Conveners
Multi-scale energy release, flares and coronal mass ejections
- Francesca Zuccarello (Universitร di Catania)
Multi-scale energy release, flares and coronal mass ejections
- Francesca Zuccarello (Universitร di Catania)
Multi-scale energy release, flares and coronal mass ejections
- Ioannis Kontogiannis (Leibniz-Institute for Astrophysics Potsdam (AIP))
Multi-scale energy release, flares and coronal mass ejections
- Ioannis Kontogiannis (Leibniz-Institute for Astrophysics Potsdam (AIP))
Multi-scale energy release, flares and coronal mass ejections
- Alessandro Bemporad (Istituto Nazionale di Astrofisica (INAF))
Coronal mass ejections (CMEs) are huge eruptions of magnetized plasma from the Sun that travel into interplanetary space. These energetic and complex phenomena, when they interact with Earth's magnetic field, can cause significant disruptions. Due to their potential impact, there has been a strong focus on studying CMEs to predict them well in advance of their arrival at our planet. In my...
Our study aims to advance our understanding of the complex interactions between Coronal Mass Ejections (CMEs) and the solar wind/interplanetary magnetic field (IMF) system. We introduce a novel flux-rope semi-analytical MHD model that incorporates a comprehensive approach to understanding the impact of magnetic erosion and virtual mass on the propagation of CMEs. This model explores the...
Coronal dimmings are sudden decreases of the solar EUV and soft X-ray emission caused by coronal mass ejection (CMEs). From the solar observations, we know that dimming regions map to the bipolar ends of closed magnetic field lines that become stretched or temporarily opened during an eruption, and the decrease in the emission is a result of the depletion of coronal plasma caused by the...
We present a rare case of a three-part solar coronal mass ejection (CME) observed in the low corona on March 28, 2022. We observe a bright core/prominence, dark cavity, and a bright CME leading edge in SolO/EUI and STEREO-A/EUVI. We perform 3D reconstructions of the filament eruption from three vantage points: SolO, STEREO-A, and SDO. The filament height increased from 28 to 616 Mm over 30...
Parker Solar Probe (PSP) and Solar Orbiter (SO) observe the Sun from unprecedented close-in orbits out of the Sun-Earth line. Due to the highly elliptical orbits of the respective S/C, they cover varying heliocentric distances during their encounters around the Sun. They both provide high-resolution observations of the heliosphere through their white light heliospheric imagers: PSP/WISPR and...
Coronal pseudostreamer flux systems have a specific magnetic configuration that influences the morphology and evolution of coronal mass ejections from these regions. Here we present the analysis of a recent, high-resolution magnetohydrodynamic simulation of a CME eruption from an idealized pseudostreamer configuration through the construction of synthetic remote sensing and in-situ...
We present observations of a solar eruption captured by Metis onboard Solar Orbiter on October 12, 2022, during its perihelion passage. Using total brightness data, we observed the outward propagation of helical structures for more than three hours, extending up to 3 solar radii following a polar crown prominence eruption. These structures exhibited a notable trend: their inclination decreased...
Observations have shown a clear association of filament/prominence eruptions with the emergence of magnetic flux in or near filament channels. Magnetohydrodynamic (MHD) simulations have been employed to systematically study the conditions under which such eruptions occur. These simulations to date have modeled filament channels as two-dimensional (2D) flux ropes or 3D uniformly sheared...
Magnetic flux rope (MFR) is generally considered the core structure of coronal mass ejections (CMEs). However, how an MFR forms and develops into a CME has been elusive. Through a series of observational studies, we found that a coherent magnetic flux rope may originate from a โseedโ MFR that is formed through magnetic reconnection in a current layer underneath a sheared magnetic arcade, as a...
The study of coronal mass ejection triggering and early evolution necessitates numerical modelling, as measuring the coronal magnetic field is challenging. A key ingredient of the modelling efforts is to reliably identify and track the underlying magnetic structure of the eruption, the magnetic flux rope (MFR), in the simulation data. To achieve this, we developed an extraction and tracking...
The properties of pre-eruptive structures of coronal mass ejections (CMEs) are important for forecasting solar eruptions, the former of which are usually quantified by measuring the properties of their footpoints in observations. However, the matter of how to identify the footpoints of pre-eruptive structures and how to do so with the use of ground-based instruments still remains elusive. In...
The 3D coronal magnetic field is the decisive component to understand the formation and eruption of flux ropes in the solar corona. Non-linear force-free magnetic field extrapolations are a frequently applied method to provide a realistic estimate of the coronal magnetic field from photospheric vector magnetograms but are typically limited to small simulation volumes.
We present a novel...
Solar flare prediction has often been studied with data from the Solar Dynamics Observatory (SDO), which provides images of the full solar disk in different wavelength bands, probing different heights of the solar atmosphere, including the photospheric magnetic field. Recent studies have shown that spectroscopic data such as observations with the Interface Region Imaging Spectrograph (IRIS)...
The three-dimensional magnetic reconnection geometries have recently been shown to be present in solar flares, providing explanations for various observed phenomena, including evolution of sigmoids, drift of the erupting flux rope legs, and the shape of solar flare arcades. We review the observational evidence for these processes and their consequences for space weather. Particular emphasis is...
X-ray observations provide insight into the energy release in solar flares - the heated material and accelerated particles detectable via thermal and non-thermal bremsstrahlung emission respectively. We present observations of small active regions flares and even smaller quite Sun โflaresโ observed with the Nuclear Spectroscopic Telescope Array (NuSTAR), a highly sensitive telescope providing...
The mechanism of energy release from solar flares are still not fully understood and the study of small-scale features is an important aspect toward this understanding. Flare ribbons act as the footpoints of a flare and are crucial to know the process of flare reconnection. We present here a study about the fine structures of flare ribbons using a high resolution observations using the Swedish...
The gradual phase is a relatively quiet stage in the evolution of a flare, encompassing most of its duration. During this phase, the hot and dense flare loops, formed by reconnection and chromospheric evaporation in the impulsive phase, gradually cool down and decrease in density. We propose and demonstrate with 3D simulation that the seemingly calm gradual-phase flare loops are filled with...
Recent exploitation of spectropolarimetric data has significantly enhanced our understanding of the dynamical and magnetic responses of the photospheric and chromospheric layers during the rapid energy release that occurs in solar flares. In this context, we utilized high-resolution observations from 22nd October 2014, captured during an X1.6 confined flare by the Interferometric Bidimensional...
During the impulsive phase of the flare, beams of non-thermal electrons move from the magnetic reconnection site towards the chromosphere, where the density increases rapidly. Therefore, we can estimate the plasma density distribution along the non-thermal electrons path directly from the observations of the energy-altitude relation obtained for the HXR footpoint sources. Its shape is...
The quest for ever higher spatial and temporal resolution in solar physics can sometimes be thwarted by photon flux. However, in solar flares the greatly increased output across most of the electromagnetic spectrum means that we can often take advantage of high spatial and temporal resolution simultaneously. The rapid evolutionary timescales of flares certainly merit this effort. This talk...
Observations of greater than 100 MeV gamma-ray emission from solar flares from active regions located behind the visible solar disk pose interesting questions regarding the acceleration sites and mechanism, the transport and interaction points of the accelerated particles during these events. Two of the most popular scenarios to explain these observations are (a) acceleration at the coronal...
The Solar Orbiter's Major Flare SOOP (Solar Orbiter Observing Plan) campaign successfully captured several M- and C-class flares as the spacecraft approached perihelion in Spring of this year (March and April). This campaign provided unprecedented observations of solar flare dynamics through high-resolution extreme ultraviolet (EUV) observations using the High Resolution Imager (HRIEUV) of the...
Monster active regions 13663 and 13664 produced not less than 18 X-class solar flares between May 3 and May 15, before rotating out of view from Earth. Despite this, AR 13664 continued to exhibit significant activity, generating numerous events observed by instruments onboard the Solar Orbiter mission. This extraordinary sequence of strong flares not only delighted sky watchers with remarkable...
For the first time we present comparison of advanced FLARIX NLTE time-dependent numerical simulations of flaring emission with spectral observations of a compact C1.6 GOES-class flare recorded with MSDP (Multichannel Subtractive Double Pass) imaging spectrograph installed at the Biaลkรณw Observatory. The high time resolution (50 ms) MSDP spectral data, enabled comprehensive analysis of H-alpha...
