This file was created by the TYPO3 extension publications --- Timezone: CEST Creation date: 2026-03-14 Creation time: 20:15:52 --- Number of references 446 article The Solar Orbiter mission completed its first remote-sensing observation windows in the spring of 2022. On 2 April 2022, an M-class flare followed by a filament eruption was seen both by the instruments on board the mission and from several observatories in Earth's orbit, providing an unprecedented view of a flaring region with a large range of observations. Aims: We aim to understand the nature of the flaring and filament eruption events via the analysis of the available dataset. The complexity of the observed features is compared with the predictions given by the standard flare model in 3D. Methods: In this paper, we use the observations from a multi-view dataset, which includes extreme ultraviolet (EUV) imaging to spectroscopy and magnetic field measurements. These data come from the Interface Region Imaging Spectrograph, the Solar Dynamics Observatory, Hinode, as well as several instruments on Solar Orbiter. Results: The large temporal coverage of the region allows us to analyse the whole sequence of the filament eruption starting with its pre-eruptive state. Information given by spectropolarimetry from SDO/HMI and Solar Orbiter PHI/HRT shows that a parasitic polarity emerging underneath the filament is responsible for bringing the flux rope to an unstable state. As the flux rope erupts, Hinode EIS captures blue-shifted emission in the transition region and coronal lines in the northern leg of the flux rope prior to the flare peak. This may be revealing the unwinding of one of the flux rope legs. At the same time, Solar Orbiter SPICE captures the whole region, complementing the Doppler diagnostics of the filament eruption. Analyses of the formation and evolution of a complex set of flare ribbons and loops, of the hard and soft X-ray emissions with STIX, show that the parasitic emerging bipole plays an important role in the evolution of the flaring region. Conclusions: The extensive dataset covering this M-class flare event demonstrates how important multiple viewpoints and varied observations are in order to understand the complexity of flaring regions. While the analysed data are overall consistent with the standard flare model, the present particular magnetic configuration shows that surrounding magnetic activity such as nearby emergence needs to be taken into account to fully understand the processes at work. This filament eruption is the first to be covered from different angles by spectroscopic instruments, and provides an unprecedented diagnostic of the multi-thermal structures present before and during the flare. This complete dataset of an eruptive event showcases the capabilities of coordinated observations with the Solar Orbiter mission. Movies associated with Figs 7, 9, 11, and 15 are available at https://www.aanda.org. 2023 September 10.1051/0004-6361/202346321 Astronomy & Astrophysics 677 https://ui.adsabs.harvard.edu/abs/2023A%26A...677A.130J M. Janvier S. Mzerguat P. R. Young E. Buchlin A. Manou Gabriel Pelouze D. M. Long L. Green A. Warmuth F. Schuller Pascal Démoulin D. Calchetti F. Kahil L. R. Bellot Rubio S. Parenti S. Baccar K. Barczynski L. K. Harra L. A. Hayes W. T. Thompson D. Müller D. Baker Stephanie L. Yardley D. Berghmans C. Verbeeck Phil Smith H. Peter R. Aznar Cuadrado S. Musset David H. Brooks L. Rodriguez F. Auchère M. Carlsson A. Fludra D. M. Hassler D. Williams Martin Caldwell Terje Fredvik A. Giunta T. Grundy Steve Guest E. Kraaikamp Sarah Leeks Joseph Plowman Werner Schmutz U. Schühle S. Sidher S. K. Solanki J. C. Del Toro Iniesta J. Woch A. Gandorfer J. Hirzberger D. Orozco Suárez T. Appourchaux G. Valori J. Sinjan K. Albert R. Volkmer article Kaithakkal2023 2023 10.1093/mnras/stad759 Monthly Notices of the Royal Astronomical Society 521 3882-3897 https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.3882K A. J. Kaithakkal J. M. Borrero A. P. Yabar J. Cruz Rodríguez article We identify a set of ~100 "cold" solar flares and perform a statistical analysis of them in the microwave range. Cold flares are characterized by a weak thermal response relative to nonthermal emission. This work is a follow-up of a previous statistical study of cold flares, which focused on hard X-ray emission to quantify the flare nonthermal component. Here, we focus on the microwave emission. The thermal response is evaluated by the soft X-ray emission measured by the GOES X-ray sensors. We obtain spectral parameters of the flare gyrosynchrotron emission and reveal patterns of their temporal evolution. The main results of the previous statistical study are confirmed: as compared to a "mean" flare, the cold flares have shorter durations, higher spectral peak frequencies, and harder spectral indices above the spectral peak. Nonetheless, there are some cold flares with moderate and low peak frequencies. In the majority of cold flares, we find evidence of the Razin effect in the microwave spectra, indicative of rather dense flaring loops. We discuss the results in the context of the electron acceleration efficiency. 2023 September 10.3847/1538-4357/acea20 The Astrophysical Journal 954 https://ui.adsabs.harvard.edu/abs/2023ApJ...954..122L/ S. M. White G. G. Motorina G. D. Fleishman Alexandra L. Lysenko Dmitry A. Zhdanov Nataliia S. Meshalkina Aleksander T. Altyntsev article Borrero2023 2023 10.1051/0004-6361/202244716 Astronomy and Astrophysics 669 A122 https://ui.adsabs.harvard.edu/abs/2023A&A...669A.122B J. M. Borrero A. Pastor Yabar article Solar flares are driven by the release of free magnetic energy and its conversion to other forms of energy-kinetic, thermal, and nonthermal. Quantification of partitions between these energy components and their evolution is needed to understand the solar flare phenomenon including nonthermal particle acceleration, transport, and escape as well as the thermal plasma heating and cooling. The challenge of remote-sensing diagnostics is that the data are taken with finite spatial resolution and suffer from line-of-sight (LOS) ambiguity including cases when different flaring loops overlap and project one over the other. Here, we address this challenge by devising a data-constrained evolving 3D model of a multiloop SOL2014-02-16T064620 solar flare of GOES class C1.5. Specifically, we employed a 3D magnetic model validated earlier for a single time frame and extended it to cover the entire flare evolution. For each time frame we adjusted the distributions of the thermal plasma and nonthermal electrons in the model so that the observables synthesized from the model matched the observations. Once the evolving model had been validated in this way, we computed and investigated the evolving energy components and other relevant parameters by integrating over the model volume. This approach removes the LOS ambiguity and permits us to disentangle contributions from the overlapping loops. It reveals new facets of electron acceleration and transport as well as of the heating and cooling of the flare plasma in 3D. We find signatures of substantial direct heating of the flare plasma not associated with the energy loss of nonthermal electrons. 2023 August 10.3847/1538-4357/ace1f4 The Astrophysical Journal 953 https://ui.adsabs.harvard.edu/abs/2023ApJ...953..174F/ G. D. Fleishman G. M. Nita G. G. Motorina article To facilitate the study of solar flares and active regions, we have created a modeling framework, the freely distributed GX Simulator IDL package, that combines 3D magnetic and plasma structures with thermal and nonthermal models of the chromosphere, transition region, and corona. Its object-based modular architecture, which runs on Windows, Mac, and Unix/Linux platforms, offers the ability to either import 3D density and temperature distribution models, or to assign numerically defined coronal or chromospheric temperatures and densities, or their distributions, to each individual voxel. GX Simulator can apply parametric heating models involving average properties of the magnetic field lines crossing a given voxel, as well as compute and investigate the spatial and spectral properties of radio, (sub)millimeter, EUV, and X-ray emissions calculated from the model, and quantitatively compare them with observations. The package includes a fully automatic model production pipeline that, based on minimal users input, downloads the required SDO/HMI vector magnetic field data, performs potential or nonlinear force-free field extrapolations, populates the magnetic field skeleton with parameterized heated plasma coronal models that assume either steady-state or impulsive plasma heating, and generates non-LTE density and temperature distribution models of the chromosphere that are constrained by photospheric measurements. The standardized models produced by this pipeline may be further customized through specialized IDL scripts, or a set of interactive tools provided by the graphical user interface. Here, we describe the GX Simulator framework and its applications. 2023 July 10.3847/1538-4365/acd343 The Astrophysical Journal Supplement Series 267 https://ui.adsabs.harvard.edu/abs/2023ApJS..267....6N G. M. Nita G. D. Fleishman A. Kuznetsov Sergey A. Anfinogentov Alexey G. Stupishin E. P. Kontar Samuel J. Schonfeld James A. Klimchuk Dale E. Gary article The intermediate stages between pores and the formation of sunspots are a rare phenomenon and can be manifested as transient photospheric penumbral-like filaments. Although the magnetic field changes rapidly during the evolution of such filaments, they have not yet been shown to be connected to magnetic reconnection events. Aims: We characterize the evolution of transient photospheric filaments around a pore and search for possible signs of chromospheric responses. Methods: We analyzed observations of a pore in NOAA AR 12739 from the Swedish Solar Telescope, including the spectropolarimetric data of the Fe I 6173 Å and the Ca II 8542 Å line and spectroscopic data of the Ca II K 3934 Å line. The VFISV Milne-Eddington inversion code and the multi-line non-LTE inversion code STiC were utilized to obtain atmospheric parameters in the photosphere and the chromosphere. Results: Multiple filamentary structures of inclined magnetic fields are found in photospheric inclination maps at the boundary of the pore, although the pore had never developed a penumbra. One of the filaments shows a clear counterpart in continuum intensity maps, in addition to photospheric blueshifts. During its decay, a brightening in the blue wing of the Ca II 8542 Å line is observed. The Ca II K 3934 Å and the Ca II 8542 Å lines show complex spectral profiles in this region. Depth-dependent STiC inversion results using data from all available lines yield a temperature increase (roughly 1000 K) and bidirectional flows (magnitudes up to 8 km s−1) at log τ = −3.5. Conclusions: The temporal and spatial correlations of the decaying filament (observed in the photosphere) to the temperature increase and the bidirectional flows in the high photosphere and low chromosphere suggest that they are connected. We propose scenarios in which magnetic reconnection happens at the edge of a rising magnetic flux tube in the photosphere. This would lead to both the decay of the filament in the photosphere as well as the observed temperature increase and the bidirectional flows in the high photosphere and low chromosphere. 2023 March 1 10.1051/0004-6361/202245703 Astronomy & Astrophysics 673 id.A65, 15 pp. https://ui.adsabs.harvard.edu/abs/2023A%26A...673A..65L/abstract P. Lindner R. Schlichenmaier N. Bello González J. Cruz Rodríguez article Earth-side observations of solar p modes can be used to image and monitor magnetic activity on the Sun's far side. In this work, we use magnetograms of the far side obtained by the Polarimetric and Helioseismic Imager (PHI) on board Solar Orbiter (SO) to directly assess the validity of far-side helioseismic holography for the first time. Aims: We wish to co-locate the positions of active regions in helioseismic images and magnetograms and to calibrate the helioseismic measurements in terms of the magnetic field strength. Methods: We identified three magnetograms displaying a total of six active regions on the far side from 18 November 2020, 3 October 2021, and 3 February 2022. The first two dates are from the SO cruise phase and the third is from the beginning of the nominal operation phase. We computed contemporaneous seismic phase maps for these three dates using helioseismic holography applied to the time series of Dopplergrams from the Helioseismic and Magnetic Imager (HMI) at the Solar Dynamics Observatory (SDO). Results: Among the six active regions seen in SO/PHI magnetograms, five of them are identified on the seismic maps at almost the same positions as on the magnetograms. One region is too weak to be detected above the seismic noise. To calibrate the seismic maps, we fit a linear relationship between the seismic phase shifts and the unsigned line-of-sight magnetic field averaged over the active region areas extracted from the SO/PHI magnetograms. Conclusions: SO/PHI provides the strongest evidence so far that helioseismic imaging is able to provide reliable information on active regions on the far side, including their positions, areas, and the mean unsigned magnetic field. 2023 June 10.1051/0004-6361/202346030 Astronomy & Astrophysics 674 https://ui.adsabs.harvard.edu/abs/2023A%26A...674A.183Y D. Yang L. Gizon H. Barucq J. Hirzberger D. Orozco Suárez K. Albert N. Albelo Jorge T. Appourchaux A. Álvarez-Herrero J. Blanco Rodríguez A. Gandorfer D. Germerott L. Guerrero P. Gutierrez-Marques F. Kahil M. Kolleck S. K. Solanki J. C. Del Toro Iniesta R. Volkmer J. Woch I. Pérez Grande E. Sanchis Kilders M. Balaguer Jiménez L. R. Bellot Rubio D. Calchetti M. Carmona W. Deutsch A. Feller G. Fernandez-Rico A. Fernández-Medina P. García Parejo J. L. Gasent Blesa B. Grauf K. Heerlein A. Korpi-Lagg T. Lange A. C. López Jiménez T. Maue R. Meller E. Moreno R. Müller E. Nakai W. Schmidt J. Schou U. Schühle J. Sinjan J. Staub H. Strecker I. Torralbo G. Valori article Berdyugin2023 2023 10.1051/0004-6361/202245149 Astronomy and Astrophysics 670 A2 https://ui.adsabs.harvard.edu/abs/2023A&A...670A...2B A. V. Berdyugin V. Piirola S. Bagnulo J. D. Landstreet S. V. Berdyugina article Schlichenmaier2023 2023 10.1051/0004-6361/202244640 Astronomy and Astrophysics 669 A78 https://ui.adsabs.harvard.edu/abs/2023A&A...669A..78S R. Schlichenmaier D. Pitters J. M. Borrero M. Schubert article The centrifugal force is often omitted from simulations of stellar convection either for numerical reasons or because it is assumed to be weak compared to the gravitational force. However, the centrifugal force might be an important factor in rapidly rotating stars, such as solar analogs, due to its Ω2 scaling, where Ω is the rotation rate of the star. Aims: We study the effects of the centrifugal force in a set of 21 semi-global stellar dynamo simulations with varying rotation rates. Included in the set are three control runs aimed at distinguishing the effects of the centrifugal force from the nonlinear evolution of the solutions. Methods: We solved the 3D magnetohydrodynamic equations with the PENCIL CODE in a solar-like convective zone in a spherical wedge setup with a 2π azimuthal extent. The rotation rate and the amplitude of the centrifugal force were varied. We decomposed the magnetic field into spherical harmonics and studied the migration of azimuthal dynamo waves (ADWs), the energy of different large-scale magnetic modes, and differential rotation. Results: In the regime with the lowest rotation rates, Ω = 5 - 10 Ω⊙, where Ω⊙ is the rotation rate of the Sun, we see no marked changes in either the differential rotation or the magnetic field properties. For intermediate rotation, Ω = 20 - 25 Ω⊙, we identify an increase in the differential rotation as a function of centrifugal force. The axisymmetric magnetic energy tends to decrease with centrifugal force, while the non-axisymmetric one increases. The ADWs are also affected, especially in the propagation direction. In the most rapidly rotating set with Ω = 30 Ω⊙, these changes are more pronounced, and in one case the propagation direction of the ADW changes from prograde to retrograde. The control runs suggest that the results are a consequence of the centrifugal force and not due to the details of the initial conditions or the history of the run. Conclusions: We find that the differential rotation and properties of the ADWs only change as a function of the centrifugal force when rotation is rapid enough. 2023 October 10.1051/0004-6361/202346768 Astronomy & Astrophysics 678 https://ui.adsabs.harvard.edu/abs/2023A%26A...678A...9N P. J. Käpylä F. H. Navarrete D. R. G. Schleicher Robi Banerjee article Ishikawa2023 2023 10.3847/1538-4357/acb64e The Astrophysical Journal 945 125 https://ui.adsabs.harvard.edu/abs/2023ApJ...945..125I R. Ishikawa J. Trujillo Bueno E. Alsina Ballester L. Belluzzi T. Pino Alemán D. E. McKenzie F. Auchère K. Kobayashi T. J. Okamoto L. A. Rachmeler D. Song article Arch-like loop structures filled with million Kelvin hot plasma form the building blocks of the quiet-Sun corona. Both high-resolution observations and magnetoconvection simulations show the ubiquitous presence of magnetic fields on the solar surface on small spatial scales of ~100 km. However, the question of how exactly these quiet-Sun coronal loops originate from the photosphere and how the magnetic energy from the surface is channeled to heat the overlying atmosphere is a long-standing puzzle. Here we report high-resolution photospheric magnetic field and coronal data acquired during the second science perihelion of Solar Orbiter that reveal a highly dynamic magnetic landscape underlying the observed quiet-Sun corona. We found that coronal loops often connect to surface regions that harbor fleeting weaker, mixed-polarity magnetic field patches structured on small spatial scales, and that coronal disturbances could emerge from these areas. We suggest that weaker magnetic fields with fluxes as low as 1015 Mx and/or those that evolve on timescales less than 5 minutes are crucial to understanding the coronal structuring and dynamics. 2023 October 10.3847/2041-8213/acf136 The Astrophysical Journal Letters 956 https://ui.adsabs.harvard.edu/abs/2023ApJ...956L...1C/abstract L. P. Chitta S. K. Solanki J. Woch D. Calchetti A. Gandorfer J. Hirzberger F. Kahil G. Valori D. Orozco Suárez H. Strecker T. Appourchaux R. Volkmer H. Peter Sudip Mandal R. Aznar Cuadrado L. Teriaca U. Schühle D. Berghmans C. Verbeeck A. N. Zhukov E. R. Priest article The brightness of faculae and network depends on the angle at which they are observed and the magnetic flux density. Close to the limb, the assessment of this relationship has until now been hindered by the increasingly lower signal in magnetograms. Aims: This preliminary study aims to highlight the potential of using simultaneous observations from different vantage points to better determine the properties of faculae close to the limb. Methods: We used data from the Solar Orbiter/Polarimetric and Helioseismic Imager (SO/PHI), and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager (SDO/HMI), recorded at an ?60° angular separation of their lines of sight at the Sun. We used the continuum intensity observed close to the limb by SO/PHI and complemented it with the co-observed BLOS from SDO/HMI, originating closer to disc centre (as seen by SDO/HMI), thus avoiding the degradation of the magnetic field signal near the limb. Results: We derived the dependence of facular brightness in the continuum on disc position and magnetic flux density from the combined observations of SO/PHI and SDO/HMI. Compared with a single point of view, we were able to obtain contrast values reaching closer to the limb and to lower field strengths. We find the general dependence of the limb distance at which the contrast is maximum on the flux density to be at large in line with single viewpoint observations, in that the higher the flux density is, the closer the turning point lies to the limb. There is a tendency, however, for the maximum to be reached closer to the limb when determined from two vantage points. We note that due to the preliminary nature of this study, these results must be taken with caution. Conclusions: Our analysis shows that studies involving two viewpoints can significantly improve the detection of faculae near the solar limb and the determination of their brightness contrast relative to the quiet Sun. 2023 October 10.1051/0004-6361/202346037 Astronomy & Astrophysics 678 https://ui.adsabs.harvard.edu/abs/2023A%26A...678A.163A K. Albert N. Krivova J. Hirzberger S. K. Solanki A. Moreno Vacas D. Orozco Suárez N. Albelo Jorge T. Appourchaux A. Álvarez-Herrero J. Blanco Rodríguez A. Gandorfer P. Gutierrez-Marques F. Kahil M. Kolleck R. Volkmer J. C. Del Toro Iniesta J. Woch B. Fiethe I. Pérez Grande E. Sanchis Kilders M. Balaguer Jiménez L. R. Bellot Rubio D. Calchetti M. Carmona W. Deutsch A. Feller G. Fernandez-Rico A. Fernández-Medina P. García Parejo J. L. Gasent Blesa L. Gizon B. Grauf K. Heerlein A. Korpi-Lagg T. Lange A. López Jiménez T. Maue R. Meller R. Müller E. Nakai W. Schmidt J. Schou J. Sinjan J. Staub H. Strecker I. Torralbo G. Valori article We study the extent to which Milne-Eddington inversions are able to retrieve and characterize the magnetic landscape of the solar poles from observations by the spectropolarimeter on board Hinode. In particular, we evaluate whether a variable magnetic filling factor is an adequate modeling technique for retrieving the intrinsic magnetic properties from every pixel in the polar field of view. We first generate synthetic spectra emerging from a numerical simulation of a "plage" region at an inclined line of sight of 65°, and degrade the data to emulate real observations. Then, we invert the synthetic spectra with two Milne-Eddington inversion codes that feature different treatments of the magnetic filling factor, and relate the retrieved magnetic quantities back to their original values in the simulation cube. We find that, while the apparent retrieved magnetic properties map the spatially degraded simulation well, the intrinsic magnetic quantities bear little relation to the magnetic field at the native resolution of the simulation. We discuss the systematic biases caused by line-of-sight foreshortening, spatial degradation, photon noise, and modeling assumptions embedded in the inversion algorithm. 2023 July 10.3847/1538-4357/acd178 The Astrophysical Journal 951 https://ui.adsabs.harvard.edu/abs/2023ApJ...951...23C/ I. Milić M. Rempel X. Sun Rebecca Canteno Nariaki V. Nitta article Umbral chromospheric observations show the presence of magnetoacoustic shocks. Several recent studies have reported magnetic field fluctuations associated with these shock waves. The mechanism behind these periodic magnetic field changes is still an unresolved question. Aims: We aim to study the properties and origin of magnetic field fluctuations in the umbral chromosphere. Methods: Temporal series of spectropolarimetric observations were acquired with the GREGOR telescope on 2017 June 18. The chromospheric and photospheric conditions, including the temporal evolution of the magnetic field, were derived from simultaneous inversions of the He I 10 830 Å triplet and the Si I 10 827 Å line using the HAZEL2 code. The oscillations were interpreted using wavelet analysis and context information from ultraviolet observations acquired with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO/AIA) and the Interface Region Imaging Spectrograph (IRIS). Results: The chromospheric magnetic field shows strong fluctuations in the sunspot umbra, with peak field strengths of up to 2900 G. This inferred field strength is comparable to the magnetic field strength in the upper photosphere. Magnetic field and velocity umbral oscillations exhibit a strong coherence, with the magnetic field lagging the shock fronts detected in the velocity fluctuations. This points to a common origin of the fluctuations in both parameters, and the analysis of the phase shift between photospheric and chromospheric velocity is consistent with upward wave propagation. These results suggest that the strong inferred magnetic field fluctuations are caused by changes in the response height of the He I 10 830 Å line to the magnetic field, which is sensitive to the high photosphere during and right after the shock. The analysis of extreme ultraviolet data shows a weak brightening in a coronal loop rooted in the umbra around the time of the measured magnetic field fluctuations. This coronal activity could possibly have some impact on the inferred fluctuations, but it is not the main driver of the magnetic field oscillations since they are found before the extreme ultraviolet event takes place. Conclusions: Chromospheric magnetic field fluctuations measured with the He I 10 830 Å triplet arise due to variations in the opacity of the line. After strong shocks are produced by the propagation of slow magnetoacoustic waves, the response of the line to the magnetic field can be shifted down to the upper photosphere. This is seen as remarkably large fluctuations in the line-of-sight magnetic field strength. 2023 August 10.1051/0004-6361/202244519 Astronomy & Astrophysics 676 https://ui.adsabs.harvard.edu/abs/2023A%26A...676A..77F T. Felipe S. J. González Manrique A. Asensio Ramos C. R. Sangeetha article The High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager on board the Solar Orbiter spacecraft (SO/PHI) and the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) both infer the photospheric magnetic field from polarised light images. SO/PHI is the first magnetograph to move out of the Sun-Earth line and will provide unprecedented access to the Sun's poles. This provides excellent opportunities for new research wherein the magnetic field maps from both instruments are used simultaneously. Aims: We aim to compare the magnetic field maps from these two instruments and discuss any possible differences between them. Methods: We used data from both instruments obtained during Solar Orbiter's inferior conjunction on 7 March 2022. The HRT data were additionally treated for geometric distortion and degraded to the same resolution as HMI. The HMI data were re-projected to correct for the 3° separation between the two observatories. Results: SO/PHI-HRT and HMI produce remarkably similar line-of-sight magnetograms, with a slope coefficient of 0.97, an offset below 1 G, and a Pearson correlation coefficient of 0.97. However, SO/PHI-HRT infers weaker line-of-sight fields for the strongest fields. As for the vector magnetic field, SO/PHI-HRT was compared to both the 720-second and 90-second HMI vector magnetic field: SO/PHI-HRT has a closer alignment with the 90-second HMI vector. In the weak signal regime (< 600 G), SO/PHI-HRT measures stronger and more horizontal fields than HMI, very likely due to the greater noise in the SO/PHI-HRT data. In the strong field regime (≳600 G), HRT infers lower field strengths but with similar inclinations (a slope of 0.92) and azimuths (a slope of 1.02). The slope values are from the comparison with the HMI 90-second vector. Possible reasons for the differences found between SO/PHI-HRT and HMI magnetic field parameters are discussed. 2023 May 10.1051/0004-6361/202245830 Astronomy & Astrophysics 673 https://ui.adsabs.harvard.edu/abs/2023A%26A...673A..31S J. Sinjan D. Calchetti J. Hirzberger F. Kahil G. Valori S. K. Solanki K. Albert N. Albelo Jorge A. Álvarez-Herrero T. Appourchaux L. R. Bellot Rubio J. Blanco Rodríguez A. Feller A. Gandorfer D. Germerott L. Gizon J. M. Gómez Cama L. Guerrero M. Kolleck A. Korpi-Lagg H. Michalik A. Moreno Vacas D. Orozco Suárez I. Pérez-Grande E. Sanchis Kilders M. Balaguer Jiménez J. Schou U. Schühle J. Staub H. Strecker J. C. Del Toro Iniesta R. Volkmer J. Woch article Waidele2023 2023 10.1007/s11207-023-02124-7 Solar Physics 298 30 https://ui.adsabs.harvard.edu/abs/2023SoPh..298...30W M. Waidele M. Roth N. K. Singh P. J. Käpylä article The understanding of the solar magnetic coronal structure is tightly linked to the shape of open field regions, specifically coronal holes. A dynamically evolving coronal hole coincides with the local restructuring of open to closed magnetic field, which leads to changes in the interplanetary solar wind structure. By investigating the dynamic evolution of a fast-tilting coronal hole, we strive to uncover clues about what processes may drive its morphological changes, which are clearly visible in EUV filtergrams. Using combined 193A and 195A EUV observations by AIA/SDO and EUVI/STEREO_A, in conjunction with line-of-sight magnetograms taken by HMI/SDO, we track and analyze a coronal hole over 12 days to derive changes in morphology, area and magnetic field. We complement this analysis by potential field source surface modeling to compute the open field structure of the coronal hole. We find that the coronal hole exhibits an apparent tilting motion over time that cannot solely be explained by solar differential rotation. It tilts at a mean rate of ~3.2°/day that accelerates up to ~5.4°/day. At the beginning of May, the area of the coronal hole decreases by more than a factor of three over four days (from ~13 * 10^9 km^2 to ~4 * 10^9 km^2), but its open flux remains constant (~2 * 10^20 Mx). Further, the observed evolution is not reproduced by modeling that assumes the coronal magnetic field to be potential. In this study, we present a solar coronal hole that tilts at a rate that has yet to be reported in literature. The rate exceeds the effect of the coronal hole being advected by either photospheric or coronal differential rotation. Based on the analysis we find it likely that this is due to morphological changes in the coronal hole boundary caused by ongoing interchange reconnection and the interaction with a newly emerging ephemeral region in its vicinity. 2023 September 10.48550/arXiv.2309.11100 eprint arXiv:2309.11100 https://ui.adsabs.harvard.edu/abs/2023arXiv230911100H Stephan G. Heinemann James A. Turtle Jens Pomoell Eleanna Asvestari A. C. Sterling A. Diercke Cooper Downs article We present high-precision optical polarimetric observations of the black hole X-ray binary Cygnus X-1 that span several cycles of its 5.6-day orbital period. The week-long observations on two telescopes located in opposite hemispheres allowed us to track the evolution of the polarization within one orbital cycle with the highest temporal resolution to date. Using the field stars, we determined the interstellar polarization in the source direction and subsequently its intrinsic polarization Pint = 0.82%±0.15% with a polarization angle ?int = 155° ±5°. The optical polarization angle is aligned with that in the X-rays recently obtained with the Imaging X-ray Polarimetry Explorer. Furthermore, it is consistent within the uncertainties with the position angle of the radio ejections. We show that the intrinsic polarization degree is variable with the orbital period with an amplitude of ?0.2% and discuss various sites of its production. Assuming that the polarization arises from a single Thomson scattering of the primary star radiation by the matter that follows the black hole in its orbital motion, we constrained the inclination of the binary orbit i > 120° and its eccentricity e < 0.08. The asymmetric shape of the orbital profiles of the Stokes parameters also implies the asymmetry of the scattering matter distribution in the orbital plane, which may arise from the tilted accretion disk. We compared our data to the polarimetric observations made in 1975-1987 and find good agrement within 1° between the intrinsic polarization angles. On the other hand, the polarization degree decreased by 0.4% over half a century, suggesting secular changes in the geometry of the accreting matter. 2023 October 10.1051/0004-6361/202346932 Astronomy & Astrophysics 678 https://ui.adsabs.harvard.edu/abs/2023A%26A...678A..58K V. Kravtsov A. V. Berdyugin Andrzej A. Zdziarski Gary D. Henson V. Piirola T. Sakanoi M. Kagitani S. V. Berdyugina J. Poutanen article Magnetic flux emergence and cancelling in the quiet Sun is a frequently observed phenomenon. The two possible physical flux-removal mechanisms involved in this cancelling process are retraction and reconnection. Aims: We seek to find distinct observational signatures characterising retraction and reconnection. Methods: We carried out three-dimensional non-grey radiative magnetohydrodynamic (MHD) simulations of convection near the solar surface and the solar photosphere using the STAGGER code, and employing different initial conditions: (1) mixed-polarity simulations with alternating horizontal stripes of opposite vertical magnetic field and separated by a zero field stripe, and (2) flux emergence simulations with continuous injection of magnetic flux from the lower boundary. These initial conditions are meant to represent two different situations in the solar photosphere, namely magnetic flux cancelling in the absence or presence of magnetic flux emergence, respectively. Results: We analyse the observational signatures of magnetic flux-removal processes for flux emergence as well as for mixed-polarity MHD simulations. In the flux emergence simulation, we are able to identify ubiquitous reconnection events anywhere from the solar surface to the upper photosphere. For a few of those reconnection events, we can identify supersonic upflow velocities in the upper photosphere as well as strong temperature enhancements. We also see strong electric currents very close to the locations where reconnection takes place, as well as supersonic horizontal velocities leading to sideways plasma compression. In the mixed-polarity simulations, we only detect observational signatures of magnetic field retraction related to large downflow velocities that appear in between regions where opposing horizontal velocities converge. These horizontal velocities are often supersonic, leading to heating due to shock dissipation. We do not see clear signatures of magnetic reconnection in these mixed-polarity simulations. Conclusions: We suggest that, in the emerging flux regions of the quiet Sun, the main flux-removal process is reconnection, while in regions without flux emergence, retraction is the dominant flux-removal process. 2023 May 10.1051/0004-6361/202245701 Astronomy & Astrophysics 673 https://ui.adsabs.harvard.edu/abs/2023A%26A...673A.163T I. Thaler J. M. Borrero article Poynting flux is the flux of magnetic energy, which is responsible for chromospheric and coronal heating in the solar atmosphere. It is defined as a cross product of the electric and magnetic fields, and in ideal MHD conditions it can be expressed in terms of the magnetic field and plasma velocity. Poynting flux has been computed for active regions and plages, but estimating it in the quiet Sun (QS) remains challenging due to resolution effects and polarimetric noise. However, with the upcoming DKIST capabilities, such estimations will become more feasible than ever before. Here, we study QS Poynting flux in SUNRISE/IMaX observations and MURaM simulations. We explore two methods for inferring transverse velocities from observations-FLCT and a neural network-based method DeepVel-and show DeepVel to be the more suitable method in the context of small-scale QS flows. We investigate the effect of azimuthal ambiguity on Poynting flux estimates, and we describe a new method for azimuth disambiguation. Finally, we use two methods for obtaining the electric field. The first method relies on an idealized Ohm's law, whereas the second is a state-of-the-art inductive electric field inversion method PDFI_SS. We compare the resulting Poynting flux values with theoretical estimates for chromospheric and coronal energy losses and find that some of the Poynting flux estimates are sufficient to match the losses. Using MURaM simulations, we show that photospheric Poynting fluxes vary significantly with optical depth, and that there is an observational bias that results in underestimated Poynting fluxes due to an unaccounted shear term contribution. 2023 October 10.3847/1538-4357/ace621 The Astrophysical Journal 956 https://ui.adsabs.harvard.edu/abs/2023ApJ...956...83T/ M. D. Kazachenko P.-E. Tremblay I. Milić V. Martínez Pillet M. Rempel Dennis Tilipman article Aims: The aim of this study is to explore the magnetic and flow properties of fully convective M dwarfs as a function of rotation period Prot and magnetic Reynolds ReM and Prandlt numbers PrM. Methods: We performed three-dimensional simulations of fully convective stars using a star-in-a-box set-up. This set-up allows global dynamo simulations in a sphere embedded in a Cartesian cube. The equations of non-ideal magnetohydrodynamics were solved with the PENCIL CODE. We used the stellar parameters of an M5 dwarf with 0.21 M⊙ at three rotation rates corresponding to rotation periods (Prot) of 43, 61, and 90 days, and varied the magnetic Prandtl number in the range from 0.1 to 10. Results: We found systematic differences in the behaviour of the large-scale magnetic field as functions of rotation and PrM. For the simulations with Prot = 43 days and PrM ≤ 2, we found cyclic large-scale magnetic fields. For PrM > 2, the cycles vanish and the field shows irregular reversals. In the simulations with Prot = 61 days for PrM ≤ 2, the cycles are less clear and the reversal are less periodic. In the higher PrM cases, the axisymmetric mean field shows irregular variations. For the slowest rotation case with Prot = 90 days, the field has an important dipolar component for PrM ≤ 5. For the highest PrM the large-scale magnetic field is predominantly irregular at mid-latitudes, with quasi-stationary fields near the poles. For the simulations with cycles, the cycle period length slightly increases with increasing ReM. 2023 October 10.1051/0004-6361/202244666 Astronomy & Astrophysics 678 P. J. Käpylä C. A. Ortiz-Rodríguez F. H. Navarrete D. R. G. Schleicher R. E. Mennickent J. P. Hidalgo B. Toro-Velásquez article We review the state of the art of three dimensional numerical simulations of solar and stellar dynamos. We summarize fundamental constraints of numerical modelling and the techniques to alleviate these restrictions. Brief summary of the relevant observations that the simulations seek to capture is given. We survey the current progress of simulations of solar convection and the resulting large-scale dynamo. We continue to studies that model the Sun at different ages and to studies of stars of different masses and evolutionary stages. Both simulations and observations indicate that rotation, measured by the Rossby number which is the ratio of rotation period and convective turnover time, is a key ingredient in setting the overall level and characteristics of magnetic activity. Finally, efforts to understand global 3D simulations in terms of mean-field dynamo theory are discussed. 2023 October 10.1007/s11214-023-01005-6 Space Science Reviews 219 https://ui.adsabs.harvard.edu/abs/2023SSRv..219...58K P. J. Käpylä Matthew K. Browning A. S. Brun Gustavo Guerrero J. Warnecke article The Slow Solar Wind Connection Solar Orbiter Observing Plan (Slow Wind SOOP) was developed to utilize the extensive suite of remote-sensing and in situ instruments on board the ESA/NASA Solar Orbiter mission to answer significant outstanding questions regarding the origin and formation of the slow solar wind. The Slow Wind SOOP was designed to link remote-sensing and in situ measurements of slow wind originating at open-closed magnetic field boundaries. The SOOP ran just prior to Solar Orbiter's first close perihelion passage during two remote-sensing windows (RSW1 and RSW2) between 2022 March 3-6 and 2022 March 17-22, while Solar Orbiter was at respective heliocentric distances of 0.55-0.51 and 0.38-0.34 au from the Sun. Coordinated observation campaigns were also conducted by Hinode and IRIS. The magnetic connectivity tool was used, along with low-latency in situ data and full-disk remote-sensing observations, to guide the target pointing of Solar Orbiter. Solar Orbiter targeted an active region complex during RSW1, the boundary of a coronal hole, and the periphery of a decayed active region during RSW2. Postobservation analysis using the magnetic connectivity tool, along with in situ measurements from MAG and SWA/PAS, showed that slow solar wind originating from two out of three of the target regions arrived at the spacecraft with velocities between ~210 and 600 km s-1. The Slow Wind SOOP, despite presenting many challenges, was very successful, providing a blueprint for planning future observation campaigns that rely on the magnetic connectivity of Solar Orbiter. 2023 July 10.3847/1538-4365/acd24b The Astrophysical Journal Supplement Series 267 https://ui.adsabs.harvard.edu/abs/2023ApJS..267...11Y Stephanie L. Yardley C. J. Owen D. M. Long D. Baker David H. Brooks Vanessa Polito L. Green S. Matthews M. Owens Mike Lockwood D. Stansby A. W. James G. Valori A. Giunta M. Janvier Nawin Ngampoopun Teodora Mihailescu Andy S. H. To Lidia van Driel-Gesztelyi Pascal Démoulin R. D'Amicis Ryan J. French Gabriel H. H. Suen A. P. Rouillard R. F. Pinto V. Reville Christopher J. Watson A. P. Walsh A. De Groof D. R. Williams I. Zouganelis D. Müller D. Berghmans F. Auchère L. Harra U. Schühle K. Barczynski E. Buchlin R. Aznar Cuadrado E. Kraaikamp Sudip Mandal S. Parenti H. Peter L. Rodriguez Conrad Schwanitz Phil Smith L. Teriaca C. Verbeeck A. N. Zhukov B. De Pontieu T. S. Horbury S. K. Solanki J. C. Del Toro Iniesta J. Woch A. Gandorfer J. Hirzberger D. Orozco Suárez T. Appourchaux D. Calchetti J. Sinjan F. Kahil K. Albert R. Volkmer M. Carlsson A. Fludra D. M. Hassler Martin Caldwell Terje Fredvik T. Grundy Steve Guest M. Haberreiter Sarah Leeks Gabriel Pelouze Joseph Plowman Werner Schmutz S. Sidher W. T. Thompson P. Louarn Andrei Federov article In November 2021, Solar Orbiter started its nominal mission phase. The remote-sensing instruments on board the spacecraft acquired scientific data during three observing windows surrounding the perihelion of the first orbit of this phase. Aims: The aim of the analysis is the detection of magnetohydrodynamic (MHD) wave modes in an active region by exploiting the capabilities of spectropolarimetric measurements. Mthods. The High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager (SO/PHI) on board the Solar Orbiter acquired a high-cadence data set of an active region. This is studied in the paper. B-ω and phase-difference analyses are applied on line-of-sight velocity and circular polarization maps and other averaged quantities. Results: We find that several MHD modes at different frequencies are excited in all analysed structures. The leading sunspot shows a linear dependence of the phase lag on the angle between the magnetic field and the line of sight of the observer in its penumbra. The magnetic pore exhibits global resonances at several frequencies, which are also excited by different wave modes. Conclusions: The SO/PHI measurements clearly confirm the presence of magnetic and velocity oscillations that are compatible with one or more MHD wave modes in pores and a sunspot. Improvements in modelling are still necessary to interpret the relation between the fluctuations of different diagnostics. 2023 June 10.1051/0004-6361/202245826 Astronomy & Astrophysics 674 https://ui.adsabs.harvard.edu/abs/2023A%26A...674A.109C D. Calchetti M. Stangalini S. Jafarzadeh G. Valori K. Albert N. Albelo Jorge A. Álvarez-Herrero T. Appourchaux M. Balaguer Jiménez L. R. Bellot Rubio J. Blanco Rodríguez A. Feller A. Gandorfer D. Germerott L. Gizon L. Guerrero P. Gutierrez-Marques J. Hirzberger F. Kahil M. Kolleck A. Korpi-Lagg A. Moreno Vacas D. Orozco Suárez I. Pérez-Grande E. Sanchis Kilders U. Schühle J. Schou J. Sinjan S. K. Solanki J. Staub H. Strecker J. C. Del Toro Iniesta R. Volkmer J. Woch article The magnetic field of the Sun is generated by internal dynamo process with a cyclic period of 11 years or a 22 year magnetic cycle. The signatures of the Sun's magnetic cycle are observed in the different layers of its atmosphere and in its internal layers. In this review, we use the same diagnostics to understand the magnetic cycles of other stars with the same internal structure as the Sun. We review what is currently known about mapping the surface magnetic fields, chromospheric and coronal indicators, cycles in photometry and asteroseismology. We conclude our review with an outlook for the future. 2023 October 10.1007/s11214-023-01000-x Space Science Reviews 219 https://ui.adsabs.harvard.edu/abs/2023SSRv..219...54J R. Kiefer Sandra V. Jeffers Travis S. Metcalfe article Contact. Spectropolarimetric reconstructions of the photospheric vector magnetic field are intrinsically limited by the 180° ambiguity in the orientation of the transverse component. So far, the removal of such an ambiguity has required assumptions about the properties of the photospheric field, which makes disambiguation methods model-dependent. Aims: The successful launch and operation of Solar Orbiter have made the removal of the 180° ambiguity possible solely using observations of the same location on the Sun obtained from two different vantage points. Methods: The basic idea is that the unambiguous line-of-sight component of the field measured from one vantage point will generally have a nonzero projection on the ambiguous transverse component measured by the second telescope, thereby determining the "true" orientation of the transverse field. Such an idea was developed and implemented as part of the stereoscopic disambiguation method (SDM), which was recently tested using numerical simulations. Results: In this work we present a first application of the SDM to data obtained by the High Resolution Telescope (HRT) on board Solar Orbiter during the March 2022 campaign, when the angle with Earth was 27 degrees. The method was successfully applied to remove the ambiguity in the transverse component of the vector magnetogram solely using observations (from HRT and from the Helioseismic and Magnetic Imager) for the first time. Conclusions: The SDM is proven to provide observation-only disambiguated vector magnetograms that are spatially homogeneous and consistent. A discussion on the sources of error that may limit the accuracy of the method, and strategies to remove them in future applications, is also presented. 2023 September 10.1051/0004-6361/202345859 Astronomy & Astrophysics 677 https://ui.adsabs.harvard.edu/abs/2023A%26A...677A..25V G. Valori D. Calchetti A. Moreno Vacas E. Pariat S. K. Solanki P. Löschl J. Hirzberger S. Parenti K. Albert N. Albelo Jorge A. Álvarez-Herrero T. Appourchaux L. R. Bellot Rubio J. Blanco Rodríguez J. I. Campos Rozo A. Feller A. Gandorfer P. García Parejo D. Germerott L. Gizon J. M. Gómez Cama L. Guerrero P. Gutierrez-Marques F. Kahil M. Kolleck A. Korpi-Lagg D. Orozco Suárez I. Pérez Grande E. Sanchis Kilders J. Schou U. Schühle J. Sinjan J. Staub H. Strecker J. C. Del Toro Iniesta R. Volkmer J. Woch article Rackham2023 2023 10.1093/rasti/rzad009 RAS Techniques and Instruments 2 148-206 https://ui.adsabs.harvard.edu/abs/2023RASTI...2..148R B. V. Rackham N. Espinoza S. V. Berdyugina H. Korhonen R. J. MacDonald B. T. Montet B. M. Morris M. Oshagh A. I. Shapiro Y. C. Unruh E. V. Quintana R. T. Zellem D. Apai T. Barclay J. K. Barstow G. Bruno L. Carone S. L. Casewell H. M. Cegla S. Criscuoli C. Fischer D. Fournier M. S. Giampapa H. Giles A. Iyer G. Kopp N. M. Kostogryz N. Krivova M. Mallonn C. McGruder K. Molaverdikhani E. R. Newton M. Panja S. Peacock K. Reardon R. M. Roettenbacher G. Scandariato S. Solanki K. G. Stassun O. Steiner K. B. Stevenson J. Tregloan-Reed A. Valio S. Wedemeyer L. Welbanks J. Yu M. K. Alam J. R. A. Davenport D. Deming C. Dong E. Ducrot C. Fisher E. Gilbert V. Kostov M. López-Morales M. Line T. Močnik S. Mullally R. R. Paudel I. Ribas J. A. Valenti article A better understanding of the processes involved in the energy transport across the solar atmosphere (e.g., jets, waves) demands more effort towards the observations. Hence, existing instruments may need to be upgraded to gain additional capabilities. To this effect, we conceive an upgrade for the HELioseismic Large Regions Interferometric DEvice (HELLRIDE) instrument at Vacuum Tower Telescope (VTT) to enable the recording of the magnetograms. We present the instrumentation aspects of this development consisting of integrating a liquid crystal-based dual-beam polarimeter with the existing instrument, compatible new hardware and software with the improved operating scheme, and the first observations to verify its functionality. The new HELLRIDE now observes a field of view of 90?×90? in four spectral lines, two chromospheric spectral lines in spectroscopy mode and two photospheric spectral lines in spectropolarimetry mode, with a cadence of 40 seconds. The increased complexity of the system, as well as the data, calls for the creation of a rigorous data processing pipeline, which is currently under development. 2023 March 10.1007/s11207-023-02138-1 Solar Physics 298 https://ui.adsabs.harvard.edu/abs/2023SoPh..298...41P Hemanth Pruthvi M. Roth article The intensity and the linear scattering polarization profiles of the hydrogen Ly? line encode valuable information on the thermodynamic and magnetic structure of the upper layers of the solar chromosphere. The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) sounding rocket experiment provided unprecedented spectropolarimetric data of this line, as well as two-dimensional broadband images in intensity and linear polarization. We theoretically investigate the potential of the Ly? broadband polarimetric signals for probing the solar chromosphere and its magnetic fields. We analyze the synthetic Stokes profiles obtained from a series of radiative transfer (RT) calculations out of local thermodynamic equilibrium, considering semi-empirical one-dimensional models of the solar atmosphere. The wavelength-integrated linear polarization signal is found to be dominated by the contribution from the wings when considering a Gaussian weighting function with a FWHM that corresponds to the CLASP slit-jaw broadband filter. These broadband linear polarization signals are strongly sensitive to magnetic fields of strengths on the order of 50 G, via the action of magneto-optical (MO) effects, and are expected to encode information on the middle-upper chromosphere. The two-dimensional broadband intensity and linear polarization images observed by CLASP can be suitably mimicked using synthetic wavelength-integrated signals obtained considering atmospheric models and magnetic fields that are representative of solar regions with different levels of activity, provided that the impact of MO effects is taken into account. Despite the limitations of a one-dimensional RT modeling, this work illustrates the diagnostic potential of filter-polarimetric Ly? signals for probing the solar chromosphere and its magnetism. 2023 April 10.3847/1538-4357/acc186 The Astrophysical Journal 947 https://ui.adsabs.harvard.edu/abs/2023ApJ...947...71A E. Alsina Ballester L. Belluzzi J. Trujillo Bueno article In order to make accurate inferences about the solar interior using helioseismology, it is essential to understand all the relevant physical effects on the observations. One effect to understand is the (complex-valued) ratio of the horizontal to vertical displacement of the p- and f-modes at the height at which they are observed. Unfortunately, it is impossible to measure this ratio directly from a single vantage point, and it has been difficult to disentangle observationally from other effects. In this paper we attempt to measure the ratio directly using 7.5 h of simultaneous observations from the Polarimetric and Helioseismic Imager on board Solar Orbiter and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. While image geometry problems make it difficult to determine the exact ratio, it appears to agree well with that expected from adiabatic oscillations in a standard solar model. On the other hand it does not agree with a commonly used approximation, indicating that this approximation should not be used in helioseismic analyses. In addition, the ratio appears to be real-valued. 2023 May 10.1051/0004-6361/202345946 Astronomy & Astrophysics 673 https://ui.adsabs.harvard.edu/abs/2023A%26A...673A..84S J. Schou J. Hirzberger D. Orozco Suárez K. Albert N. Albelo Jorge T. Appourchaux A. Álvarez-Herrero J. Blanco Rodríguez A. Gandorfer D. Germerott L. Guerrero F. Kahil M. Kolleck S. K. Solanki J. C. Del Toro Iniesta R. Volkmer J. Woch B. Fiethe I. Pérez Grande E. Sanchis Kilders M. Balaguer Jiménez P. García Parejo J. L. Gasent Blesa L. Gizon B. Grauf K. Heerlein A. Korpi-Lagg A. López Jiménez T. Maue R. Meller A. Moreno Vacas R. Müller E. Nakai W. Schmidt J. Sinjan J. Staub H. Strecker I. Torralbo G. Valori article Lindner2023 2023 May 10.1051/0004-6361/202245702 Astronomy and Astrophysics 673 A64 https://ui.adsabs.harvard.edu/abs/2023A&A...673A..64L P. Lindner C. Kuckein S. J. González Manrique N. Bello González L. Kleint T. Berkefeld article Tziotziou2023 2023 10.1007/s11214-022-00946-8 Space Science Reviews 219 1 https://ui.adsabs.harvard.edu/abs/2023SSRv..219....1T K. Tziotziou E. Scullion S. Shelyag O. Steiner E. Khomenko G. Tsiropoula J. R. Canivete Cuissa S. Wedemeyer I. Kontogiannis N. Yadav I. N. Kitiashvili S. J. Skirvin I. Dakanalis A. G. Kosovichev V. Fedun article Aims: We use wavefront sensing to characterise the image quality of the High Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager (SO/PHI) data products during the second remote sensing window of the Solar Orbiter (SO) nominal mission phase. Our ultimate aims are to reconstruct the HRT data by deconvolving with the HRT point spread function (PSF) and to correct for the effects of optical aberrations on the data. Methods: We use a pair of focused-defocused images to compute the wavefront error and derive the PSF of HRT by means of a phase diversity (PD) analysis. Results: The wavefront error of HRT depends on the orbital distance of SO to the Sun. At distances > 0.5 au, the wavefront error is small, and stems dominantly from the inherent optical properties of HRT. At distances < 0.5 au, the thermo-optical effect of the Heat Rejection Entrance Window (HREW) becomes noticeable. We develop an interpolation scheme for the wavefront error that depends on the thermal variation of the HREW with the distance of SO to the Sun. We also introduce a new level of image reconstruction, termed `aberration correction', which is designed to reduce the noise caused by image deconvolution while removing the aberrations caused by the HREW. Conclusions: The computed PSF via phase diversity significantly reduces the degradation caused by the HREW in the near-perihelion HRT data. In addition, the aberration correction increases the noise by a factor of only 1.45 compared to the factor of 3 increase that results from the usual PD reconstructions. 2023 July 10.1051/0004-6361/202346033 Astronomy & Astrophysics 675 https://ui.adsabs.harvard.edu/abs/2023A%26A...675A..61K F. Kahil A. Gandorfer J. Hirzberger D. Calchetti J. Sinjan G. Valori S. K. Solanki Stephanie L. Yardley K. Albert N. Albelo Jorge A. Álvarez-Herrero T. Appourchaux L. R. Bellot Rubio J. Blanco Rodríguez A. Feller B. Fiethe D. Germerott L. Gizon L. Guerrero P. Gutierrez-Marques M. Kolleck A. Korpi-Lagg H. Michalik A. Moreno Vacas D. Orozco Suárez I. Pérez Grande E. Sanchis Kilders J. Schou U. Schühle J. Staub H. Strecker R. Volkmer J. Woch article Kosak2022 2022 10.1093/mnras/stac647 Monthly Notices of the Royal Astronomical Society 512 5743-5754 https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5743K K. Kosak R. Kiefer A.-M. Broomhall inproceedings Fleck2022 2022 44th COSPAR Scientific Assembly. Held 16-24 July 44 2503 https://ui.adsabs.harvard.edu/abs/2022cosp...44.2503F B. Fleck M. Carlsson E. Khomenko M. Rempel F. Riva O. Steiner G. Vigeesh misc CaniveteCuissa2022 2022 10.5194/egusphere-egu22-5744 EGU General Assembly Conference Abstracts EGU22-5744 https://ui.adsabs.harvard.edu/abs/2022EGUGA..24.5744C J. R. Canivete Cuissa O. Steiner article Poutanen2022 2022 10.1126/science.abl4679 Science 375 874-876 https://ui.adsabs.harvard.edu/abs/2022Sci...375..874P J. Poutanen A. Veledina A. V. Berdyugin S. V. Berdyugina H. Jermak P. G. Jonker J. J. E. Kajava I. A. Kosenkov V. Kravtsov V. Piirola M. Shrestha M. A. Perez Torres S. S. Tsygankov article Mehta2022 2022 10.1093/mnras/stac1943 Monthly Notices of the Royal Astronomical Society 515 2415-2429 https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.2415M T. Mehta K. Jain S. C. Tripathy R. Kiefer D. Kolotkov A.-M. Broomhall inproceedings Zeuner2022 2022 10.1117/12.2629250 Ground-based and Airborne Instrumentation for Astronomy IX 12184 121840T https://ui.adsabs.harvard.edu/abs/2022SPIE12184E..0TZ F. Zeuner D. Gisler M. Bianda R. Ramelli S. V. Berdyugina article Strecker2022 2022 10.1051/0004-6361/202142564 Astronomy and Astrophysics 664 A195 https://ui.adsabs.harvard.edu/abs/2022A&A...664A.195S H. Strecker N. Bello González article Dominguez-Tagle2022 2022 10.1142/S2251171722500143 Journal of Astronomical Instrumentation 11 2250014 https://ui.adsabs.harvard.edu/abs/2022JAI....1150014D C. Dominguez-Tagle M. Collados R. Lopez J. J. V. Cedillo M. A. Esteves O. Grassin N. Vega A. Mato J. Quintero H. Rodriguez S. Regalado F. González misc Solanki2022 2022 10.5194/egusphere-egu22-4327 EGU General Assembly Conference Abstracts EGU22-4327 https://ui.adsabs.harvard.edu/abs/2022EGUGA..24.4327S S. K. Solanki J. Blanco F. Kahil P. Loeschl H. Strecker J. Hirzberger D. Orozco Suárez J. C. Del Toro Iniesta J. Woch A. Gandorfer A. Álvarez-Herrero T. Appourchaux R. Volkmer article Zeuner2022 2022 10.1051/0004-6361/202243350 Astronomy and Astrophysics 662 A46 https://ui.adsabs.harvard.edu/abs/2022A&A...662A..46Z F. Zeuner L. Belluzzi N. Guerreiro R. Ramelli M. Bianda article Bate2022 2022 10.3847/1538-4357/ac5c53 The Astrophysical Journal 930 129 https://ui.adsabs.harvard.edu/abs/2022ApJ...930..129B W. Bate D. B. Jess V. M. Nakariakov S. D. T. Grant S. Jafarzadeh M. Stangalini P. H. Keys D. J. Christian F. P. Keenan article Berdyugin2022 2022 10.1051/0004-6361/202142173 Astronomy and Astrophysics 657 A105 https://ui.adsabs.harvard.edu/abs/2022A&A...657A.105B A. V. Berdyugin V. Piirola S. Bagnulo J. D. Landstreet S. V. Berdyugina inproceedings Kahil2022 2022 10.1117/12.2628942 Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave 12180 121803F https://ui.adsabs.harvard.edu/abs/2022SPIE12180E..3FK F. Kahil A. Gandorfer J. Hirzberger D. Orozco Suárez K. Albert N. Albelo Jorge T. Appourchaux A. Álvarez-Herrero J. Blanco Rodríguez D. Germerott L. Guerrero P. Gutierrez Marquez J. Sinjan D. Calchetti M. Kolleck S. K. Solanki J. C. Toro Iniesta R. Volkmer J. Woch B. Fiethe J. M. Gómez Cama I. Pérez-Grande E. Sanchis Kilders M. Balaguer Jiménez L. R. Bellot Rubio M. Carmona W. Deutsch G. Fernandez-Rico A. Fernández-Medina P. García Parejo J. L. Gasent Blesa L. Gizon B. Grauf K. Heerlein A. Korpi-Lagg T. Lange A. López Jiménez T. Maue R. Meller H. Michalik A. Moreno Vacas R. Müller E. Nakai W. Schmidt J. Schou U. Schühle J. Staub H. Strecker I. Torralbo G. Valori article CaniveteCuissa2022 2022 10.1051/0004-6361/202243740 Astronomy and Astrophysics 668 A118 https://ui.adsabs.harvard.edu/abs/2022A&A...668A.118C J. R. Canivete Cuissa O. Steiner article Peter2022 2022 10.1007/s10686-021-09774-0 Experimental Astronomy 54 185-225 https://ui.adsabs.harvard.edu/abs/2022ExA....54..185P H. Peter E. A. Ballester V. Andretta F. Auchère L. Belluzzi A. Bemporad D. Berghmans E. Buchlin A. Calcines L. P. Chitta K. Dalmasse T. del P. Alemán A. Feller C. Froment R. Harrison M. Janvier S. Matthews S. Parenti D. Przybylski S. K. Solanki J. Štěpán L. Teriaca J. T. Bueno misc Rackham2022 2022 Bulletin of the American Astronomical Society 54 404.04 https://ui.adsabs.harvard.edu/abs/2022BAAS...54e4404R B. V. Rackham N. Espinoza S. V. Berdyugina H. Korhonen R. J. MacDonald B. T. Montet B. M. Morris M. Oshagh A. I. Shapiro Y. C. Unruh E. V. Quintana R. T. 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