Our Sun is uniquely placed to enable a detailed study of astrophysical plasmas and how they are governed by the magnetic fields that thread through them. On the one hand, magnetic fields confine plasma and determine plasma heating, flows, and energisation. On the other hand, magnetic fields and their evolution give rise to the most violent eruptions in the Solar System. Understanding the details of how energy is built up and released, and the impact of these physical processes on the plasma, remain key open questions that directly map to UKRI's science strategy through the STFC Solar System Advisory Panel's roadmap for Solar System research goals: What are the causes, consequences and predictability of solar magnetic variability and the solar cycle? What are the structures, dynamics and energetics of the Sun? What are the underlying processes that drive Sun-planet connections? And what are the fundamental processes at work in the Solar System? As laid out in this White Paper, the Moon-Enabled Sun Occultation Mission (MESOM) directly addresses these questions and in doing so delivers several Pillars of the National Space Strategy.

Small-scale propagating disturbances (PDs) are ubiquitous in the solar corona. The method called time-normalised optical flow (TNOF) was developed for mapping PDs velocity fields in time series of extreme-ultraviolet (EUV) images. We show PDs velocity fields of a quiet-Sun (QS) region containing a small coronal hole (CH) and filament channel (FC) that were jointly observed by Extreme Ultraviolet Imager (EUI) on board the Solar Orbiter and Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The QS observations acquired on 28 October 2023 in the 174 Å channel of High Resolution EUV Imager (HRIEUV) of EUI and 171 Å channel of AIA were used. During the time of the observations, the separation angle between Solar Orbiter and SDO was approximately 26°. A novel image-alignment analysis shows that the dominant formation heights are 11.4 Mm for HRIEUV and 4 Mm for AIA. Despite this height difference, the PDs velocity fields obtained from the observations from the two instruments agree well throughout the region. In the QS, the median PDs speed is about 6.7 and 7.4 kms−1 for HRIEUV and AIA, respectively, with maximum speeds of about 40 kms−1. The small equatorial CH region is dominated by a low temperature of ≈0.8 MK and is host to high PDs speeds, with a median speed of 17 kms−1. The velocity field bridges coherently across the CH from neighbouring QS regions from east to west, and the CH must therefore be overlaid by a system of long, low-lying closed magnetic loops. This unexpected configuration is supported by a potential field (PF) magnetic model and might be caused by the longevity of the CH, which allows time for interchange reconnection with neighbouring closed-field regions. The FC is observed to be multi-thermal, with a narrow central high-emission strip at low (0.8 MK) and high (2.5 MK) temperatures and low emission at a warm (1.2 MK) temperature. Despite this distinct temperature profile, the PDs speeds in the FC are similar to those of the QS. The TNOF velocity field shows that PDs tend to flow into the FC from neighbouring regions before they align along the FC in a coherent direction. This means that PDs within filaments are driven by external sources. The vector field is consistent with a highly non-potential barbs-and-spine tubular magnetic field; the PF model fails to replicate this configuration. We conclude that longer magnetic loops are required for higher PDs speeds, as observed for CH here, and that the smaller loop systems of the QS and FC generally lead to lower speeds. These multi-instrument results show that the TNOF method can confidently be used as a diagnostic tool for the kinematics of PDs, and it highlights its potential for probing the coronal magnetic field orientation, particularly in highly non-potential regions, where extrapolation models may fail.

The ratio of radially to tangentially polarized Thomson-scattered white light provides a powerful tool for locating the 3D position of compact structures in the solar corona and inner heliosphere, and the Polarimeter to Unify the Corona and Heliosphere (PUNCH) has been designed to take full advantage of this diagnostic capability. Interestingly, this same observable that establishes the position of transient blob-like structures becomes a local measure of the slope of the global falloff of density in the background solar wind. It is thus important to characterize the extent along the line of sight of structures being studied, in order to determine whether they are sufficiently compact for 3D positioning. In this paper, we build from analyses of individual lines of sight to three-dimensional models of coronal mass ejections (CMEs), allowing us to consider how accurately polarization properties of the transient and quiescent solar wind are diagnosed. In this way, we demonstrate the challenges and opportunities presented by PUNCH polarization data for various quantitative diagnostics.

The Polarimeter to Unify the Corona and Heliosphere (PUNCH) mission is a NASA Small Explorer to determine the cross-scale processes that unify the solar corona and heliosphere. PUNCH has two science objectives: (1) understand how coronal structures become the ambient solar wind, and (2) understand the dynamic evolution of transient structures, such as coronal mass ejections, in the young solar wind. To address these objectives, PUNCH uses a constellation of four small spacecraft in Sun-synchronous low Earth orbit, to collect linearly polarized images of the K corona and young solar wind. The four spacecraft each carry one visible-light imager in a 1 + 3 configuration: a single Narrow Field Imager solar coronagraph captures images of the outer corona at all position angles, and at solar elongations from 1.5° (6 R⊙) to 8° (32 R⊙); and three separate Wide Field Imager heliospheric imagers together capture views of the entire inner solar system, at solar elongations from 3° (12 R⊙) to 45° (180 R⊙) from the Sun. PUNCH images include linear-polarization data, to enable inferring the three-dimensional structure of visible features without stereoscopy. The instruments are matched in wavelength passband, support overlapping instantaneous fields of view, and are operated synchronously, to act as a single “virtual instrument” with a 90∘ wide field of view, centered on the Sun. PUNCH launched in March of 2025 and began science operations in June of 2025. PUNCH has an open data policy with no proprietary period, and PUNCH Science Team Meetings are open to all.

Interface Region Imaging Spectrograph bright points (IBPs) are ubiquitous, small-scale energetic events with a multithermal nature, typically observed in the chromosphere or transition region and closely linked to photospheric structure and coronal composition. Their evolution is shaped by various physical processes, including plasma dynamics and magnetic interactions. This paper explores IBP evolution through a large statistical sample, focusing on when maximum values of attributes occur, and examines whether statistical differences exist between “Active Quiet Sun” (AQS; above the network) and “True Quiet Sun” (TQS; above the internetwork) IBPs. The attributes analyzed are maximum brightness, plane-of-sky (POS) speed, POS travel distance, POS acceleration, and apparent size (POS area). IBPs can reach peak brightness/size at any point during their lifetimes, likely due to complex chromospheric interactions. AQS and TQS IBPs are similar in most attributes and tend to reach maximum POS speed around halfway through their lifetimes. Acceleration typically occurs early in their lifetime, with deceleration more common toward the end. Preliminary findings indicate two distinct IBP regimes with differing relationships between POS speed, brightness, and area. This study provides strong statistical evidence that IBPs—whether representing plasma motion or propagating heating events—follow arched trajectories along small magnetic loops. In this interpretation, the midpoint of an IBP’s lifetime corresponds to the crest of the arch, coinciding with the highest POS travel speeds. Magnetic reconnection likely initiates at photospheric footpoints, after which IBPs travel along loops, eventually returning to another footpoint. Deviations from loop-like evolution reflect complexity, asymmetry, and variability of loops.

Reliable identification of low-coronal CME origins remains a key limitation in space weather forecasting with coronagraphs not directly resolving low-coronal signatures. We present a re-engineered multi-thermal implementation of the ALMANAC algorithm, designed to detect eruptive signatures in EUV observations. The framework extends the method to a multi-wavelength system, improving robustness against projection effects, instrumental artifacts, and wavelength-dependent ambiguities via complementary temperature responses. A spatiotemporal clustering scheme merges detections across channels, reducing event bifurcation and improving coherence while maintaining NRT performance through parallel computing. Benchmarking against 20 halo CMEs from CDAW shows improved interpretability and operational usability, with clearer separation of eruptions and more consistent onset localisation relative to coronagraph estimates. The main benefits arise from improved event discrimination, reduced fragmentation, and more interpretable source region identification. ALMANAC shows sensitivity to precursor low-coronal activity not always captured in white-light catalogues, highlighting its advantages for early warning detection. When coupled with the ARTop framework, it enables co-analysis of coronal intensity variability and photospheric magnetic evolution. In this context, kurtosis time-series from multi-wavelength EUV data exhibit recurrent pre-eruptive spikes that frequently align with enhancements in magnetic winding and helicity injection. Across multiple regions, these signatures often precede solar activity, including potential discrimination of X-class flares, while remaining suppressed during magnetically quiet intervals. Overall, integrating coronal diagnostics with photospheric topology offers a pathway toward improved eruption forecasting and space weather prediction.

The population of small-scale brightenings observed across broad regions of the quiet-Sun (QS) corona shows coherent strong periodicities of approximate to 5 minutes and amplitudes of 20% to 30% of the mean. The periodicity is in the total number of detected brightenings, their creation rate, and their mean lifetime. Atmospheric Imaging Assembly/Solar Dynamics Observatory extreme-ultraviolet data spanning 2 hr shows that the periodicity is significant across broad areas of the QS. The periodicities are strong in the hotter 171 & Aring; (300 s period) and 193 & Aring; (340 s period) channels, but absent from the upper chromospheric 304 & Aring; channel, although periodicities are present in the 304 & Aring; channel in other datasets. The density of brightenings is highest above the photospheric network, with the network concentration becoming increasingly pronounced in the hotter channels. An extended study of 11 QS datasets spanning several years shows that these periodic modulations are common, with most periodicities found in the 4 to 6 minutes range. The time profiles of area and brightness for most brightenings show a gradual, nonimpulsive onset inconsistent with local reconnection, and the brightenings are more likely to appear first in the 171 & Aring; channel, then in the hotter 193 & Aring; channel. This suggests that the most plausible formation mechanism is wave or shock dissipation at or near the transition region, likely connected to spicule activity. This heating is modulated by photospheric p-modes and drives the production of transient brightenings in the QS upper chromosphere, transition region, and low corona.

Understanding how active-region properties influence coronal mass ejection (CME) dynamics is essential for constraining eruption models and improving space-weather prediction. Magnetic diagnostics derived above polarity inversion lines (PILs), including the critical height ($h_{\rm crit}$) of torus instability onset, the overlying field strength ($B_{\rm t}$), and ribbon flux ($R_{\rm f}$), provide physically motivated measures of eruption onset. The two main aims of this work are to (i) show that $h_{\rm crit}$ and $B_{\rm t}$ can equally well predict CME speeds when evaluated over the region of interest (ROI) not directly above the PIL, and (ii) assess the value of $h_{\rm crit}$, $B_{\rm t}$ and $R_{\rm f}$ in predicting CME speed. Photospheric magnetograms are modeled with potential-field extrapolations to obtain decay index profiles. Critical heights above PILs correlate strongly with 3D CME speed ($r = 0.71$). Using ROIs of $\approx$ 1.8, 3.7, and 7.3 Mm), centered on the PIL, weighted $h_{\rm crit}$ from the 7.3x7.3 ROI provides the strongest correlation ($r = 0.73$), while mean $B_{\rm t}$ at 150 Mm is weaker ($r = 0.33$). Combining both offers little improvement ($r = 0.74$), confirming $h_{\rm crit}$ as the dominant predictor. CME speed correlates moderately with $B_{\rm t} \times R_{\rm f}$ ($r = 0.44$), and highest when combined with $h_{\rm crit}$ ($r = 0.76$). Thus, in potential field models, ROI-based critical heights are as predictive as those above the PIL, indicating that the broader active-region field structure is equally valid as a diagnostic. When all parameters are considered together, $h_{\rm crit}$ alone consistently shows the highest predictive power for CME speed.

The large-scale plasma density structure of the extended solar corona is a tracer of the underlying magnetic field configuration and dictates the structure of the solar wind in interplanetary space. Accurate density maps are therefore important to probe the physics of the solar corona and the solar wind, and to improve space-weather forecasting. Density can be estimated from coronagraph observations using solar rotational tomography and is independently provided by global magnetohydrodynamic models. This study compares densities from tomography with the Magnetohydrodynamic Algorithm outside a Sphere (MAS) model across the whole corona over a solar cycle from 2007 to late 2023. The dependence of electron densities on latitude and heliocentric height is compared, with densities in better agreement at equatorial regions and lower heights. The streamer and nonstreamer regions are compared separately, as well as the average width of the streamer belt over the duration of solar cycle 24. The MAS model densities contain more fine-scale detail than those of the tomography, but there is a very good overall agreement in the structure and location of high-density features. In polar regions, where the photospheric magnetic field measurements that drive the MAS simulations present very large uncertainties, the tomographic densities are more accurate. Investigating the accuracy and reliability of these models, and understanding their limitations is crucial. Comparisons with observations highlight their advantages and disadvantages while stressing the importance of observational techniques to help constrain current and future models.

We use silicon-based nanograins as model nanodust in planetary nebulae and present photo-excitation and stability studies using synchrotron extreme ultraviolet radiation, while monitoring the induced cascade of visible/UV luminescence. We also conduct theoretical studies (atomistic simulations and classical Mie scattering), as well as stability studies of the grains under long-wavelength UV excitation using lasers or discharge lamps or under thermal treatments. We report that the luminescence of 1-nm grains remains stable for above ionization limit excitation [5-22 eV, 10(12) (photons/cm(2))/s]. Under excitation below the ionization limit, using lasers or discharge lamps (3.5 eV, 10(14)/cm(2)/s) or under thermal treatment, the luminescence exhibits partial stability at a steady similar to 50%, with slow partial recovery. Time-dependent density functional theory shows the structural stability of neutral or ionized ultrasmall nanograins, while organic dye molecules are fully quenched with no recovery. Computations also show the enhancement of scattering of soft x rays over the geometrical cross section. We analyze the results in terms of quantum confinement induced effects, including inhibition of e-h and e-Coulomb scattering, enhancement of e-e correlation, and relativistic e-vibration coupling. These effects lead to multi-electron excitation, singlet-triplet intersystem conversion, and plasmon-type Mie "polarizmon scattering" by valence electrons. Such novel characteristics point to the survivability of ultrasmall grains in x-ray or UV environments, which may serve as a UV shield for large interstellar molecules, necessary to life. (c) 2025 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution (CC BY) license(https://creativecommons.org/licenses/by/4.0/).

Accurate 3D reconstruction of coronal mass ejections (CMEs) is essential for understanding their propagation and improving space weather forecasts. In this study, we present a proof‐of‐concept deep learning framework that predicts seven parameters from synthetic multi‐view coronagraph images. We generate 9250 synthetic CME events using a 3D wireframe model, each defined by randomly sampled values for CME's longitude, latitude, tilt‐angle, and 3D propagation speed. The speed is used to compute heights at three timepoints aligned with SOHO/LASCO C3 and STEREO‐A/COR2 and STEREO‐B/COR2 cadences. These values are used to render time‐resolved synthetic images, serving as inputs to a convolutional neural network (CNN). The CNN is trained using five‐fold cross‐validation to predict the sine and cosine of the longitude, latitude, tilt‐angle, and apex heights at the three specified times. CNN achieves mean absolute errors (MAE) of 4.88°, 2.50°, and 13.35° for longitude, latitude, and tilt, and for heights. The predicted heights are used to derive CME speed via height‐time fitting. Performance metrics include Pearson's for most parameters (tilt: ), and values of 0.99 for longitude and latitude, with heights , and 0.61 for tilt. The average test MAE across all outputs is 0.134 0.004. When applied to a real CME event, the CNN's predictions fall within the typical uncertainties reported for standard geometric fitting approaches. While challenges remain in handling real data, our results indicate that the trained model can generalize beyond synthetic data, highlighting its potential for operational space weather forecasting.

The magnetic field of the low corona above quiet Sun regions is extremely challenging to observe directly, and the topology is difficult to discern from extreme ultraviolet (EUV) image data due to the lack of distinct loops that are present in, for example, active regions. We aim to show that the velocity field of faint propagating disturbances (PD) observed on-disk in the quiet corona can be interpreted in terms of the underlying magnetic topology. The PD are observed in Atmospheric Imaging Assembly/Solar Dynamics Observatory (AIA/SDO) time series in three channels: 304, 171, and 193 Å corresponding to the high chromosphere, transition region/low corona, and the corona, respectively. An established Time-Normalised Optical Flow method enhances the PD and applies a Lucas–Kanade algorithm to gain their velocity field. From the velocity field, we identify the source and sink locations of the PDs, and compare these locations between channels and with the underlying photospheric network. Source regions tend to be located above the photospheric network, and sink regions with the internetwork. Sink regions in the internetwork suggest either that closed field can be concentrated rather than evenly distributed in the internetwork, or that fieldlines opening into the corona can sometimes be concentrated above internetwork regions. We find regions of almost exact alignment between channels, and other regions where similar-shaped structures are offset by a few pixels between channels. These are readily interpreted as vertical or non-vertical alignment of the magnetic field relative to the observer viewing from above. Regions of isolated source regions in the cold (304 Å) or hotter (171 and 193 Å) channels can be interpreted in terms of the magnetic topology, but support for this is weaker. These results offer support for the future use of PD velocity fields as a coronal constraint on magnetic extrapolation models.

In a space weather context, the most geoeffective coronal mass ejections (CMEs) are fast CMEs from Earth-facing solar active regions. These CMEs are difficult to characterize in coronagraph data due to their high speed (fewer observations), faintness, Earthward orientation (halo CMEs), and disruptions from associated high-energy particle storms. Any diagnostic aiding in early CME speed identification is valuable. This study investigates whether the 3D speeds of 37 CMEs are correlated with the critical heights of their source regions, to test the hypothesis that if the critical height is located at a higher altitude in the corona, the weaker magnetic field environment will enable a faster CME to be produced. Critical heights near CME onset are calculated by identifying polarity inversion lines (PIL) in magnetogram data using automated and manual methods. 3D speeds are determined by fitting a Graduated Cylindrical Shell model to multiviewpoint coronagraph images. For the automated method, we find a high correlation of 71% ± 8% between CME speed and critical height, dropping to 48% ± 12% when using CME plane-of-sky speeds, on which most previous similar studies are based. An attempt to improve the critical height diagnostic through manual PIL selection yields a lower correlation of 58% ± 13%. The higher correlation from the automated method suggests that encompassing the full PIL structure is a better measure of the magnetic conditions that influence CME dynamics. Our results highlight the potential for critical height as a continuously computable diagnostic for forecasting the 3D speeds of Earth-directed CMEs.

Bright points (BPs) are ubiquitous, small-scale energetic events with multithermal signatures, typically observed in the chromosphere and linked to both photospheric structure and coronal composition. Their evolution is influenced by various physical processes, including plasma dynamics and magnetic interactions. This paper examines BP evolution using a large statistical sample, focusing on when they reach maximum values for key attributes, and explores differences between BPs in the "Active Quiet Sun" (AQS, above the network) and the "True Quiet Sun" (TQS, above the internetwork). Observed attributes include maximum brightness (total and intrinsic), plane-of-sky (POS) speed, travel distance, acceleration, and apparent size (POS area). BPs can reach maximum brightness and size at almost any time during their lifetime, likely due to complex chromospheric interactions. AQS and TQS BPs show similar behaviour overall and tend to reach maximum POS speed around the midpoint of their lifetimes. Positive acceleration usually occurs early, while negative acceleration is more common near the end. Preliminary results suggest two distinct BP regimes with differing relationships between intrinsic brightness and area. We interpret these trends as evidence that BPs, whether due to plasma motion or a heating event, follow arched paths – likely along short magnetic loops. In this model, the midpoint of a BP's life corresponds to the crest of the arch, producing the greatest POS speeds. Reconnection may occur at a footpoint, with the BP moving along the loop before returning to the photosphere. Deviations from this expected evolution may result from complex chromospheric interactions or BPs with highly non-linear POS motions.

In a space weather context, the most geoeffective coronal mass ejections (CMEs) are fast CMEs from Earth-facing solar active regions. These CMEs are difficult to characterize in coronagraph data due to their high speed (fewer observations), faintness, Earthward orientation (halo CMEs), and disruptions from associated high-energy particle storms. Any diagnostic aiding in early CME speed identification is valuable. This study investigates whether the 3D speeds of 37 CMEs are correlated with the critical heights of their source regions, to test the hypothesis that if the critical height is located at a higher altitude in the corona, the weaker magnetic field environment will enable a faster CME to be produced. Critical heights near CME onset are calculated by identifying polarity inversion lines (PIL) in magnetogram data using automated and manual methods. 3D speeds are determined by fitting a Graduated Cylindrical Shell (GCS) model to multi-viewpoint coronagraph images. For the automated method, we find a high correlation of 71 dropping to 48 previous similar studies are based. An attempt to improve the critical height diagnostic through manual PIL selection yields a lower correlation of 58 13 encompassing the full PIL structure is a better measure of the magnetic conditions that influence CME dynamics. Our results highlight the potential for critical height as a continuously computable diagnostic for forecasting the 3D speeds of Earth-directed CMEs.

Understanding how active-region properties influence coronal mass ejection (CME) dynamics is essential for constraining eruption models and improving space-weather prediction. Magnetic diagnostics derived above polarity inversion lines (PILs), including the critical height ( h _crit ) of torus instability onset, the overlying field strength ( B _t ), and ribbon flux ( R _f ), provide physically motivated measures of eruption onset. The two main aims of this work are to (i) show that h _crit and B _t can equally well predict CME speeds when evaluated over the region of interest (ROI) not directly above the PIL, and (ii) assess the value of h _crit , B _t , and R _f in predicting CME speed. Photospheric magnetograms are modeled with potential-field extrapolations to obtain decay index profiles. Critical heights above PILs correlate strongly with 3D CME speed ( r = 0.71). Using ROIs of ≈1.8, 3.7, and 7.3 Mm, centered on the PIL, weighted h _crit from the 7.3 × 7.3 ROI provides the strongest correlation ( r = 0.73), while mean B _t at 150 Mm is weaker ( r = 0.33). Combining both offers little improvement ( r = 0.74), confirming h _crit as the dominant predictor. CME speed correlates moderately with B _t × R _f ( r = 0.44), and highest when combined with h _crit ( r = 0.76). Thus, in potential field models, ROI-based critical heights are as predictive as those above the PIL, indicating that the broader active-region field structure is equally valid as a diagnostic. When all parameters are considered together, h _crit alone consistently shows the highest predictive power for CME speed.

The three-dimensional (3D) coronal magnetic field has not yet been directly observed. However, for a better understanding and prediction of magnetically driven solar eruptions, 3D models of solar active regions are required. This work aims to provide insight into the significance of different extrapolation models for analyzing the preeruptive conditions of active regions with morphological parameters in 3D. Here, we employed potential field (PF), linear force-free field (LFFF), and nonlinear force-free field (NLFFF) models and a neural network-based method integrating observational data and NLFFF physics (NF2). The 3D coronal magnetic field structure of a "flaring" (AR11166) and "flare-quiet" (AR12645) active region, in terms of their flare productivity, is constructed via the four extrapolation methods. To analyze the evolution of the field, six prediction parameters were employed throughout, from the photosphere up to the base of the lower corona. First, we find that the evolution of the adopted morphological parameters exhibits similarity across the investigated time period when considering the four types of extrapolations. Second, all the parameters exhibited preeruptive conditions not only at the photosphere but also at higher altitudes in the case of active region (AR) 11166, while three out of the six proxies also exhibited preeruptive conditions in the case of AR12645. We conclude that: (i) the combined application of several different precursor parameters is important in the lower solar atmosphere to improve eruption predictions, and (ii) to gain a quick yet reliable insight into the preflare evolution of active regions in 3D, the PF and LFFF are acceptable; however, the NF2 method is likely the more suitable option.

The strongly coupled hydrodynamic, magnetic, and radiation properties of the plasma in the solar chromosphere makes it a region of the Sun's atmosphere that is poorly understood. We use data obtained with the high-resolution Visible Broadband Imager (VBI) equipped with an H$\beta$ filter and the Visible Spectro-Polarimeter (ViSP) at the Daniel K. Inouye Solar Telescope to investigate the fine-scale structure of the plage chromosphere. To aid the interpretation of the VBI imaging data, we also analyze spectra from the CHROMospheric Imaging Spectrometer on the Swedish Solar Telescope. The analysis of spectral properties, such as enhanced line widths and line depths explains the high contrast of the fibrils relative to the background atmosphere demonstrating that H$\beta$ is an excellent diagnostic for the enigmatic fine-scale structure of the chromosphere. A correlation between the parameters of the H$\beta$ line indicates that opacity broadening created by overdense fibrils could be the main reason for the spectral line broadening observed frequently in chromospheric fine-scale structures. Spectropolarimetric inversions of the ViSP data in the Ca II 8542 {\AA} and Fe I 6301/6302 {\AA} lines are used to construct semiempirical models of the plage atmosphere. Inversion outputs indicate the existence of dense fibrils in the Ca II 8542 {\AA} line. The analyses of the ViSP data show that the morphological characteristics, such as orientation, inclination and length of fibrils are defined by the topology of the magnetic field in the photosphere. Chromospheric maps reveal a prominent magnetic canopy in the area where fibrils are directed towards the observer.