Solar PhysicsPub Date : 2025-05-15DOI: 10.1007/s11207-025-02476-2
Luke Majury, Ryan Milligan, Elizabeth Butler, Harry Greatorex, Maria Kazachenko
{"title":"Spectral Irradiance Variability in Lyman-Alpha Emission During Solar Flares","authors":"Luke Majury, Ryan Milligan, Elizabeth Butler, Harry Greatorex, Maria Kazachenko","doi":"10.1007/s11207-025-02476-2","DOIUrl":"10.1007/s11207-025-02476-2","url":null,"abstract":"<div><p>The Lyman-alpha (Ly<span>(alpha )</span>; 1216 Å) line is the brightest emission line in the quiescent solar spectrum and radiates a significant fraction of the available nonthermal energy during flares. Despite its importance, there is a lack of detailed studies of Ly<span>(alpha )</span> spectral variability during flares. Recently, spectrally resolved Ly<span>(alpha )</span> flare observations from the SORCE/SOLSTICE instrument have become available. This study examines Ly<span>(alpha )</span> spectral variability and its relationship with HXR emission from nonthermal electrons, using observations of two M-class flares from SORCE/SOLSTICE and RHESSI. Imaging observations from STEREO/SECCHI EUVI and SDO/AIA provide further context. Enhancements across the Ly<span>(alpha )</span> line profile were found to closely correlate with bursts of HXR emission, suggesting a primarily nonthermal origin. Red enhancement asymmetries at the peak of each flare were attributed to chromospheric evaporation, while blue wing enhancement and blue asymmetry were linked to a bright filament-eruption seen in SDO/AIA 1600 Å images. These findings contribute to the understanding of spectral Ly<span>(alpha )</span> variability during flares and highlight the need for future studies using a higher quality and quantity of spectral Ly<span>(alpha )</span> flare observations. Such studies will further characterise the physical mechanisms driving Ly<span>(alpha )</span> flare variability.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02476-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143949633","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-05-09DOI: 10.1007/s11207-025-02472-6
Robert Kamlah, Meetu Verma, Carsten Denker, Ioannis Kontogiannis, Alexander G. M. Pietrow, Jürgen Rendtel, Emily Lößnitz, Arooj Faryad, Reiner Volkmer, Rolf Schlichenmaier, Thomas Berkefeld, Miguel Esteves, Olivier Grassin, Markus Roth
{"title":"Wide-Field Image Restoration of G-Band and Ca ii K Images Containing Large and Complex Active Regions","authors":"Robert Kamlah, Meetu Verma, Carsten Denker, Ioannis Kontogiannis, Alexander G. M. Pietrow, Jürgen Rendtel, Emily Lößnitz, Arooj Faryad, Reiner Volkmer, Rolf Schlichenmaier, Thomas Berkefeld, Miguel Esteves, Olivier Grassin, Markus Roth","doi":"10.1007/s11207-025-02472-6","DOIUrl":"10.1007/s11207-025-02472-6","url":null,"abstract":"<div><p>Restoration of solar images to achieve near diffraction-limited spatial resolution is commonly implemented on large-aperture solar telescopes. However, the extent of the restored field-of-view is typically only 100<sup>′′</sup> or even smaller. This study reports on wide-field image restoration of G-band and Ca <span>ii</span> K images obtained with the 0.7-meter Vacuum Tower Telescope (VTT) at Observatorio del Teide, Tenerife, Spain. The Kiepenheuer Adaptive Optics System (KAOS) at the VTT provides a field-of-view with a diameter of 270<sup>′′</sup>. Time series of datasets with 100 images were acquired with a large-format (7920 × 6004 pixels) CMOS imager at a frame rate of 30 Hz. An experimental optical setup that enabled wide-field imaging is briefly presented. Results from speckle-masking imaging and Multi-Frame Blind Deconvolution (MFBD) demonstrate the unique potential of the VTT for wide-field imaging. Power spectral analysis quantifies the instrument performance as a function of time and with distance from the lock point of the AO system. Further science capabilities are established using Local Correlation Tracking (LCT), Background-subtracted Solar Activity Maps (BaSAMs), and image quality/seeing metrics. In summary, commercial off-the-shelf camera systems can become an asset to sub-meter-class solar telescopes and open up new science opportunities at the interface between large-aperture and synoptic solar telescopes.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143929890","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-05-07DOI: 10.1007/s11207-025-02468-2
Janmejoy Sarkar, V. N. Nived, Soumya Roy, Rushikesh Deogaonkar, Sreejith Padinhatteeri, A. Raja Bayanna, Ravi Kesharwani, A. N. Ramaprakash, Durgesh Tripathi, Rahul Gopalakrishnan, Bhushan Joshi, Sakya Sinha, Mahesh Burse, Manoj Varma, Anurag Tyagi, Reena Yadav, Chaitanya Rajarshi, H. N. Adithya, Abhijit Adoni, Gazi A. Ahmed, Dipankar Banerjee, Rani Bhandare, Bhargava Ram B.S., Kalpesh Chillal, Pravin Chordia, Avyarthana Ghosh, Girish Gouda, Anand Jain, Melvin James, Evangeline Leeja Justin, Deepak Kathait, Aafaque Khan, Pravin Khodade, Abhay Kohok, Akshay Kulkarni, Ghanshyam Kumar, Nidhi Mehandiratta, Vilas Mestry, Deepa Modi, Srikanth Motamarri, K. Nagaraju, Dibyendu Nandy, S. Narendra, Sonal Navle, Nashiket Parate, Sujit Punnadi, A. Ravi, K. Sankarasubramanian, Ghulam Sarvar, Nigar Shaji, Sami K. Solanki, Rethika T, Koushal Vadodariya, D. R. Veeresha, R. Venkateswaran
{"title":"Test and Calibration of the Solar Ultraviolet Imaging Telescope (SUIT) on Board Aditya-L1","authors":"Janmejoy Sarkar, V. N. Nived, Soumya Roy, Rushikesh Deogaonkar, Sreejith Padinhatteeri, A. Raja Bayanna, Ravi Kesharwani, A. N. Ramaprakash, Durgesh Tripathi, Rahul Gopalakrishnan, Bhushan Joshi, Sakya Sinha, Mahesh Burse, Manoj Varma, Anurag Tyagi, Reena Yadav, Chaitanya Rajarshi, H. N. Adithya, Abhijit Adoni, Gazi A. Ahmed, Dipankar Banerjee, Rani Bhandare, Bhargava Ram B.S., Kalpesh Chillal, Pravin Chordia, Avyarthana Ghosh, Girish Gouda, Anand Jain, Melvin James, Evangeline Leeja Justin, Deepak Kathait, Aafaque Khan, Pravin Khodade, Abhay Kohok, Akshay Kulkarni, Ghanshyam Kumar, Nidhi Mehandiratta, Vilas Mestry, Deepa Modi, Srikanth Motamarri, K. Nagaraju, Dibyendu Nandy, S. Narendra, Sonal Navle, Nashiket Parate, Sujit Punnadi, A. Ravi, K. Sankarasubramanian, Ghulam Sarvar, Nigar Shaji, Sami K. Solanki, Rethika T, Koushal Vadodariya, D. R. Veeresha, R. Venkateswaran","doi":"10.1007/s11207-025-02468-2","DOIUrl":"10.1007/s11207-025-02468-2","url":null,"abstract":"<div><p>The Solar Ultraviolet Imaging Telescope (SUIT) on board the Aditya-L1 mission observes the Sun in the 200 – 400 nm wavelength range. This paper presents the results of various on-ground and on-board tests and their comparison with the specifications. Moreover, we also present the scheme for data calibration. We demonstrate that the test results are compliant with the specified numbers, except the spatial resolution. Such discrepancy will limit the photometric measurements only, at a scale of 2.2<sup>′′</sup> instead of 1.4<sup>′′</sup> as originally envisioned. The results obtained here show that SUIT observations open a new window for solar observations.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143919035","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-04-25DOI: 10.1007/s11207-025-02465-5
Zhentong Li, Yang Su, Wei Liu, Wei Chen, Fu Yu, Weiqun Gan
{"title":"Spectral Cross-Calibrations of ASO-S/HXI with Other X-ray Missions","authors":"Zhentong Li, Yang Su, Wei Liu, Wei Chen, Fu Yu, Weiqun Gan","doi":"10.1007/s11207-025-02465-5","DOIUrl":"10.1007/s11207-025-02465-5","url":null,"abstract":"<div><p>Cross-calibration of X-ray instruments is crucial for stereoscopic studies of solar hard X-ray directivity and three-dimensional morphology, where spectral and imaging differences observed from multiple perspectives provide critical constraints. We present the preliminary results of the spectral calibrations of ASO-S/HXI through internal consistency checks of its three total flux detectors and cross-calibrations with Solar Orbiter/STIX, Fermi/GBM, and Konus-Wind data. Both calibration tests suggest that the response matrix of one of the HXI total flux monitors, D94 (with a thin aluminum window), needs to be modified. The new response matrix is determined by testing the series of response matrices with changing effective aluminum thickness through simulations. Post-correction analysis reveals <span>(sim 88%)</span> of co-observed events demonstrate electron spectral index consistency within <span>(pm 0.5)</span>, while comparisons of the total counts above 30 keV show < 10% differences for STIX-HXI flares with separation angles < 20° and Fermi-observed moderate flares. Though challenges persist regarding detector response uncertainties, the pile-up effect, and other nonideal factors, the achieved inter-instrument consistency enables quantitative electron anisotropy investigations through joint spectral analysis.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02465-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143875473","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-04-25DOI: 10.1007/s11207-025-02466-4
Mohammed H. Talafha, Kristóf Petrovay, Andrea Opitz
{"title":"Effect of Nonlinear Surface Inflows into Activity Belts on Solar Cycle Modulation","authors":"Mohammed H. Talafha, Kristóf Petrovay, Andrea Opitz","doi":"10.1007/s11207-025-02466-4","DOIUrl":"10.1007/s11207-025-02466-4","url":null,"abstract":"<div><p>Converging flows are visible around bipolar magnetic regions (BMRs) on the solar surface, according to observations. Average flows are created by these inflows combined, and the strength of these flows depends on the amount of flux present during the solar cycle. In models of the solar cycle, this average flow can be depicted as perturbations to the meridional flow. In this article, we study the effects of introducing surface inflow to the surface flux transport models (SFT) as a possible nonlinear mechanism in the presence of latitude quenching for an inflow profile whose amplitude varies within a cycle depending on the magnetic activity. Using a grid based on one-dimensional SFT models, we methodically investigate the extent of the nonlinearity caused by inflows, latitude quenching (LQ), and their combinations. The results show that including surface inflows in the model in the presence of both LQ and tilt quenching (TQ) produced a polar field within a <span>(pm 1sigma )</span> of an average cycle polar field (<span>(sigma )</span> is the standard deviation) with a correlation coefficient of 0.85. We confirm that including inflows produces a lower net contribution to the dipole moment (10 – 25%). Furthermore, the relative importance of LQ vs. inflows is inversely correlated with the dynamo effectivity range (<span>(lambda _{R})</span>). With no decay term, introducing inflows into the model results in a less significant net contribution to the dipole moment. Including inflows in the SFT model shows a possible nonlinear relationship between the surface inflows and the solar dipole moment, suggesting a potential nonlinear mechanism contributing to the saturation of the global dynamo. For lower <span>(lambda _{R})</span> (<span>(lessapprox 10^{circ })</span>), TQ always dominates LQ, and for higher <span>(lambda _{R})</span>, LQ dominates. However, including inflows makes the domination earlier in case of having a decay term in the model.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02466-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143875262","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Analysis of the Vertical Current Evolution for the X9.3 Flare on 6 September 2017","authors":"Haili Li, Xiaofeng Deng, Hongfei Liang, Xinping Zhou, Yu Liu, Zhongquan Qu","doi":"10.1007/s11207-025-02467-3","DOIUrl":"10.1007/s11207-025-02467-3","url":null,"abstract":"<div><p>In this article, we examine the morphological evolution and current distribution of the X9.3-class flare on 6 September 2017 that occurred in the active region (AR) 12673. We combine the high-resolution observations of the Atmospheric Imaging Assembly (AIA) and Helioseismic Magnetic Imager (HMI) instruments on board the Solar Dynamics Observatory. The vertical current intensity and the soft X-ray flux within the active region showed two peaks, corresponding, respectively, to the X2.2 and X9.3 flares on that day, while the latter constituted a more significant increase. A pair of conjugate current ribbons appeared at the same locations consistent with the two ribbons of the flare. These current ribbons underwent sustained and significant changes during the X9.3 flare eruption. In the early period of the flare, there was a substantial decrease in the area of the current ribbons, resulting in the emergence of a series of high-density small current islands. During the later phase, not only did the area of the currents rapidly increase, but also the flare kernels evolved into two flare bands along the sheared magnetic neutral line in the photosphere. The AIA 1600 Å and 304 Å images revealed that the two ribbons of the X9.3 flare formed from small bright kernels. It was also observed that the positions of the flare kernels closely matched those of the current islands. Based on the vertical current distribution and evolution near the highly sheared core field region during the X9.3 flare, we conclude that this flare eruption should be attributed to tether-cutting magnetic reconnection.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143871417","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-04-08DOI: 10.1007/s11207-025-02459-3
Mohammed Akram Zermane, Nadia Oulebsir, Mohamed Reda Bekli, Zahir Belhadi, Katia Becheker, Abdeldjalil Zaidi, Abdelghani Hadj Hammou
{"title":"Magnitude Prediction of Solar Cycle 26 Using a New Precursor Approach","authors":"Mohammed Akram Zermane, Nadia Oulebsir, Mohamed Reda Bekli, Zahir Belhadi, Katia Becheker, Abdeldjalil Zaidi, Abdelghani Hadj Hammou","doi":"10.1007/s11207-025-02459-3","DOIUrl":"10.1007/s11207-025-02459-3","url":null,"abstract":"<div><p>A long-term prediction approach for solar cycles is proposed by including the century-scale modulation in the SODA (Solar Dynamo Amplitude) and XSODA (Extended Solar Dynamo Amplitude) indices of Schatten and Pesnell, MSODA and MXSODA. Additionally, we also introduce a new technique, the minimal fluctuation method, to reduce temporal fluctuations. By combining this method with MSODA, we predict that Solar Cycle 26 will reach a maximum sunspot number of <span>(109.14pm 32.92)</span> in the year <span>(2035.3 pm 2.3)</span>. Using MXSODA, the most reliable indicator, the peak is expected to reach a maximum amplitude of <span>(160.70pm 47.83)</span> on the same date.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793173","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-04-07DOI: 10.1007/s11207-025-02456-6
S. Liu, Shahid Idrees, D. Liu, S. G. Zeng
{"title":"The Properties of Non-Potential Magnetic Field Parameters in a Super-Active Region with Complex Structures and Strong Solar Flares","authors":"S. Liu, Shahid Idrees, D. Liu, S. G. Zeng","doi":"10.1007/s11207-025-02456-6","DOIUrl":"10.1007/s11207-025-02456-6","url":null,"abstract":"<div><p>Solar active regions (ARs), characterized by intense magnetic fields, are prime locations for solar flares. Understanding the properties of these magnetic fields is crucial for predicting and mitigating space weather events. In this study, the non-potential magnetic field parameters of active region (AR) NOAA 9077 are investigated; this AR experienced a super-strong X5.7 solar flare. Using advanced extrapolation techniques, the 3D magnetic field structure from vector magnetograms is obtained using the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station (HSOS). Then, various non-potential parameters are calculated, including current density, shear angle, quasi-separatrix layers (QSLs), twist, and field line helicity. By analyzing the spatial and temporal distributions of these parameters, we aim to shed light on the relationship between magnetic field properties and solar flare occurrence. Our findings reveal that high twist and complex magnetic field configurations are prevalent before flares, while these features tend to weaken after the eruption. Additionally, we observe decreases in helicity and free energy after the flare, while the free energy peaks approximately 1.5 days prior to the onset of the flare. Furthermore, we investigate the distribution of quasi-separatrix layers and twist, finding high degrees of complexity before flares. Multiple patterns of high current density regions suggest unstable magnetic structures prone to flaring, coinciding with the shear angle distribution. Relative field line helicity patterns exhibit distinct characteristics compared to current density, concentrating before flares and diverging afterward. Overall, our results highlight the contrasting nature of current density and relative field line helicity patterns in relation to solar flares, in addition to the aforementioned features in the set of commonly derived non-potential parameters for this particular event.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143793101","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Solar PhysicsPub Date : 2025-04-04DOI: 10.1007/s11207-025-02455-7
Jie Chen, Jiangtao Su, Wenbin Xie, Yuanyong Deng, Xianyong Bai, Ziyao Hu, Haiqing Xu, Suo Liu, Yin Zhang, Yingzi Sun, Yongliang Song, Xiaofan Wang
{"title":"Direct Measurement of the Longitudinal Magnetic Field in the Solar Photosphere with the Zeeman Effect","authors":"Jie Chen, Jiangtao Su, Wenbin Xie, Yuanyong Deng, Xianyong Bai, Ziyao Hu, Haiqing Xu, Suo Liu, Yin Zhang, Yingzi Sun, Yongliang Song, Xiaofan Wang","doi":"10.1007/s11207-025-02455-7","DOIUrl":"10.1007/s11207-025-02455-7","url":null,"abstract":"<div><p>The primary objective of our research is to validate direct measurements of the solar magnetic field through calculating the splitting of polarized spectral lines. The data are collected by the Solar Magnetism and Activity Telescope (SMAT) located at the Huairou Solar Observing Station (HSOS). The number of sampling points of the spectral line profile was varied from 5 to 31. By fitting the profiles of left- and right-circularly polarized light intensities, we determined the spectral line splitting, and the error between the magnetic-field strength determined from this and the true value was less than 2%. We found that the correlation between the magnetic-field strength measured in the active regions by SMAT and that observed by Helioseismic and Magmetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) reached about 80%, but in the quiet region, this correlation was very low.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 4","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143778065","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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