Mauna Loa Mountain at 3400m above sea level. MLSO is an NSF observing facility operated by HAO since 1965 which has collected the longest record of coronal observations. There are two coronagraphs at MLSO: the COSMO K-Coronagraph (K-Cor) and the Updated Coronal Multi-Channel Polarimeter (UCoMP) which is the prototype for the proposed 1.5m COSMO large coronagraph.
K-Cor observes the low and middle corona from ~1.05 to 3 solar radii in polarized visible light. It was designed to study the formation and early acceleration of CMEs with a high temporal cadence of 15s. K-Cor data are calibrated and made publicly available in near-real time within 2-3m from acquisition and are ideally suited to be part of an early warning forecast system of SEP events. K-Cor can provide the first detection of an in-progress CME even before the CME enters the LASCO field-of-view. An automated CME detection code runs in real time at MLSO and alerts are sent to the community and to the NASA’s Community Coordinated Modeling Center SEP scoreboard.
UCoMP is an imaging polarimeter with a tunable Lyot filter that measures the Stokes parameters, I, Q, U, V in several coronal emission lines in the visible and near IR from ~1.03 to 2 solar radii. UCoMP data are processed overnight and usually posted on the MLSO webpage the day after observations are taken. The level2 data products include: intensity at three or more wavelength positions for each emission line, line-of-sight velocity, line width, linear polarization, and azimuth. Coronal densities, plane-of-sky magnetic field, and coronal waves can be derived from these data products. UCoMP provides unique information on the magnetic and plasma structure of the corona, including regions that are prone to eruptions. For example, linear polarization is used to identify signatures of magnetic flux ropes in coronal cavities and active regions and magnetic null points in pseudo-streamers. While not specifically designed to study solar eruptions, UCoMP captured several CMEs.
MLSO synoptic observations supply observational constraints to coronal and CME models, provide information on the ambient solar corona where CMEs propagate into, advance our understanding of pre-eruptive and eruptive coronal structures, and can provide early warning for CMEs. Ground-based coronagraphs like K-Cor and UCoMP complement space-based coronagraphs that observe at higher heights at a fraction of the cost of a space-based mission and provide context images and plasma diagnostics of the entire off-disk corona to complement existing EUV imagers and spectrometers. Furthermore, facilities on the Earth can be more easily updated than in space and are ideal testbeds for new instruments and new technology. We illustrate the current capabilities for space weather research and forecasts of the existing MLSO instruments, show examples of observations taken at MLSO including eruptive events, present plans for future instruments and upgrades, and highlight the potential of a network of facilities like the one at Mauna Loa for space weather.
Author(s): Keith Groves, David Hysell, Tim Fuller-Rowell, John Retterer, Charles Carrano, J. Vince Eccles, Jade Morton, Anthea Coster, Endawoke Yizengaw, P. T. Jayachandran, Alan Hoskinson, Yukitoshi Nishimura
Boston College; Cornell University; NOAA/University of Colorado Boulder; Boston College; Boston College; Space Dynamics Laboratory; University of Colorado, Boulder; MIT Haystack Observatory; Aerospace Corporation; University of New Brunswick; Boston College; Boston University
Abstract: The NASA-sponsored SPAce Research and Technology Applications (SPARTA) Center of Excellence is a multi-institutional activity led by Boston College focused on forecasting small-scale ionospheric irregularities and associated scintillations on a global scale. Although driven by science, SPARTA has practical objectives in terms of generating and validating probabilistic forecasts for scintillation activity 2-24 hours in advance and seeks collaborations in the international community for observations, modeling, validation and product-development related to this task. Forecasting capability will be demonstrated with the Whole Atmosphere Model-Ionosphere Plasmasphere Electrodynamics (WAM-IPE) currently run by the US NOAA Space Weather Prediction Center (SWPC), though the modular system under development in SPARTA will facilitate the use of virtually any background ionospheric model capable of providing the required drivers (plasma and neutral densities, drifts and temperatures). To measure performance and progress, extensive validation efforts are planned exploiting both ground- and space-based data sources such as GNSS TEC and scintillation, incoherent scatter radar, ionosondes, HF radar, GNSS radio occultations, in situ densities and GNSS reflectometry. While these efforts are fairly comprehensive, more validation sources are needed, particularly of direct scintillation measurements, to fully evaluate SPARTA’s forecast skill. We plan to implement the forecast models in the NASA Community Coordinated Modeling Center (CCMC) during the course of the project to enable community-wide access providing further opportunities for refinement and improvement. Here we will present the technical approach employed by SPARTA, planned products and opportunties for collaboration with the international community.
Author(s): Lorenzo Scavarda, Alessandro Rovera, Jens Dirk Schiemann, David Bushnell
ALTEC, Turin (Italy); ALTEC, Turin (Italy); ESA, ESTEC, Noordwijk, The Netherlands; ESA, ESTEC, Noordwijk, The Netherlands
Abstract: Human space travel is entering a new phase of exploration beyond Earth. By 2030, we expect regular trips to the Moon orbit and surface, along with increased preparations for sending humans to Mars. However, ensuring the safety of astronauts during these missions presents several challenges. One of the biggest hazards is dealing with the harmful effects of space radiation due to Solar Particle Events (SPEs) and Galactic Cosmic Rays (GCRs).
SPEs, a manifestation of space weather, drastically enhance radiation levels in a short time. Forecasting SPEs is critical for deep space operations to plan and use countermeasures effectively, adhering to the “As Low As Reasonably Achievable” (ALARA) principle for astronaut protection. SPE forecasting utilizes knowledge of solar physics and particle radiation dynamics through radiation transport physics-based models or analytical models. Currently, forecasting from physics-based models lacks the accuracy needed for human protection. Now-casting, based on precursor measurements and studies of previous SPEs, is essential for effective warnings. Development priorities include a system to exploit forecast methods and accurate measurements of the external field for now-casting and data assimilative forecasts.
This is only one of the critical points which the Scientific Community is demanded to investigate in order to develop an ESA Radiation Risk Model to better characterize mission radiation risks to astronauts.
Addressing these challenges requires broad and interdisciplinary scientific competencies. The European Radiation Facility Network – Data Hub (ERFNet-DH) project, funded and coordinated by ESA and ASI and implemented by ALTEC (Turin, Italy), aims to provide solutions by fostering international collaboration. This project enables experts in medicine, physics, biology, engineering, and other fields to exchange knowledge and insights, advancing our understanding of space radiation effects and enhancing our ability to mitigate risks for future space exploration missions.
ERFNet offers a framework where scientists and researchers from diverse disciplines can come together to access and exploit historical data, share projects and results. Indeed, it provides a scientific environment for the broader space research community to access data from historical and present missions, develop data processing algorithms, run numerical simulations and a platform to share papers, presentation, results and reach experts of the field.
Additionally, ERFNet-DH will support ESA radiation payloads on the Lunar Gateway, collecting, processing, and distributing radiation data. The first two payloads will be the European Radiation Sensor Array (ERSA) and the Internal Dosimeter Array (IDA), dedicated to space weather forecasting and dosimetry, respectively. The processed data will be made available not later 6 months in the scientific environment to the broader Scientific Community for downloading and science exploitation.
The first ERFNet Demo was presented to the ESA ERFNet Project Team in November 2023 and the first Beta version is going to be released by June 2024 for a limited group of test-users. This project exemplifies the importance of international coordination and cooperation demonstrating the value of joint efforts in advancing our understanding of space radiation and space weather impacts to ensure the safety of human space exploration.
Author(s): Olga E. Malandraki, Arik Posner, Michalis Karavolos, Kostas Tziotziou, Janet Barzilla, Edward Semones, Kathryn Whitman, M. Leila Mays, Chinwe Didigu, Christopher J. Stubenrauch, Henrik Droege, Bernd Heber, Patrick Kuehl, Monica Laurenza, Milan Maksimovic, Vratislav Krupar, Nikolas Milas
National Observatory of Athens, IAASARS, Athens, Greece; NASA Headquarters, USA & NASA Johnson Space Center, USA; National Observatory of Athens, IAASARS, Athens, Greece; National Observatory of Athens, IAASARS, Athens, Greece; Leidos Inc., USA; NASA Johnson Space Center, USA; KBR, USA; NASA Goddard Space Flight Center, USA; ADNET Systems, USA; NASA M2M/Catholic University of America, USA (former); Christian-Albrechts-Universität zu Kiel, Germany; Christian-Albrechts-Universität zu Kiel, Germany; Christian-Albrechts-Universität zu Kiel, Germany; INAF-Istituto di Astrofisica e Planetologia Spaziali, Italy; Observatoire de Paris, France; University of Maryland Baltimore County, USA; National Observatory of Athens, IAASARS, Athens, Greece
Abstract: Solar Energetic Particle (SEP) events feature a wide range of energy spectrum profiles, with energies ranging from tens of keV to a few GeV and can last for a few hours to several days or even weeks. Reliable forecasts of SEPs with sufficient advance warning are mandatory for swift mitigation of threats to modern technology, impacting spacecraft, avionics and commercial aircraft in extreme circumstances, as well as minimization of radiation hazards to astronauts especially on future Lunar or Mars missions. The HESPERIA Relativistic Electron Alert System for Exploration (REleASE) forecasting tools, operational through the Space Weather Operational Unit of the National Observatory of Athens and accessible through the dedicated website http://www.hesperia.astro.noa.gr, were developed by the HESPERIA H2020 project (Project Coordinator: Dr. Olga Malandraki). They generate real-time predictions of the proton flux (30-50 MeV) at L1, making use of relativistic and near-relativistic electron measurements by the SOHO/EPHIN and ACE/EPAM experiments, respectively. The real-time, highly accurate and timely performance offered by HESPERIA REleASE attracted attention from various space organizations (e.g., NASA/CCMC, SRAG) and ESA selected these products to be integrated and provided through the ESA Space Weather (SWE) Service Network (https://swe.ssa.esa.int/noahesperia-federated) under the Space Radiation Expert Service Center (R-ESC). A recent, international collaboration between partners, with complementary expertise on particles and radio data resulted, in an innovative upgrade, namely HESPERIA REleASE+. The new implementation uses the novel approach of combining for the first time real-time Type III solar radio burst observations by the STEREO S/WAVES instrument, as clear evidence of particle escape from the Sun, within the HESPERIA REleASE system. To this end, a robust automated algorithm has been developed for identification of Type III radio bursts and their qualification as a precondition for intense SEP events at Earth’s orbit. This new implementation, HESPERIA REleASE+, leads to a substantial step forward in improving the accuracy of the tool and reduction of false alarms.
Author(s): Clive Dyer, Keith Ryden, Fan Lei, Ben Clewer, Fraser Baird
CSDRadConsultancy & University of Surrey Space Centre; University of Surrey Space Centre; University of Surrey Space Centre; University of Surrey Space Centre; University of Surrey Space Centre
Abstract: High energy protons (> 300 MeV) from galactic cosmic rays (GCRs) and very energetic solar particle events interact with atmospheric molecules to produce a radiation field extending throughout the atmosphere and some distance below ground. The former have been known and studied since 1912, while the latter were first detected in 1942 and have become known as Ground Level Enhancements (GLEs). The galactic cosmic rays are modulated slowly by the solar cycle with occasional rapid decline and recovery (Forbush Decreases) caused by Coronal Mass Ejections. The GLEs now number 74 and have short timescales with some risetimes less than 1 minute and decay times from hours to days.
The record GLE since 1942 occurred on 23rd February 1956 (Feb56) when an increase of 4500% was observed at the Leeds (UK) ground level neutron monitor. There are now some 5 five historic events confirmed from cosmogenic nuclides in tree rings and ice cores and ranging from 10xFeb56 to 100xFeb56.
The radiation field can give single event effects (SEEs) in human cells, leading to increased cancer risks, and in microelectronics, leading to effects ranging from bit-flips to burnouts. The need to control human exposure and malfunctions in avionics has led to several attempts to provide scales and warning levels as well as standards for the design of avionics. There is a key need for international collaboration and consistency. The SWPC S-scale for 10 MeV protons is at too low an energy for this. Both the D-scale and the recent ICAO levels are formulated around effective dose to humans and there is a further need to consider electronics.
In 2017 we suggested a scale based on the Feb56 event and multiples/fractions thereof. A probability distribution was generated using data from 71 GLEs and 2 cosmogenic events. Since then, the Oulu team and others have added further historic events to the distribution and have confirmed that scaling from NM events is indeed a good first order approach. We propose an atmospheric radiation scale (AR) to bring this knowledge together and provide a widely understood alert system. On this scale AR1 would correspond to ICAO MOD, occurring approximately once per year, and AR2 would match ICAO SEV and maybe re-occur every 3 years. AR5 would be at Feb56 level (1 per 50 to 70 years), potentially giving 20 mSv in TransAtlantic flight. Further details of corresponding effective dose and SEE rates will be given in the talk.
Standards for avionics (IEC 62396) and safety critical ground systems (JESD89) need further development and enforcement to enable risk to be assessed and proportionate response initiated. This wide programme must include model comparisons, continuous flights of radiation monitors and extension of the ground level neutron monitor networks (classical, mini and COSMOS) in order to allow for the early stage anisotropies present in many GLEs.
Author(s): Chi Wang, Jiyao Xu, Hui Li
National Space Science Center, CAS; National Space Science Center, CAS; National Space Science Center, CAS
Abstract: Monitoring and investigating the solar-terrestrial space environment is a huge challenge for humans in the space age. To this end, China has established the Ground-based Space Environment Monitoring Network, namely the Chinese Meridian Project (CMP). The project comprises three major systems: The Space Environment Monitoring System, the Data and Communication System, and the Scientific Application System. The Space Environment Monitoring System adopts a well-designed monitoring architecture, known as “One Chain, Three Networks, and Four Focuses”, to achieve stereoscopic and comprehensive monitoring of the entire solar-terrestrial space. The “One-Chain” component utilizes optical, radio, interplanetary scintillation, and cosmic ray instruments to cover the causal chain of space weather disturbances from the solar surface to near-Earth space. For the ionosphere, middle and upper atmosphere, and magnetic field, instruments are deployed along longitudes of 120°E and 100°E, and latitudes of 30°N and 40°N, forming the “Three Networks”.
Furthermore, more powerful monitoring facilities or large-scale instruments have been deployed in four key regions: the high-latitude polar region, the mid-latitude region in northern China, the low-latitude region at Hainan Island, and the Tibet region. These four regions are crucial for disturbances propagation and evolution or possess unique geographical and topographical characteristics. The Data and Communication System and Scientific Application System are designed for data collecting, processing, storage, mining, and providing user service based on data acquired by the Space Environment Monitoring System. The data obtained by CMP will be shared with the global scientific community, facilitating enhanced collaboration on space weather and space physics research.
In addition, the CMP provides a robust foundation for the International Meridian Circle Program (IMCP). IMCP will integrate and build a comprehensive ground-based monitoring network along 120°E-60°W meridian circle, to track the propagation of space weather events from the sun to the earth, and its evolution in geospace. Currently, we have built the IMCP headquarters building in Beijing. Additionally, construction is ongoing for further regional networks to monitor the ionosphere and the middle and upper atmosphere.
Author(s): Ligia Da Silva, Jiankui Shi, Livia R. Alves, Oleksiy Agapitov, Luis Eduardo A. Vieira, Laysa C. A. Resende, David Sibeck, Joaquim E. R. Costa, José Paulo Marchezi, Hui Li, Sony S. Chen, Zhengkuan Liu
China-Brazil Joint Laboratory for Space Weather – National Institute for Space Research; State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences; National Institute for Space Research – INPE; University of California, Berkeley – UCB – Space Sciences Laboratory; National Institute for Space Research – INPE; China-Brazil Joint Laboratory for Space Weather – National Institute for Space Research; NASA Goddard Space Flight Center; National Institute for Space Research – INPE; Department of Physics and Astronomy, University of New Hampshire; State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences; National Institute for Space Research – INPE; State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences
Abstract: The dynamics of the Earth’s inner radiation belt directly affect the atmosphere’s ionization level through the low-energy Electron Precipitation (EP- tens of keV to cents of keV), specifically over the South American Magnetic Anomaly (SAMA) region. This behavior makes this low latitude region to be considered as peculiar, presenting characteristics similar to auroral regions, such as the generation of the sporadic auroral-type E layer in the D region, increasing odd hydrogen (HOx) and odd nitrogen (NOx) in the mesosphere/stratosphere, and consequently decreasing the ozone over the center of the SAMA region. Additionally, electrons and protons trapped in the inner belt or precipitating over SAMA can impact the circuits on board the satellites, causing Single Event Upset (SEU – protons) and Deep Dielectric Charging (DDC – electrons), with higher frequency over the SAMA, when compared to other regions over the globe. The impact on human health on board aircraft in this region still needs to be better understood, as contradictory results are presented in the literature. However, some precautions should be considered when estimating the Effective Dose over this region, such as the models’ initial conditions (neutron detection). It is important to emphasize that in situ measurements (inner belt) and those precipitating over the SAMA region are generally contaminated by protons, making it difficult to perfectly quantify the dynamics related to each impact. Therefore, we have proposed a project to Brazilian agencies, named Project Particles (Charged Particles Trapped in the Inner Radiation Belt and Precipitated Locally over South America). This project aims to be developed by the Brazilian radiation belts team in collaboration with researchers from NASA’s Goddard Space Flight Center and UC Berkeley. The proposal has three phases: (Phase 1) Balloon Campaigns (x-ray detector); (Phase 2) Development of a conceptual model of detector prototype; (Phase 3) CubeSat missions (electron/proton detector). Their results aim to address several open questions regarding the dynamics of the inner radiation belt and the safety of the space environment over the SAMA region.
Author(s): Laysa C. A. Resende, Y. Zhu, C. M. Denardini, R. A. J. Chagas, L. A. Da Silva, S. Chen, J. Moro, J. E. R. Costa, L. R. Alves, H. Li, C. Wang, Z. Liu
State Key Laboratory of Space Weather (CBJLSW)/ National Institute for Space Research (INPE); State Key Laboratory of Space Weather/3University of Chinese Academy of Sciences; National Institute for Space Research (INPE); National Institute for Space Research (INPE); State Key Laboratory of Space Weather (CBJLSW)/ National Institute for Space Research (INPE); National Institute for Space Research (INPE); State Key Laboratory of Space Weather (CBJLSW)/ National Institute for Space Research (INPE); National Institute for Space Research (INPE); National Institute for Space Research (INPE); State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences; State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences.; State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences.
Abstract: Sporadic E layers (Es) are electron density increments located at 100-150 km in the ionosphere, composed mainly of metallic ions, such as Fe+, Mg+, Na+, K+, and Si+. The presence of strong Es layers can negatively impact technological systems and the aviation sector by disrupting radio communication systems. Therefore, we present a study on the atypical and widespread Sporadic E-layers (Es) observed in digisonde data during both quiet times and space weather events. In fact, we analyzed a set of days over Cachoeira Paulista (CXP, 22.41°S, 45°W, dip ~35°), that caused an increment in the Es layers. Such inhomogeneous Es layer is associated with the auroral-type Es layer (Esa) occurrence in this low latitude due to the electron precipitation over the South American Magnetic Anomaly (SAMA) region. However, we also observe that the spreading Es layers occurring days before magnetic storms or during quiet times can also affect technological systems. We used additional data from imagers, satellites, meteor radars, and models to understand the dynamic processes involved in the formation of these Es layers. We show evidence that the instabilities added to the wind shear mechanism, such as Kelvin-Helmholtz instability (KHI), and particle precipitation mechanism due to the SAMA can cause strong and atypical Es layers, modifying the usual dynamics of the low-altitude ionosphere. An important discovery of this work is that the spreading Es layer, mainly during quiet times, is not necessarily due to the presence of particle precipitation over the SAMA. We found that wind shear can be turbulent, influencing the development of the Es layer. Our analysis provides a better understanding of Es layer behavior during both quiet and disturbed times.
Author(s): Drew L. Turner
Johns Hopkins Applied Physics Laboratory
Abstract: On 8-9 May, 2024, The Johns Hopkins Applied Physics Laboratory conducted the first-ever tabletop exercise (TTX) for the United States government (local to federal levels) to evaluate the full government response to a series of space weather events and impacts. The TTX was sponsored by NASA, NOAA, NSF, and FEMA, and participants included top-level representatives and decision-makers from those agencies plus over 30 other local, state, and federal departments and agencies across the US government. The exercise consisted of participants working through a hypothetical scenario in which a series of solar eruptions result in a range of space weather impacts on systems ranging from astronauts on the Moon to public, commercial, and government communications and navigation disruptions and power infrastructure. In this presentation, we provide an overview of the exercise and its objectives, the space weather scenario used in the exercise, and some of the major lessons learned and outcomes of the exercise itself. Quite serendipitously, the exercise was held on the same day as the solar eruptive events that triggered the 10th of May geomagnetic superstorm (G5 level) that received so much public and media attention. We also put the scenario exercise into context with that actual series of events and detail our preparedness for mitigating the negative impacts of space weather on our infrastructure and society.
P1-p16 Solar Activity Monitor Network (SAMNet) - Next step in ground-based Space Weather forecasting
Author(s): Robertus Erdelyi
SP2RC/U of Sheffield
Abstract: Space Weather storms, in the forms of e.g. flares and Coronal Mass Ejections (CMEs), are one of the greatest risks to our technosphere. The question is not anymore “whether” but “when” a large solar eruption may disrupt the functioning of our technology-driven socio-economic system. Therefore we need to develop a suitable and accurate warning system that can reliable predict these larges eruptions in our Solar System. This is a great challenge and there may be various solutions. Here, I will report one: The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet).
SAMNet is a UK-lead international consortium of ground-based solar telescope stations. SAMNet, at its full capacity, will continuously monitor the intensity, LoS component of magnetic and Doppler velocity fields at multiple heights in the lower solar atmosphere (LSA), i.e. from the photosphere to the upper chromosphere. The solar activity magnetic monitor (SAMM) sentinels with identical telescopes equipped with magneto-optical filter (MOFs) may take observations in K~I and Na~D spectral bands.
The objectives of SAMNet are i) to cater LoS magnetic and Doppler data for space weather research and ii) forecast. The goal is to achieve an operationally sufficient lead time of e.g. flare warning of up to 24 hours, and provide much sought-after continuous synoptic maps (e.g., LoS magnetic and velocity fields, intensity) of the lower solar atmosphere with spatial resolution limited only by seeing with a cadence of 10-min. The individual SAMM sentinels link into their master HQ hub at Gyula Bay Zoltan Solar Observatory (GSO) where data received from all the slave stations are processed and flare warning is issued up to 38 hrs in advance. We present briefly the MOF concept, the science behind forecasting with SAMNet data and show the superb first-light images. We also discuss why such a ground-based system may complement reliable and very economically space-borne instrumentation and the associated data.
Author(s): Jussi Lehti, Deepa Anantha Raman, Osku Raukunen, Pasi Virtanen, Tero Säntti, Mika Hirvonen, Philipp Oleynik
ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy); ASRO (Aboa Space Research Oy)
Abstract: Space weather, driven by dynamic solar activities, poses significant challenges for global technological systems. The increasing number of satellite launches and the New Space approach of using commercial-off-the-shelf (COTS) components underscore the critical need for improved radiation monitoring. Furthermore, traditional space research organisations such as NASA, ESA, and NOAA are increasing the procurement of commercial data and international cooperation. Advanced artificial intelligence and machine learning models, which benefit from vast amounts of high-quality data, further highlight the importance of comprehensive space weather measurement capability.
Are these dramatic changes leading to a paradigm shift in space weather monitoring globally? Can we anticipate a similar trend in the space weather ecosystem as seen in the Earth Observation (EO) market? What new business models and strategies can contribute to this?
The traditional space weather ecosystem needs additional support to respond to these dramatic changes. Private companies with agile methods and new business models can support a global approach to space weather monitoring through novel solutions. By building international partnerships, the aim is to increase data sharing and cooperation, speed up development times, and improve our understanding of space weather impacts.
Finnish space technology company ASRO (Aboa Space Research Oy), with long-standing expertise in radiation instruments, addresses the shortage of readily available solutions for space applications, offering state-of-the-art instruments tailored for space weather applications. ASRO actively engages in international collaborations to enhance global space weather monitoring by filling gaps and complementing existing infrastructure. This is achieved through ASRO’s innovative radiation monitor family designed to provide science-grade instrumentation for commercial applications.
The radiation monitor family includes the Relativistic Electron and Proton Experiment (REPE), the Miniaturized Instrument for Radiation Analysis (MIRA), the Flare Examination and Lookout in X-ray (FELIX), and the Low Energy Electron Vigilance Instrument (LEEVI). With flight-proven heritage, these instruments are adaptable, affordable, and rapidly deployable across diverse mission architectures, from Low Earth Orbit (LEO) to higher orbits. Furthermore, simulated instrument data can be provided to facilitate rapid mission planning in new space applications.
By showcasing ASRO’s advancements and partnerships, we aim to stimulate further collaboration, reduce redundancy, and optimise the use of resources in the global space weather monitoring community. Through coordinated efforts, we can enhance our collective ability to predict and mitigate the impacts of space weather, ensuring the protection and resilience of technological systems that underpin modern society.
Author(s): Dimitrios Vassiliadis, Steven Hill, Laurel Rachmeler, Jeff Johnson, William Rowland, Nazila Merati, Jacob Inskeep, Matthew Devaney, Christopher Pagan, James Marshall
NOAA/NESDIS/Space Weather Observations; NOAA/NWS/SWPC; NOAA/NESDIS/NCEI; NOAA/NWS/SWPC; NOAA/NESDIS/NCEI; NOAA/NESDIS/NCEI; NOAA/NESDIS/SWO; NOAA/NESDIS/SWO; NOAA/NESDIS/NCEI; NOAA/NESDIS/SWO
Abstract: The primary objective of Space Weather Follow On (SWFO) Program is to provide operational solar-coronal images and in situ solar-wind data to the Space Weather Prediction Center (SWPC) forecasters and to other users. The first data are expected from the Compact Coronagraph 1 (CCOR-1) which will operate on board the GOES-U geostationary satellite scheduled to be launched on June 25, 2024. First images will be obtained and processed during the Post-Launch Testing (PLT) phase which is scheduled to last from September to December 2024. A second coronagraph (CCOR-2) and several in situ instruments are part of the SWFO-L1 mission which will be placed in orbit around Lagrange 1 (L1) in 2025. This talk will provide an overview of the operational and science goals for the Program. The SWFO data products will be described, including types and levels, formats, latency, and documentation. The talk will present types of access to the data including the Space Weather Portal that the National Centers for Environmental Information (NCEI) have developed for SWFO and other NOAA space weather missions. An important objective is the comparison with other missions observing the Sun such as SOHO, STEREO, SDO, Solar Orbiter, and GOES-R; and missions in orbit around L1 such as ACE, WIND, DSCOVR, Aditya-L1, and IMAP. Such comparisons will focus on coronal phenomena including CMEs, and on the 3D structure and evolution of solar wind transient structures, and will enable instrument intercalibration.
Author(s): Christine Verbeke, M. Petrenko, A. Isavnin, M.L. Mays, C. Wiegand, M. Kuznetsova, S. Poedts, P. Jiggens, NASA CCMC team, VSWMC team
KU Leuven / NASA GSFC; NASA GSFC; Rays of Space; NASA GSFC; NASA GSFC; NASA GSFC; KU Leuven; ESA; NASA CCMC team; VSWMC team
Abstract: Modern heliophysics models and coupled modelling frameworks are important instruments in heliophysics research and space weather forecasting. Despite the increasing adoption of the ideas and principles of open science in the community, utilising of the models requires ever-growing computational resources and expertise, effectively putting them out of reach of many users.
Several heliophysics modelling centres were established to facilitate research and mitigate the high cost of entry. Two of these centres are the Coordinated Community Modelling Centre (CCMC) at NASA Goddard Space Flight Center and the Virtual Space Weather Modelling Centre (VSWMC) at ESA. They host some of the most cutting-edge models and provide guided services in running the models, and interpreting and archiving the results of the runs. While both centres provide similar services, maintaining close contact is important to serve our heliophysics community and needs best.
This talk will give an overview of the CCMC and VSWMC services. Furthermore, we provide an overview of the successes and challenges of interconnecting simulation services, run results archives and opportunities for the future.
Author(s): Dario Del Moro, Monica Laurenza, Anna Milillo, Alberto Bigazzi, Christina Plainaki, Giuseppe Sindoni, Marco Giardino, Gianluca Polenta
University of Rome Tor Vergata; INAF-IAPS; INAF-IAPS; Italian Space Agency; Italian Space Agency; Italian Space Agency; Italian Space Agency; Italian Space Agency
Abstract: The prototype of the scientific data centre for Space Weather of the Italian Space Agency (ASI) called ASPIS (ASI SPace Weather InfraStructure) has been recently developed and validated by the CAESAR (Comprehensive Space Weather Studies for the ASPIS prototype Realization) project.
The ASPIS prototype unifies multiple Space Weather (SWE) resources through a flexible and adaptable architecture to allow scientists to perform studies across the SWE-related fields, e.g., adopting an integrated approach, encompassing the whole chain of phenomena from the Sun to the Earth up to planetary environments or parts of it.
This work presents the challenges and the first results of creating the ASPIS prototype. The database handles the heterogeneity of metadata and data while storing and managing the interconnections of various space weather events. The pilot database is complete, and user interfaces, including a graphical web interface and an advanced Python module called ASPISpy, have been developed to facilitate data discovery, access, and analysis
Author(s): Jim Spann
NOAA
Abstract: This talk and subsequent discussion is centered on the need and characteristics, including membership and scope, of a coordinating body for those agencies that fund space weather applied investigations and space weather research missions. This body would provide a forum to share plans and foster discussions leading to possible collaborations that advance understanding and enable progress of space weather operations and applications. This would not be a decisional body and it would complement, not replace, the current space weather operational coordination groups.
Author(s): Barbara Matyjasiak, Hanna Rothkaehl, Mariusz Pożoga, Marcin Grzesiak, Łukasz Tomasik, Dorota Przepiórka, PITHIA-NRF Consortium
Space Research Center of the Polish Academy of Sciences; Space Research Center of the Polish Academy of Sciences; Space Research Center of the Polish Academy of Sciences; Space Research Center of the Polish Academy of Sciences; Space Research Center of the Polish Academy of Sciences; Space Research Center of the Polish Academy of Sciences; https://pithia-nrf.eu/pithia-nrf-developers/consortium/members
Abstract: PITHIA-NRF aims to create a European-wide distributed network that integrates observing facilities, data processing tools, and models focused on ionosphere, thermosphere, and plasmasphere research. The project seeks to unify and provide access to key national and regional research infrastructures in Europe, including EISCAT, LOFAR, Ionosondes and Digisondes, GNSS receivers, Doppler sounding systems, riometers, and VLF receivers. These comprehensive resources are accessible to scientific and private sector users, enabling them to collaboratively exploit the data collected from the network’s research infrastructures.
PITHIA-NRF, through its Innovation Platform, has an ambition to act as a catalyst for innovation, bridging the gap between research and application. By providing effective access to Europe’s key research facilities (nodes), PITHIA-NRF facilitates scientific collaboration and knowledge exchange among academia, Small and Medium Enterprises (SMEs), large companies, and public organisations. In the Transnational Access (TNA) program, subsidised access is granted to external research teams, enabling them to conduct projects within PITHIA-NRF nodes. This access empowers teams to gain hands-on experience in operating observing facilities from campaign setup to data collection, analysis, and utilisation, leveraging the project’s tools and services.
This work presents the PITHIA-NRF innovation activities.
Author(s): Kyung-Suk Cho
KASI
Abstract: The Sun-Earth Lagrange point L4 is considered as one of the unique places where the solar activity and heliospheric environment can be observed in a continuous and comprehensive manner. The L4 mission affords a clear and wide-angle view of the Sun-Earth line for the study of the Sun-Earth and Sun-Moon connections from the perspective of remote-sensing observations. In-situ measurements of the solar radiation, solar wind, and heliospheric magnetic field are critical components necessary for monitoring and forecasting the radiation environment as it relates to the issue of safe human exploration of the Moon and Mars. A dust detector on the ram side of the spacecraft allows for an unprecedented detection of local dust and its interactions with the heliosphere. The purpose of this talk is to emphasize the importance of L4 observations as well as to outline a strategy for the planned L4 mission with remote and in-situ payloads onboard a Korean spacecraft. It is expected that the Korea-lead L4 mission can significantly contribute to improving the space weather forecasting capability by enhancing the understanding of the heliosphere through comprehensive and coordinated observations of the heliosphere at multi-points with other existing or planned L1 and L5 missions.
Author(s): Jussi Lehti, Deepa Anantha Raman, Osku Raukunen, Pasi Virtanen, Mika Hirvonen, Tero Säntti, Philipp Oleynik, Rami Vainio, Davide Calcagno, Davide Monferrini, Monica Laurenza, Maria Federica Marcucci, Stefano Cicalò
ASRO (Aboa Space Research Oy), Turku, Finland; ASRO (Aboa Space Research Oy), Turku, Finland; ASRO (Aboa Space Research Oy), Turku, Finland; ASRO (Aboa Space Research Oy), Turku, Finland; ASRO (Aboa Space Research Oy), Turku, Finland; ASRO (Aboa Space Research Oy), Turku, Finland; University of Turku, Turku, Finland; University of Turku, Turku, Finland; ARGOTEC, Torino, Italy; ARGOTEC, Torino, Italy; INAF, IAPS, Roma, Italy; INAF, IAPS, Roma, Italy; SpaceDyc, Pisa, Italy
Abstract: The need for reliable and cost-effective monitoring of Space Weather has grown significantly with the increasing reliance on satellites, space missions, and global communication networks. Aboa Space Research Oy (ASRO) introduces the Relativistic Electron and Proton Experiment (REPE), an advanced particle radiation monitoring instrument for a wide range of missions and space weather applications.
REPE is a compact energetic particle instrument, initially conceptualised for studying the Van Allen belts. The original development was undertaken for the nanosatellite mission (Foresail-2) as a collaborative effort between University of Turku (UTU) and ASRO. REPE measures electrons within 0.2 – 5 MeV and protons within 2 – 100+ MeV energy range using a stack of three silicon detectors and a scintillator with photodiode readout. The chosen configuration enables adaptability to different energy ranges. The instrument is well-suited for scientific missions in Low Earth Orbit (LEO), high Earth orbits and beyond.
REPE will be a part of the scientific payload of The HEliospheric pioNeer for sOlar and interplanetary threats defeNce (HENON) 12-unit CubeSat mission developed by a consortium led by Argotec under European Space Agency contracts within the General Support Technology Programme.
HENON aims to provide timely alerts of potentially harmful Space Weather phenomena. In addition to REPE, HENON will carry the Faraday Cup Analyzer (FCA) for measuring the integrated energy distribution of solar wind ions, and the MAGnetometer from Imperial College (MAGIC) for measuring the magnetic field.
The HENON mission will fly in the previously unexplored Distant Retrograde Orbit (DRO), in the Sun-Earth binary system, in which it will remain upstream of the Earth, further than L1, for extended periods of time, making it possible to provide Space Weather alerts with significantly increased warning times. Furthermore, the mission will provide an important demonstration of reliable use of CubeSat technologies in deep space.