Session P3 - Multi-techniques to monitor the Sun and solar wind for space weather
Stephan G. Heinemann, onsite (Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany), Eleanna Asvestari, onsite (University of Helsinki, Helsinki, Finland), Camilla Scolini, onsite (Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, US)
Interplanetary coronal mass ejections, interplanetary shocks, stream and co-rotating interaction regions (SIRs/CIRs) and high speed solar wind streams are the primary drivers of strong to minor geomagnetic activity and play a major role in shaping the heliospheric environment in which they propagate. Therefore, understanding the heliospheric solar wind, ambient magnetic field, and their solar sources are vital in validating and refining space weather forecasting efforts. The aim of this session is to address the characteristics of these flows, the heliospheric background solar wind structure in which they propagate with respect to their solar source regions through the means of observations and models. Newly launched missions including Parker Solar Probe (PSP) and Solar Orbiter (SolO), as well as, established missions such as the Solar Dynamics Observatory (SDO) and the Solar Terrestrial Relations Observatories (STEREOs) provide a multitude of information that may be used to validate, improve, and refine current knowledge in this field. We encourage submissions relating to solar wind sources both for slow and fast wind, solar wind acceleration/ejection, interplanetary coronal mass ejections and shocks, stream interaction, and the structure of the magnetic field and plasma topology at the source surface and in the inner heliosphere. We advocate for authors to present their work that utilizes observations and/or models with relation to space weather.
Thursday October 27, 08:30 - 13:30, Poster AreaTalks
Thursday October 27, 08:45 - 10:15, Water HallClick here to toggle abstract display in the schedule
Talks : Time scheduleThursday October 27, 08:45 - 10:15, Water Hall
|08:45||Connecting the Observed Solar Wind to its Solar Origin||Wallace, S et al.||Invited Oral|
| ||Samantha Wallace, Charles N. Arge, Nicholeen M. Viall, Shaela Jones[3,2], Carl Henny|
| ||NASA Postdoctoral Program / GFSC; NASA/GSFC; Catholic University of America; Air Force Research Laboratory|
| ||Several fundamental outstanding questions in heliophysics pertain to the genesis and energization of the solar wind – both of which are driven by physical processes that largely occur in the solar atmosphere. Recent missions (i.e. SolO, PSP), alongside existing ground and space-based observatories provide an unprecedented multi-vantage-point view of the corona, pristine solar wind, and inner heliosphere. However, advancing our understanding of how the solar wind is formed and energized hinges on our ability to connect in situ solar wind observations back to their solar source observed remotely. In this talk, I will motivate the importance of establishing this connection to improve space weather forecasting, review the various techniques used in our community to do so, and discuss the uncertainties and limitations of each method. I will also discuss my own work using the Wang-Sheeley-Arge (WSA) model driven by Air Force Data Assimilative Photospheric Flux Transport (ADAPT) time-dependent photospheric field maps to connect in situ solar wind observations from various spacecraft (e.g. PSP, Helios, L1 monitors) to their source regions at 1 Rs. I will present results in which we apply our modeling approach to test solar wind formation theories (e.g. reconnection/S-web, waves-turbulence, expansion factor), and to characterize the solar wind from specific sources (e.g. active region vs. quiet Sun coronal hole boundaries, deep inside coronal holes).|
|09:10||Helioseismic far-side imaging: An empirical approach to model active-region magnetic fields||Yang, D et al.||Oral|
| ||Dan Yang and Stephan G.Heinemann|
| ||Max planck institute for solar system research, 37077 Göttingen, Germany|
| ||Synchronic magnetograms of the Sun’s full surface are an important boundary condition for modeling large-scale heliospheric magnetic fields and subsequent real-time space weather forecasts. So far, SO/PHI is the only instrument that measures magnetic fields on the solar far side, however, this is not done on a daily basis. In practice, far-side magnetic fields are modeled by applying surface flux transport models to magnetograms on the Earth side to simulate the behavior of the magnetic field on the far side (e.g., ADAPT magnetograms). As a consequence, active regions which emerged on the far side will not be included in the models until they rotate to the Earth side. Helioseismology can be used to detect the emergence of active regions on the far side and track their signatures until they appear on the Earth side by using the solar 5-min oscillations. Furthermore, far-side seismic signals are found to be correlated with strong magnetic fields, which means they have the potential to fill the missing active regions in the magnetograms. In this talk, we will explain how helioseismology can be used to detect active regions on the far side, and show an empirical approach to convert state-of-the-art seismic measurements into magnetic fields. Example synchronic magnetograms will be presented by inserting converted active-region magnetic fields into a surface flux transport model based on SDO/HMI line-of-sight magnetograms.|
|09:25||Solar wind acceleration at the inner Heliosphere ||Larrodera, C et al.||Oral|
| ||C. Larrodera, C. Cid, M. Flores-Soriano |
| ||University of Alcalá|
| ||Space weather forecasting requires accurate modelling of the background solar wind. Up to date, propagation models assume that the solar wind flows at a constant speed from a specific distance to the Sun. We have analyzed how the solar wind distribution function evolves between 16 and 172 solar radii using in-situ measurements from the Parker Solar Probe. Our results suggest that the solar wind is accelerated until at least 60 solar radii, further away than assumed in space weather modelling.|
|09:40||Studying dynamics of the fast solar wind, through observations and modelling||Magdalenic, J et al.||Oral|
| ||Jasmina Magdalenic ,, Senthamizh Pavai Valliappan , Luciano Rodriguez |
| || Royal Observatory of Belgium, Belgium;  Katholieke Universiteit Leuven, Belgium|
| ||The dynamics and variability of the solar wind has been actively studied for decades, employing both modelling and observations. However, majority of studies were up to now limited to the distances of about 1 AU, at which the in situ observations of solar wind characteristics were up to now routinely taken. The recently available Parker Solar Probe (PSP) observations provide us the unique possibility to study the solar wind characteristics in the low solar corona, at distances of only few tens of solar radii. The first few perihelion passes of the PSP reveal the highly variable structure of both, fast and slow solar wind, indicating that the solar wind characteristics are indeed strongly changing as the wind propagates away from the Sun.
In this study, we compare the characteristics of the fast solar wind observed by the PSP with the characteristics of the solar wind flows observed at Earth. As the accent is put on the solar wind characteristics originating from the small coronal holes, we have employed a magnetic connectivity tool (developed by ESA’s MADAWG group) to associate the solar wind observed by the PSP with their source regions on the Sun. Our first results indicate that we can well distinguish and identify the solar wind observed by the PSP originating not only from the big, but also from the small coronal holes. After that, we looked for the corresponding fast solar wind in situ at 1 AU. The observations were confronted with the solar wind characteristics modelled by the 3D MHD model EUHFORIA. We discuss how the observed and modelled characteristics of the solar wind close to the Sun compare with the solar wind characteristics observed at 1 AU. |
|09:55||WHPI: Recent campaigns and future opportunities||Hofmeister, S et al.||Oral|
| ||Stefan J. Hofmeister for the WHPI team|
| ||Leibniz Institute for Astrophysics Potsdam|
| ||The current availability of new satellites and instrumentation, be it Parker Solar Probe, Solar Orbiter, or DKIST, offers great opportunities to advance our current understanding of the Sun-Earth system within the heliosphere. Modelling these systems involves collaboration and coordination of many scientific communities. The Whole Heliosphere and Interplanetary Interaction initiative serves as a framework for coordinating the efforts of the various communities for scientific purposes and organizes large-scale campaigns. I will give a short overview over the recent campaigns, future plans, and how one can become active within the WHPI initiative. In particular, we plan to organize a Grand Challenge together with the magnetospheric community, trying to model the Sun-Earth connection and the heliosphere for a specific time interval to the best of our efforts. We welcome every scientist to join the effort to test our current understanding of the heliosphere and to identify open issues.
|1||LDE3's weekly Solar Orbiter/STIX flare bulletin||Pinto, R et al.||Poster|
| ||R. F. Pinto, A. Finley, B. Perri, A. Strugarek, A. S. Brun|
| || LDE3, Université Paris-Saclay, CEA, France|
| ||We present the weekly Solar Orbiter/STIX flare bulletin that is being produced continuously since early 2021, following the start of the continued operation of the STIX instrument. The bulletin provides systematic monitoring of the flare activity as observed from Solar Orbiter's vantage point, put in relation with many other relevant instruments (on SO, but also on PSP, SoHO, SDO, STEREO, Hinode, etc), as well as other solar observation services. The bulletin highlights pertinent connections between the observed events and space weather phenomena, while keeping track of the long term trends of solar activity.
The bulletin is supported by a set of automated tools developed at the LDE3 that aim at providing continuous monitoring of flaring activity as complete as possible in terms of temporal cadence and longitudinal coverage of the surface of the Sun (e.g, Earth-bound and farside). Quick flare amplitude and location estimates are provided systematically.
Finally, the bulletin is currently distributed through a mailing list open to all interested parties.|
|2||Spatial distribution and survival rate of magnetosheath jets during CMEs, SIRs, and HSSs.||Weiss, S et al.||Poster|
| ||Stefan Weiss , Florian Koller , Manuela Temmer , Adrian T. LaMoury , Owen W. Roberts , Ferdinand Plaschke , Luis Preisser |
| || Institute of Physics, University of Graz, Austria  The Blackett Laboratory, Imperial College London, London, UK  Space Research Institute, Austrian Academy of Sciences, Graz, Austria  Institut für Geophysik und extraterrestrische Physik, TU Braunschweig, Germany|
| ||The dayside magnetosheath and magnetosphere of the Earth are fundamentally influenced by large-scale solar wind (SW) structures like coronal mass ejections (CMEs), stream interaction regions (SIRs) and high speed streams (HSSs). The SW plasma impinging on the terrestrial bow shock often generates dynamic pressure enhancements in the magnetosheath, which we call jets. The majority of jets are caused by processes at the quasi-parallel shock and start to dissipate while they travel through the magnetosheath. Long-lived jets may travel anti-sunward through the entire magnetosheath where they further impact Earth’s magnetopause and become geoeffective. Incoming large-scale SW structures profoundly affect the conditions that govern jet generation and the state of the magnetosheath plasma through which jets propagate. We investigate, how jet location and “survival rate”, i.e., the likelihood of them reaching the magnetopause, are influenced by CMEs, SIRs, and HSSs. We use upstream solar wind data from OMNI and magnetosheath data from the THEMIS spacecraft as well as a collection of lists of large-scale solar wind structures in the time range of 2008 – 2021, having a total of 51,737 jets that were detected using the criterion of Archer and Horbury (2013). The three-dimensional bow shock model from Merka et al. (2005) and the magnetopause model from Shue et al. (1998) are used to determine the position of jets within the magnetosheath. The statistical analysis relating jet locations and characteristics during each type of large-scale SW event will give a better understanding of their origin and propagation, hence, identifying potential Space Weather events.|
|3||A revised version of the Empirical Solar Wind Forecast (ESWF) model||Temmer, M et al.||Poster|
| ||D. Milošić, M. Temmer, S.G. Heinemann, T. Podladchikova, A. Veronig, B. Vršnak|
| ||Institute of Physics, University of Graz, Austria; Max-Planck-Institut für Sonnensystemforschung, 37077 Goettingen, Germany; Skolkovo Institute of Science and Technology, Bolshoy Boulevard 30, bld. 1, 121205, Moscow, Russia; Hvar Observatory, Faculty of Geodesy, University of Zagreb, Croatia|
| ||The empirical solar wind forecast (ESWF) model uses a simple empirical relation to forecast from the fractional area of coronal holes (CHs) in meridional slices measured at the Sun, the solar wind speed at 1 AU. It currently runs as ESA Space Safety service in the Heliospheric-Weather Expert Service Center. The “CH area-SW speed” relation was improved over the years in several steps, but still has the drawback that Gaussian type speed profiles are produced as the CH rotates in and out of the meridional slice. We present next development steps to ESWF, implementing compression and rarefaction effects occurring between SW streams of different velocities in interplanetary space. We show with a statistical analysis in the period 2012 - 2021 that our adaptions improve the ability to predict HSS speed profiles as well as smaller structures with higher precision. In addition, we also present first steps towards a robust Dst forecast, using CH areas and their magnetic field information. |
|5||Mapping the coronal plasma density using type III radio bursts, Parker Solar Probe observations and modeling with EUHFORIA||Deshpande, K et al.||Poster|
| ||Ketaki Deshpande[1, 2], Jasmina Magdalenic[1, 2], Immanuel Christopher Jebraj[1, 2], Senthamizh Pavai Valliappan, Vratislav Krupar[3, 4]|
| ||Solar Terrestrial Center of Excellence, SIDC, Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Uccle, Belgium, Center for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium, Heliospheric Physics Laboratory, Heliophysics Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA, Goddard Planetary Heliophysics Institute, University of Maryland, Baltimore County, Baltimore, MD 21250, US.|
| || Solar wind plasma properties are dynamically changing with the increasing distance from the Sun. Mapping of the coronal plasma density is very important, as this is one of the main inputs to the solar wind and CME models. Until now, the validation of different methods for obtaining coronal plasma characteristics was possible only with the in-situ observations taken at distances close to 1 AU. The recently available Parker Solar Probe (PSP) observations provides the possibility to study the coronal plasma characteristics also at the distances close to the Sun.
The main focus of this study are type III radio bursts observed in the dynamic spectra as fast-drifting structures. Type III bursts are the signatures of the fast electron beams travelling along the open and quasi-open magnetic field lines. These fast beams provide us the information on acceleration of electron beams and characteristics of the environment through which they are propagating. The type III radio bursts are studied for decades, but we still do not fully understand how they propagate through the solar corona.
We present the study of four groups of type III radio bursts observed during the 2nd perihelion of PSP, on April 05, 2019. We employed the direction-finding observations from STEREO/Waves and WIND/Waves in order to obtain the 3D radio source positions and the electron density profiles. The obtained density profiles are compared with the in situ measurements of the PSP and the solar wind density simulated by the recently developed MHD model EUHFORIA (EUropean Heliospheric FORecasting Information Asset). The first results show somewhat overestimated densities obtained from the radio observations indicating that the electron beams might have propagated through the coronal regions of the higher density than usually observed.
The propagation path of the two pairs of subsequent type III radio bursts observed on April 05, indicate quite different propagation path, despite the same region of origin on the Sun.|
|6||HelioCast: A white light constrained MHD model for space weather forecast of the heliosphere||Réville, V et al.||Poster|
| ||Victor Réville, Alexis Rouillard, Nicolas Poirier, Athanasios Kouloumvakos, Rui Pinto, Naïs Fargette, Mikel Indurain|
| ||IRAP, Université Toulouse III - Paul Sabatier, CNRS, CNES, Toulouse; Département d'Astrophysique, AIM - CEA Saclay|
| ||Space weather operations and predictions rely on fast and inexpensive models of the solar corona derived from remote observations. They are usually based on photospheric measurements of the solar magnetic field. However, a precise description of all coronal physical processes needs a very large amount of computing power, notwithstanding the many uncertainties on solar magnetograms. In recent months, we have developed a new method to derive empirically coronal properties through the identification and the localization of the heliospheric current using white light observations from the SOHO/LASCO coronagraph. Wind velocities, magnetic field, and densities are derived at 0.1 AU and then propagated up to 1 AU with a 3D MHD model. In this talk, we present this novel method and its results in nowcasting and forecasting of the solar wind plasma parameters at 1 AU. We compare this novel method
with more comprehensive models for the coronal region: Multi-VP, which is a multiple 1D MHD model using a PFSS extrapolation for the magnetic field, and WindPredict-AW, a full 3D MHD model of the corona including the physics of Alfvén waves turbulence and dissipation. We validate the model during the first semester of 2018, during which many high speed streams have been observed at Earth. Finally, we propose paths to extend the method to more active phases of the solar cycle.|
|7||The Space Weather Follow On (SWFO) Product Generation and Distribution (PGD) element||Vassiliadis, D et al.||Poster|
| ||Dimitrios Vassiliadis (1), Ame Fox (1), Steven Hill (2), Jacob Inskeep (1), Jeff Johnson (2), Laurel Rachmeler (3), Rob Redmon (3), William Rowland (3)|
| ||(1) NOAA/NESDIS/OPPA, (2) NOAA/NWS/SWPC, (3) NOAA/NESDIS/NCEI|
| ||NOAA’s Space Weather Follow On (SWFO) program will focus on monitoring solar and solar-wind activity with the Compact Coronagraph (CCOR-1) hosted on the geostationary satellite GOES-U and the SWFO-Lagrange 1 (SWFO-L1) observatory. The two satellites are planned for launch in 2024 and 2025, respectively. The Ground Segment of the program contains the Product Generation and Distribution (PGD) element which is responsible for processing the raw imagery and in situ data and creating data products. These elements are made available to operational users at low latency and to retrospective users within 5 days. The data will be stored in the NOAA Common Cloud Framework (NCCF) and made available through the SWFO Science Center website. The presentation will discuss the data types, algorithm development, and other technical and programmatic information for this ground project.|
|8||Triangulating Solar Radio Bursts using Bayesian Methods||Canizares, L et al.||Poster|
| ||L Alberto Canizares ,, Peter T Gallagher , Eoin P Carley , Shane A Maloney |
| ||Dublin Institute of Advanced Studies, Ireland Trinity College Dublin, Ireland|
| ||Solar eruptive activity results in the expulsion of plasma and acceleration of particles. These energetic particles interact with the local plasma environment resulting in the generation of intense radio bursts known as solar radio bursts. Type III radio bursts are a particular type of solar radio burst attributed to electrons travelling along open magnetic field lines. When an electron travels along a magnetic field line, it will produce radio waves at the local plasma frequency which can then be detected from Earth. However, the acceleration mechanisms that eject these particles away from the Sun are not fully understood and are still subject to investigation. Tracking of these particles is usually performed by means of triangulating type III radio bursts observed by different spacecraft located in different positions around the inner solar system. However standard methods of triangulation are found to have large uncertainties. In this project, we investigate the use of bayesian statistics to obtain a probabilistic positional map of a type III radio burst (Cañizares et al (in prep)).|
|9||Status of the Space Weather Observatory and Services at the Royal Meteorological Institute of Belgium||Sapundjiev, D et al.||Poster|
| ||Danislav T. Sapundjiev Stanimir M. Stankov, Jean-Claude Jodogne|
| ||Royal Meteorological Institute of Belgium|
| ||Since its foundation in 1956 the Geophysical Centre (Le Centre de Physique du Globe (CPG)) of the Royal Meteorological Institute of Belgium is pursuing the mission to study and measure geophysical phenomena. It operates a standard 8-NM-64 Neutron Monitor for the monitoring of the cosmic rays activity, and measurements of the geomagnetic vector on a minute basis as well as and high cadence ionospheric soundings for the characterisation of the main ionospheric parameters are carried out. The centre is well known for its high quality data spanning long time periods.
Since 2012 the CPG was gradually increasing its research activities under the subject of Space Weather(SW) real-time data provision and development of models and services. During this period Several additional instruments were added to the initial infrastructure: two GNSS receivers for ionospheric monitoring of the total electron content and scintillations, a solar flare monitor (SuperSID) and a new modern neutron monitor was constructed. Several other projects and developments are underway - construction of a muon telescope to support the cosmic rays measurements as well as a feasibility and practical study for deployment of a network of soil moisture monitors based on neutron detectors - a project that will complement both the space- and atmospheric weather services.
In this presentation we will report the current status of the SW observatory at the CPG in Dourbes and will present the status of the SW services for now- and forecast with the focus on Ground Level Enhancement and Solar Particles predictions and Radiation Dose real-time nowcast over the BENELUX region.
|10||Assessment of the source surface neutral line as a predictor of the heliospheric current sheet crossings at 1 AU||Liou, K et al.||Poster|
| ||Kan Liou, and Chin-Chun Wu|
| ||Johns Hopkins University Applied Physics Laboratory; U.S. Naval Research Laboratory|
| ||The heliospheric current sheet (HCS), the largest solar wind structure in the heliosphere, plays an important role in space weather. It is a transition between a toward and an away interplanetary magnetic field sector, a pilot feature of co-rotating interaction regions and high-speed streams, and a source location of magnetic field reconnection. It also affects the propagation of coronal mass ejections and their driven shocks, thus the propagation of solar energetic particles. Previous studies have indicated a generally good correlation between the neutral line determined from the source surface maps and the HCS (or the sector boundary) observed in the inner heliosphere. Since it takes 2–6 days for the solar wind to propagate to 1 AU, thus it is possible to predict the crossing of the HCS at the Earth using the source surface maps. In this study, we analyze the source surface maps for the period from 1995 to 2021. The expected neutral line crossings are mapped to 1 AU using Parker’s spiral field model and compared with the HCS crossings observed by the Wind spacecraft. It is found that while there are cases with a good match, the majority of the cases show a large discrepancy. In addition, we found a solar cycle variation in the discrepancy. We will present detailed results and discuss the implications of the results. |
|11||MHD simulations in the Solar Terrestrial ObseRvations and Modeling Service (STORMS)||Indurain, M et al.||Poster|
| ||Indurain, M., Dalmasse, K., Alexandre, M., Pinto, R., Reville, V., Rouillard, A.P.|
| ||As part of the Solar Terrestrial ObseRvations and Modeling Service (STORMS), an important development axis is the production of heliospheric magnetohydrodynamic (MHD) simulations for monitoring and studying solar activity in the heliosphere and the near-Earth environment.
Starting from observations on the photosphere, 1D MHD model Multi-VP and 3D MHD model Heliocast give a physical and consistant description of the solar wind. The creation of synthetic imagery make it possible to compare the results with observations like coronagraph.
A part of these simulations are available through the VSWMC Virtual Space Weather Modelling Center and can be coupled with other models (EUHFORIA). A « run on request » mode for users can help user in studying a particular event.|
|12||CUBE (CME Catcher Carousel) – a nanosatellite space mission concept for future ESA space weather activities ||Ivanovski, S et al.||Poster|
| ||S. Ivanovski, F. Fiore, M. Lavagna, M. Piersanti, M. Laurenza, R. Iuppa, R. Battiston, S. Danzeca, P. Diego, D. Gacnik, I. Kramberger, A. Menicucci, and V. Vilona |
| ||INAF – Osservatorio Astronomico di Trieste, Italy; Politecnico di Milano – Dipartimento di Scienze e Tecnologie Aerospaziali, Italy; Università degli studi dell’Aquila, Italy; INAF- IAPS, Italy; Università di Trento, Italy; CERN, Switzerland; SkyLabs, Slovenia; University of Maribor; ESA, the Netherlands|
| ||We are pleased to announce that INAF (Istituto nazionale di Astrofisisca), POLIMI (Politecnico Milano), SkyLabs d.o.o., TU Delft, University of Maribor, University of Trent, joined in a consortium of research institutes, universities and industry, won the tender "Space Weather Monitor Nanosatellites" published by the European Space Agency (ESA) with a project proposal called CUBE (CME Catcher Carousel).
We propose multi-point, multi-in-situ measurements with a low-cost constellation of nano-satellites to monitor the Earth’s magnetospheric response, at magnetic reconnection sites and near the poles of the Earth, to various Space Weather phenomena directly associated to the solar activity, such as Coronal Mass Ejections (CME) and Solar Energetic Particle (SEP) events). This approach complies three main aspects of nowadays research - 1) advanced low-cost technology to study phenomena that can be investigated not only 2) at better spatial and temporal resolution but to be performed through 3) synergetic and simultaneous measurements.
Describing and quantifying the solar wind energy transfer to the Earth's magnetosphere-ionosphere system is one of the fundamental questions in space physics. The main objective of the proposed future CUBE constellation is to identify incoming Coronal Mass Ejections (CME) and solar energetic particle (SEP) events, measure them at different magnetospheric locations and altitude to quantitatively understand the energy transport toward the Earth. One of the objectives is also to study the SEP penetration in the magnetosphere, ionization of the ionosphere, and oscillations of the magnetic field during SEP events. All proposed studies above can be achieved by a constellation of nano-satellites hosting magnetometers and sensitive particle monitors.
The baseline mission analysis, to be confirmed during the study, includes two 6U spacecraft on circular SSO and six 12U spacecraft on a highly energetic circular orbit, ~60000 km radius, phased 60 degrees away from one another. All units will be equipped with magnetometers, plasma analyzer, and particle monitors capable of measuring magnetic field strength of a few nT, proton spectra from a few tens keV to a few hundred MeV, and electron spectra up to a few hundred keV. The preliminary analysis of the mission suggests a three-year period for deploying in orbit the constellation of 6-8 nano-satellites of the 6-12U class.|
|13||The Solar Terrestrial ObseRvations and Modeling Service (STORMS)||Alexandre, M et al.||Poster|
| ||Alexandre M., Indurain M., Rouillard A.P., Dalmasse K., Pinto R.|
| || IRAP;  InforMarty;  Now Thales Alenia Space;  CEA|
| ||We present an on-going effort to develop a public infrastructure to support research in heliophysics as well as space-weather forecasting. STORMS combines a wide range of observation and in situ measurements with heliospheric models to study and model the influence of solar activity on the near-Earth environment. Supporting operations of space missions, such as Solar Orbiter, is an important goal for this service. The Magnetic Connectivity Tool helps with deciding the pointing of remote-sensing instruments by exploiting real-time data and forecasts based on numerical simulations. It finds regions of the solar surface that may be connected with a spacecraft in a near future. It is operational since 2020 and is
currently used for Solar Orbiter mission. Predicting solar wind properties is achieved by combining coronal and heliospheric models (Multi-VP, Pluto, 1D-MHD). Analysis of multi-point imaging to derive the 3-D structure of solar wind structures such as Coronal Mass Ejections (CMEs) and Corotating Interaction Regions (CIRs) is also performed (Shock Tool). Daily forecasts provides prediction to the scientific community and end users. As a community service, STORMS allows « run on request » simulations for users, helping them in studying a particular event. This is available through the VSWMC Virtual Space Weather Modelling Center and can be coupled with other models (EUHFORIA). Further STORMS services will integrate runs-on-demand of the new multi-species IRAP Solar Atmosphere Model (ISAM) and a full database of 3-D MHD simulations.||