Conveners
SWR1 – Magnetic Sources of Space Weather Across Solar Atmospheric Layers: Orals - Part 1
- Hanna Strecker (Instituto de Astrofísica de Andalucía)
- Paolo Pagano (Università degli Studi di Palermo)
- Clementina Sasso (INAF-Osservatorio Astronomico di Capodimonte, Italy)
- Ioannis Kontogiannis (ETH Zurich and IRSOL Locarno)
SWR1 – Magnetic Sources of Space Weather Across Solar Atmospheric Layers: orals - part 2
- Hanna Strecker (Instituto de Astrofísica de Andalucía)
- Clementina Sasso (INAF-Osservatorio Astronomico di Capodimonte, Italy)
- Paolo Pagano (Università degli Studi di Palermo)
- Ioannis Kontogiannis (ETH Zurich and IRSOL Locarno)
SWR1 – Magnetic Sources of Space Weather Across Solar Atmospheric Layers: orals - part 3
- Hanna Strecker (Instituto de Astrofísica de Andalucía)
- Ioannis Kontogiannis (ETH Zurich and IRSOL Locarno)
- Paolo Pagano (Università degli Studi di Palermo)
- Clementina Sasso (INAF-Osservatorio Astronomico di Capodimonte, Italy)
Description
Space weather is largely driven by the drastic and sudden evolution of magnetic structures in the Sun. Sometimes such transients lead to the sudden release of magnetic energy in the form of radiation or mass ejections. In other cases, newly formed or emerging structures alter the equilibrium of a magnetic complex, triggering eruptions. While the study of the magnetic field in the solar atmosphere remains a significant challenge for observations and models, understanding these mechanisms is essential to improve our space weather prediction capabilities. Magnetic structures, such as flux ropes, filaments/prominences and coronal loops form as part of active regions and along polar inversion lines. These structures evolve dynamically across the layers of the solar atmosphere, from the photosphere to the corona, and their evolution can culminate in eruptive events. Many theories based on observations (from new instruments such as PHI, EUI, METIS on-board Solar Orbiter) or numerical simulations have been put forward to explain how they trigger space weather events. Moreover, such mechanisms in the solar corona are the only close and observable examples of several plasma processes (e.g. magnetic reconnection or magnetic confinement) that hold the key to a deeper understanding of plasma physics. In this session, we will host contributions that show the current state of the art of observation and modelling of the solar atmosphere that illustrate the role of these magnetic structures and how their evolution affects space weather and how they can be used to help to improve our forecasts.
Magnetic flux ropes are ubiquitous features observed in the low corona and propagating through the solar atmosphere. They are formed by combined action of the magnetic field of the Sun and its internal processes, observed remotely and in situ. Flux ropes are one of the main components of Coronal Mass Ejections, drivers of major geomagnetic storms, and they are therefore of high importance in...
The inference of the photospheric magnetic field has, until recently, been limited to one view point: that from Earth. This is especially important when studying the long term evolution of active regions, where they are only close to disc centre for approximately a week. The Polarimetric and Helioseismic Imager (PHI) on board Solar Orbiter (SO) has made it a reality to extend the coverage of...
Our Sun is a highly dynamic star, exhibiting a broad range of activity from subtle dynamic events to powerful flares and large-scale coronal mass ejections (CMEs). CMEs are vast expulsions of magnetised plasma from the solar corona, while flares are intense bursts of electromagnetic radiation originating in the solar atmosphere. A flare and CME often occur concomitantly; the flare would then...
Solar eruptions are ubiquitous in the sun and play a significant role in space weather. With the advent of multi-view observations, we can gain a better understanding of the three-dimensional structure of these eruptive events and identify the various energetic processes involved. To fully grasp the physics behind these phenomena, it is essential to develop innovative simulations that...
Understanding the causative mechanisms behind solar eruptions and solar energetic particle events is crucial for space weather forecasting. However, although numerous models have been proposed regarding the relationship between the magnetic fields of active regions and solar eruptions, the structure and parameters of the magnetic fields that govern these events remain unclear, which still...
Studying magnetic flux ropes is crucial for understanding the origin and evolution of Coronal Mass Ejections (CMEs), as these twisted magnetic structures often serve as the core configuration driving CMEs from the solar corona. On November 9, 2021, the Metis coronagraph (Antonucci et al. 2020) on-board ESA Solar Orbiter mission, observed a slow erupting flux rope, when the spacecraft was at...
The ERC-AdG project Open SESAME (project No 101141362) aims to develop a time-evolving model for the entire solar atmosphere, including the chromosphere and transition region, based on a multifluid description. Currently, models are primarily steady, rely on a single-fluid description and include only the corona due to computational challenges. We plan to use time-evolving ion-neutral and...
Solar flares are primary drivers of space weather and play a crucial role in the Sun-Earth connection. The physical mechanisms underlying solar flare initiation remain a topic of intense research. It is widely accepted that flares result from the rapid release of magnetic energy stored in the stressed configurations of ARs. Several competing, and possibly concurrent, mechanisms have been...
The METIS Coronagraph onboard Solar Orbiter observes simultaneously in the Visible (VL) band between 580 and 640 nm and the Ultraviolet (UV) band at 121.6 nm. It also observes at a high spatial and temporal resolution, thus allowing a comprehensive characterisation of solar events.
In particular, the Metis team is creating a database of solar eruptive events observed in both the VL and UV...
We present a comprehensive statistical study between type II radio bursts from the metric (m) to the dekameric–hectometric (DH) domain and their association with different solar and space weather phenomena, namely, solar flares, sunspot configurations, filament eruptions, coronal mass ejections, their interplanetary counterparts and shocks, in situ detected particles and geomagnetic storms. We...
Solar active regions, accumulations of strong magnetic field, play a crucial role in driving space weather. Their evolution can influence the solar wind, and they can trigger eruptive phenomena. Active regions have long been studied from Earth’s vantage point using instruments such as the Helioseismic and Magnetic Imager (HMI) on the Solar Dynamics Observatory (SDO). While HMI allows for...
Coronal Mass Ejections (CMEs) are the primary drivers of space weather phenomena.
Once a CME reaches Earth the severity of the geomagnetic response is dependent on CME properties such as speed, dynamic pressure, and the specific magnetic configuration of the CME. CMEs can be modelled with a bright front, dark cavity and core. This core is associated with a flux rope in CME models.
We...
Physics-based modelling of the large-scale dynamics caused by space-weather relevant Coronal Mass Ejections (CMEs) is conventionally carried out employing either a coronal or heliospheric approach. In the former, the dynamics all the way from the low corona to the heliosphere is modeled, while in the latter the simulation is started at heliocentric distances where the solar wind is...
The solar storms of May 2024 were a series of powerful solar flares and coronal mass ejections (CMEs) that occurred between 10 and 13 May 2024, followed by a few strong solar flares over the next few days during solar cycle 25. As these eruptions propagated through the corona, they generated multiple solar type II radio bursts, indicating the presence of shock waves.
This study aims to...
In recent decades, diverse catastrophic phenomena, from earthquakes and landslides to structural collapses and myocardial infarctions, have been framed as critical transitions in complex systems, marked by a sudden, irreversible shift from equilibrium to an unstable state. Here, we extend for the first time the Natural Time Analysis (NTA) framework to solar Active Regions (ARs) in order to...
Modelling solar eruptions is crucial to understand their triggers and how they might impact Earth's magnetic environment. Thus, magnetic field simulations of the low solar corona are of great relevance for space weather forecasting. In particular, simulations that are driven by the observed magnetic field at the photosphere have proven to be a powerful tool to model the energy build up and...
Solar flares result from the rapid conversion of stored magnetic energy within the Sun's corona. These energy releases are associated with coronal magnetic loops, which are rooted in dense photospheric plasma and are passively transported by surface advection. Their emissions cover a wide range of wavelengths, with soft X-rays being the primary diagnostic for the past fifty years. Despite the...
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CHESS expands the training of two baseline Convolutional Neural Networks (CNNs) to obtain a more efficient, least-biased CNN model for segmenting coronal holes (CHs).
Our two CNNs are based on (i) a U-Net and (ii) a Res-U-Net architecture. These two CNNs have been pre-trained with the coronal hole (CH) boundary data from the Heliophysics Events Knowledgebase (HEK). These initial,...
The chromosphere plays a pivotal role by linking the Sun interior to its interplanetary environment. It indeed regulates energy and mass transfer into the corona and solar wind, particularly during small-scale magnetic flux emergence events. The interplay between shock-driven processes and magnetic reconnection is known to be key for the chromospheric heating, however any characterisation of...
Coronal mass ejections (CMEs) are the main drivers of particle acceleration in the heliosphere, leading to geoeffective events in the Earth's environment.
Observations showing the buildup of CMEs reveal that the start of CME is the existence of a flux rope with a cool filament or not near the solar surface. Instability like torus or kink instability leads to the rise of the flux rope in the...
We performed full Stokes spectropolarimetric observations of loop footpoints in the active region NOAA 13363 during a C-class flare with the GREGOR Infrared Spectrograph (GRIS) on 2023 July 16. The observed spectral region included the photospheric Si I 10 827 A and Ca I 10 839 A lines and the chromospheric He I 10 830 A triplet. Simultaneously, high-cadence and high-resolution imaging...
The association between solar flares and coronal mass ejections (CMEs) plays a critical role in understanding solar eruptive phenomena and their impact on space weather. This work presents a comprehensive statistical analysis of 49 solar radio bursts detected by the POEMAS (POlarization Emission of Millimeter Activity at the Sun) instrument, which operates at 45 and 90 GHz at the CASLEO...
We at NICT currently forecast the maximum expected magnitude of solar flares for the next 24 hours. However, providing early warnings for major solar flares remains a significant challenge. To address this limitation, we are developing an alert system capable of predicting and issuing warnings for large flares at least several hours before their onset.
We recently implemented a...
Coronal jets are known to be transient phenomena associated with energy release processes, with magnetic reconnection being their most probable origin. However, the precise timing and location of the reconnection events have not been clearly established. Moreover, the pronounced geometric complexity of coronal hole (CH) boundaries — where these jets typically originate — suggests a dynamic...
The Astro-rivelatore Gamma a Immagini LEggero (AGILE) has been a unique and successful space mission of the Italian Space Agency (ASI), with the programmatic and technical contribution of INAF and INFN. During almost 17 years of observations, since the launch on April 23, 2007 to the satellite re-entry on February 14, 2024, AGILE contributed to high-energy astrophysics, terrestrial and solar...
Tremendous progress have been made in computing realistic global simulation of the solar magnetism and its 11 yr cycle. Yet there is still one paradox: none of the published dynamo simulations display sunspots. This is the so-called spotty-dynamo paradox. In this talk we will discuss what we think is missing in current global HPC simulation of the solar dynamo and 11 yr cycle and how new high...
We aim to develop a more coherent understanding of the evolution of the physical properties of solar eruptions as they propagate through interplanetary space. Recent multi-spacecraft observations of single ICME events allow us to systematically trace magnetic field related properties across vast spatial domains. Among these properties, magnetic helicity appears to be especially interesting. As...
Context: On 26 September 2022, a quiescent solar prominence was observed using Hα imaging spectroscopy with the Solar Dynamics
Doppler Imager on the Solar Magnetic Activity Research Telescope. Prior studies identified 4- and 15-min oscillations using a narrow
slit and 1D wavelet methods, limiting spatial coverage. We extend this analysis to the entire prominence using a 3D wavelet...
The Space Weather Follow-On (SWFO) program will provide operational solar-coronal images and in situ solar wind measurements to the science community and to space weather information users. Here we first give status updates on the Compact Coronagraph 1 (CCOR-1) onboard the Geostationary Operational Environmental Satellite 19 (GOES-19) since its June 25, 2024 launch. The Post-Launch Test (PLT)...
