Solar PhysicsPub Date : 2025-06-27DOI: 10.1007/s11207-025-02500-5
Momchil E. Molnar, Roberto Casini, Paul Bryans, Ben Berkey, Kalista Tyson
{"title":"Detection of “Diffuse” Coronal He I 1083 During the April 8, 2024 Solar Eclipse: Evidence for Terrestrial Atmospheric Scattering Contribution","authors":"Momchil E. Molnar, Roberto Casini, Paul Bryans, Ben Berkey, Kalista Tyson","doi":"10.1007/s11207-025-02500-5","DOIUrl":"10.1007/s11207-025-02500-5","url":null,"abstract":"<div><p>Strong He <span>i</span> 1083 nm atomic line signals have previously been measured during total solar eclipses at coronal heights above the lunar limb. These rather unexpected measurements have kindled a discussion about the suggested presence of significant amounts of neutral helium at coronal conditions. We performed spectroscopic observations of the He <span>i</span> 1083 nm wavelength region during the April 8th, 2024 total solar eclipse, using an instrument specifically designed to test the presence of He <span>i</span> 1083 in the solar corona. We were able to detect the He <span>i</span> 1083 line, the forbidden coronal line of Fe <span>xiii</span> at 1074.7 nm, as well as the chromospheric H <span>i</span> 1093.8 nm (Paschen-<span>(gamma )</span>) line in our data. The chromospheric He <span>i</span> 1083 nm and H <span>i</span> 1093.8 nm lines were detected in both the corona and on the lunar disc. We hypothesize that our observations support a terrestrial atmospheric scattering of the solar flash spectrum as the origin of the He <span>i</span> 1083 signal during the April 8th, 2024 eclipse. Our findings challenge the notion of abundant neutral helium in the solar corona suggested by previous eclipse observations.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 7","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145145494","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 : 2025-06-25DOI: 10.1007/s11207-025-02494-0
K. Sankarasubramanian, Monoj Bug, Abhilash Sarwade, Vaishali Sharan, Kumar, Ankur Kushwaha, Smrati Verma, M. C. Ramadevi, Kiran Lakshmipathaiah, Mukund Kumar Thakur, Kinshuk Gupta, Nidhi Sharma, Evangelin Leeja Justin, S. Narendra, Abhijit Adoni, Motamarri Srikanth, Vivek Subramanian, Shree Niwas Sahu, Vishnu Kishore Pai, Sajjade Faisal Mustafa, Nashiket Parate, Shamrao, Arjun Dey, Srikanth T, Priyanka Upadhyay, Rethika T, Gayathri Malhotra, S. V. Satyanarayana, Medasani Thejasree, Murugiah S, Naraya Rao G S, Bijaya Kumar Patra, Shalini Maiya, Lakshmi A, Ravi A, Kumar Shivam, Amit Purohit
{"title":"Solar Low Energy X-ray Spectrometer (SoLEXS) on Board Aditya-L1 Mission","authors":"K. Sankarasubramanian, Monoj Bug, Abhilash Sarwade, Vaishali Sharan, Kumar, Ankur Kushwaha, Smrati Verma, M. C. Ramadevi, Kiran Lakshmipathaiah, Mukund Kumar Thakur, Kinshuk Gupta, Nidhi Sharma, Evangelin Leeja Justin, S. Narendra, Abhijit Adoni, Motamarri Srikanth, Vivek Subramanian, Shree Niwas Sahu, Vishnu Kishore Pai, Sajjade Faisal Mustafa, Nashiket Parate, Shamrao, Arjun Dey, Srikanth T, Priyanka Upadhyay, Rethika T, Gayathri Malhotra, S. V. Satyanarayana, Medasani Thejasree, Murugiah S, Naraya Rao G S, Bijaya Kumar Patra, Shalini Maiya, Lakshmi A, Ravi A, Kumar Shivam, Amit Purohit","doi":"10.1007/s11207-025-02494-0","DOIUrl":"10.1007/s11207-025-02494-0","url":null,"abstract":"<div><p>The Solar Low-Energy X-ray Spectrometer (SoLEXS) is a moderate spectral resolution (≈ 170 eV at 5.9 keV) instrument with a soft X-ray energy coverage. SoLEXS is one of the experiments on board the Aditya-L1 mission to study the solar atmospheric dynamics along with other remote sensing and in situ payloads. Aditya-L1 was launched in September 2023 and acquired its final orbit at the Sun-Earth Lagrangian point L1 on January 06, 2024. SoLEXS experiment was powered on during December 2023 and is being operated continuously. SoLEXS has observed more than fifty X-class flares and several hundreds of M-class flares so far. This paper provides the details of the SoLEXS instrument along with its capabilities and potential science. This paper also briefly covers the science SoLEXS can provide in combination with other instruments on board Aditya-L1 making it a versatile instrument to study the solar flares and associated phenomena.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 7","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145144929","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 : 2025-06-19DOI: 10.1007/s11207-025-02493-1
P. T. Jain Jacob, Ram Ajor Maurya, Durgesh Tripathi
{"title":"Dynamics of Plasma and Magnetic Fields in a Quiescent Prominence Formation","authors":"P. T. Jain Jacob, Ram Ajor Maurya, Durgesh Tripathi","doi":"10.1007/s11207-025-02493-1","DOIUrl":"10.1007/s11207-025-02493-1","url":null,"abstract":"<div><p>We study the evolution and reorganization of magnetic field lines and associated plasma dynamics during the formation of a quiescent prominence. For this purpose, we have utilized the observations taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Our observations revealed an abrupt ascent of an EUV bright structure (or EUV jet) accompanied by a downflow during the early stage of the prominence formation. We closely tracked the rising motion and the associated downflow, estimating their average speeds around 2.8 km s<sup>−1</sup> and 10.1 km s<sup>−1</sup>, respectively, in conjunction with the brightening of a rising jet. We derived the temperature of the jet plasma by employing the Differential Emission Measure (DEM) on AIA observations and found it to be higher than expected temperature of prominence plasma (around <span>(log _{10}T approx 5.2)</span>). Moreover, we observed bi-directional plasma motions and brightening in jet plasma at the same time. These observations could be due to the reorganization of the magnetic field lines as part of magnetic reconnection within the prominence during early phase of its formation.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145144174","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 : 2025-06-19DOI: 10.1007/s11207-025-02496-y
M. S. Ruderman, N. S. Petrukhin, L. Y. Kataeva
{"title":"Nonlinear Propagating Slow Waves in Cooling Coronal Magnetic Loops","authors":"M. S. Ruderman, N. S. Petrukhin, L. Y. Kataeva","doi":"10.1007/s11207-025-02496-y","DOIUrl":"10.1007/s11207-025-02496-y","url":null,"abstract":"<div><p>We study the propagation of slow magnetosonic waves in coronal magnetic loops. In our study we take nonlinearity and loop cooling into account. We use the small beta approximation and neglect the effect of magnetic field perturbation on the wave propagation. In accordance with this we assume that the tube cross-section does not change. We also neglect the equilibrium plasma density variation along and across the tube. As a result the equations of magnetohydrodynamics reduce to purely one-dimensional gasdynamic equations that includes the effect of viscosity and thermal conduction. We assume that the perturbation amplitude is sufficiently small and use the reductive perturbation method to derive the generalised Burgers’ equation describing the evolution of initial perturbations. First we study a case with weak dissipation and drop the term describing it. When there is no cooling the evolution of the initial perturbation results in a gradient catastrophe. However strong cooling can prevent it. Then we solve the full equation numerically assuming that the temperature decreases exponentially. We fix the initial perturbation amplitude and then study the dependence of perturbation evolution on the cooling time. The main result that we obtain is that moderate cooling decelerates the wave damping. This effect is related to the fact that the dissipation coefficients are proportional to the temperature in <span>(5/2)</span> power. As a result they decrease fast because of plasma cooling. However strong cooling can cause perturbation damping on its own.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02496-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145144178","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 : 2025-06-16DOI: 10.1007/s11207-025-02495-z
Philip Gordon Judge
{"title":"Changing Methodologies in Solar Physics","authors":"Philip Gordon Judge","doi":"10.1007/s11207-025-02495-z","DOIUrl":"10.1007/s11207-025-02495-z","url":null,"abstract":"<div><p>This study attempts to establish a basis for understanding how methods used in research in solar physics have evolved since World War II (WWII). The goal is to begin to explore if and how the changing research environment affects the training of young scientists, and the future of solar physics research at our institutions. A strategy based upon a sample of 650 PhD theses is used to seek possible trends over 8 decades, with the aim of uncovering any correlations between methods used and measures of success. Necessarily subjective, results depend on how methods are defined, and how success is measured. Although a brief justification of the choices made is attempted, trying mainly to avoid pitfalls such as counting citations, it is clear that further assessment is required. The statistical analysis is based upon necessarily subjective categorization and the inference of likelihoods of two different distributions being drawn from the same underlying distribution. The statistics seem to reflect historical events, such as the Kennedy Moonshot program and the associated SKYLAB mission, with changes delayed by a few years. The data suggest that impactful advances are becoming more rare. Yet the methods used have changed little barring those related to obvious technological advances (e.g. the advent of spacecraft, adaptive optics). A follow-up study to explore the 100,000+ publications in solar physics through machine learning seems warranted.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02495-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143793","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 : 2025-06-13DOI: 10.1007/s11207-025-02502-3
Youcheng Chu, Xinyu Wang, Haoyuan Zhong, Qingjian Ni
{"title":"An Enhanced ResNet Model for Solar Activity Classification with Dual-Passband CHASE Data","authors":"Youcheng Chu, Xinyu Wang, Haoyuan Zhong, Qingjian Ni","doi":"10.1007/s11207-025-02502-3","DOIUrl":"10.1007/s11207-025-02502-3","url":null,"abstract":"<div><p>Fully automated detection of solar activity manifested in spectral images of the solar disk holds significant scientific value for advancing solar physics research. This study formulates the task as a classification problem using localized images of the solar disk. We first construct a solar activity classification dataset derived from CHASE full-disk spectral images. This dataset comprises both single-channel H<span>(alpha )</span> images and multi-channel images spanning the H<span>(alpha )</span> and Fe I passbands of the CHASE data. These multi-channel data represent a novel resource, as prior studies have not explored solar activity recognition using dual-passband multi-channel data. Subsequently, we develop a classification model leveraging Residual Networks (ResNets), and by optimizing the network architecture and incorporating attention mechanisms, the model effectively captures visual features of solar activity from multi-channel spectral images. Furthermore, we introduce a strategy of spectral channel normalization and downsampling to improve the model’s classification accuracy and training efficiency. Comparative and ablation experiments confirm that the proposed model delivers robust classification accuracy and efficient inference performance on this dataset.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143353","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 : 2025-06-11DOI: 10.1007/s11207-025-02501-4
Louis-Simon Guité, Paul Charbonneau, Antoine Strugarek
{"title":"Avalanching Together: A Model for Sympathetic Flaring","authors":"Louis-Simon Guité, Paul Charbonneau, Antoine Strugarek","doi":"10.1007/s11207-025-02501-4","DOIUrl":"10.1007/s11207-025-02501-4","url":null,"abstract":"<div><p>Avalanche models running in a self-organized critical regime have proven powerful in reproducing the power-law distributions and scale invariance that characterize the statistical properties of solar flares. They are often interpreted as representing an individual active region of the Sun. As a result, this class of models has rarely been applied to describe sympathetic flares—solar eruptions that occur in close spatial and temporal proximity, seemingly driven by their mutual interaction. In this study, we investigate the phenomenon of sympathetic flaring using avalanche models and compare their statistical properties with observations of sympathetic flares on the Sun. We developed a novel avalanche model featuring two connected lattices, each representing a distinct active region. This connectivity allows the transfer of nodal variable between the lattices, simulating the non-local effects expected to occur during sympathetic flares. Our results show that under strong connectivity, the lattices exhibit temporal synchronization, with correlations between their avalanche energies. Furthermore, increasing the connectivity between the lattices results in an excess of avalanches at short waiting times. A quantitative comparison with observational data suggests that only a weak connectivity allows our model to replicate the observed solar waiting time distributions. Consequently, we propose that if magnetic connectivity between distinct active regions drives sympathetic flaring on the Sun, it must remain relatively weak.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145142921","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 : 2025-06-06DOI: 10.1007/s11207-025-02478-0
Musheng Lin, Ya Wang, Liheng Yang, Jie Chen, Wenwei Pan, Shuyue Li, Qingmin Zhang
{"title":"Transverse Oscillations of Coronal Loops Induced by a Jet-Related Confined Flare on 11 July 2022","authors":"Musheng Lin, Ya Wang, Liheng Yang, Jie Chen, Wenwei Pan, Shuyue Li, Qingmin Zhang","doi":"10.1007/s11207-025-02478-0","DOIUrl":"10.1007/s11207-025-02478-0","url":null,"abstract":"<div><p>In this article, we report the multiwavelength and multiview observations of transverse oscillations of two loop strands induced by a jet-related, confined flare in active region NOAA 13056 on 11 July 2022. The jet originates close to the right footpoint of the loops and propagates in the northeast direction. The average rise time and fall time of the jet are ≈ 11 and ≈ 13.5 minutes, so that the lifetime of the jet reaches ≈ 24.5 minutes. The rising motion of the jet is divided into two phases with average velocities of ≈ 164 and ≈ 546 km s<sup>−1</sup>. The falling motion of the jet is coherent with an average velocity of ≈ 124 km s<sup>−1</sup>. The transverse oscillations of the loops, lasting for 3 – 5 cycles, are of fundamental standing kink mode. The maximal initial amplitudes of the two strands are ≈ 5.8 and ≈ 4.9 Mm. The average periods are ≈ 405 s and ≈ 407 s. Both of the strands experience slow expansions during oscillations. The lower limits of the kink speed are <span>(895_{-17}^{+21})</span> km s<sup>−1</sup> for loop_1 and <span>(891_{-35}^{+29})</span> km s<sup>−1</sup> for loop_2, respectively. The corresponding lower limits of the Alfvén speed are estimated to be <span>(664_{-13}^{+16})</span> km s<sup>−1</sup> and <span>(661_{-26}^{+22})</span> km s<sup>−1</sup>.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145142699","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 : 2025-06-06DOI: 10.1007/s11207-025-02490-4
F. H. van der Merwe, N. E. Engelbrecht
{"title":"Revisiting the Winding Angle of the Heliospheric Magnetic Field: Investigating the Influence of Turbulence","authors":"F. H. van der Merwe, N. E. Engelbrecht","doi":"10.1007/s11207-025-02490-4","DOIUrl":"10.1007/s11207-025-02490-4","url":null,"abstract":"<div><p>The nature, and geometry, of the heliospheric magnetic field (HMF) plays a significant role in the transport of energetic charged particles, whether these be of solar or galactic origin. The present study investigates the winding angle of the HMF by analysing almost 60 years of spacecraft data, by employing methods based on the assumption of a Parker HMF from prior studies, as well as a 3D definition of the winding angle. The 2D results reveal an overwound (relative to the expected Parker field result) winding angle with a clear solar cycle dependence, in agreement with previous studies. The 3D results, however, indicate a consistently underwound field. It is further demonstrated that this winding can potentially be explained by the meandering of HMF lines due to the presence of turbulence. Furthermore, consequences of this phenomenon for energetic particle transport, particularly for magnetic focusing, are discussed.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-025-02490-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145142305","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":"On the Magnetic Reconnection and Its Properties During a Flare Using a Magnetohydrodynamics Simulation","authors":"Sushree S. Nayak, Qiang Hu, Wen He, Sanjay Kumar, Ramit Bhattacharyya","doi":"10.1007/s11207-025-02492-2","DOIUrl":"10.1007/s11207-025-02492-2","url":null,"abstract":"<div><p>We study the magnetic reconnection during a flare by investigating flare ribbon dynamics using observations and data-constrained magnetohydrodynamics (MHD) simulation. In particular, we estimate the reconnection flux and the reconnection flux rates using flare ribbons of an M1.1 flare hosted by the active region 12184 utilizing the technique developed by Qiu et al. (2002). The reconnection flux and corresponding flux rates are found to be <span>(10^{20})</span> Mx and <span>(10^{18})</span> Mx s<sup>−1</sup> respectively. To understand the flare onset and the origin of flare ribbons, we perform an MHD simulation initiated by the non-force-free-field extrapolation. Importantly, the extrapolated configuration identifies a three-dimensional (3D) magnetic neutral point and a flux rope in the flaring region, which is crucial to the flaring activity. The reconnection initiates at the null point and, subsequently the flux rope rises and appears to reconnect there, which is favorable for the eruption of the filament. The surrounding field lines also seem to take part in the null point reconnection. In later stage, a current sheet is formed below the null point ensuing a secondary reconnection near an X-type topology, further contributing to the energy release process in the flare. We trace the footpoint evolution of the field lines lying over the flare ribbons and find a significant similarity between the observed flare ribbons and the evolution of footpoints computed from the MHD simulation. We estimated induced electric field during the flare and found it to be ≈ 0.52 V cm<sup>−1</sup>, a slight less value, as per many past literatures. Additional findings are the enhancement of vertical current density near the flaring ribbons, a signature of successive reconnections near the null point. Overall, the present work contributes to the understanding of the ribbon formation in a flaring process and the involved magnetic reconnection.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"300 6","pages":""},"PeriodicalIF":2.4,"publicationDate":"2025-06-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145142617","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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