Solar Physics最新文献

{"title":"Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H(alpha ) Solar Explorer (CHASE)","authors":"Qiao Li,&nbsp;Ying Li,&nbsp;Yang Su,&nbsp;Dechao Song,&nbsp;Hui Li,&nbsp;Li Feng,&nbsp;Yu Huang,&nbsp;Youping Li,&nbsp;Jingwei Li,&nbsp;Jie Zhao,&nbsp;Lei Lu,&nbsp;Beili Ying,&nbsp;Jianchao Xue,&nbsp;Ping Zhang,&nbsp;Jun Tian,&nbsp;Xiaofeng Liu,&nbsp;Gen Li,&nbsp;Zhichen Jing,&nbsp;Shuting Li,&nbsp;Guanglu Shi,&nbsp;Zhengyuan Tian,&nbsp;Wei Chen,&nbsp;Yingna Su,&nbsp;Qingmin Zhang,&nbsp;Dong Li,&nbsp;Yunyi Ge,&nbsp;Jiahui Shan,&nbsp;Yue Zhou,&nbsp;Shijun Lei,&nbsp;Weiqun Gan","doi":"10.1007/s11207-024-02313-y","DOIUrl":"10.1007/s11207-024-02313-y","url":null,"abstract":"<div><p>Solar white-light flares are characterized by an enhancement in the optical continuum, which are usually large flares (X- and M-class flares). Here, we report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the <i>Advanced Space-based Solar Observatory</i> and the <i>Chinese H</i><span>(alpha )</span> <i>Solar Explorer</i> (CHASE). This flare exhibits an increase of ≈ 6.4% in the photospheric Fe <span>i</span> line at 6569.2 Å and ≈ 3.2% in the nearby continuum. The continuum at 3600 Å also shows an enhancement of ≈ 4.7%. The white-light bright kernels are mainly located at the flare ribbons and co-spatial with nonthermal hard X-ray sources, which implies that the enhanced white-light emissions are related to nonthermal electron-beam heating. At the bright kernels, the Fe <span>i</span> line displays an absorption profile that has a good Gaussian shape, with a redshift up to ≈ 1.7 km s⁻¹, while the H<span>(alpha )</span> line shows an emission profile having a central reversal. The H<span>(alpha )</span> line profile also shows a red or blue asymmetry caused by plasma flows with a velocity of several to tens of km s⁻¹. It is interesting to find that the H<span>(alpha )</span> asymmetry is opposite at the conjugate footpoints. It is also found that the CHASE continuum increase seems to be related to the change in the photospheric magnetic field. Our study provides comprehensive characteristics of a small white-light flare that help understand the energy release process of white-light flares.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02313-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141192374","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":"Properties of Type-II Radio Bursts in Relation to Magnetic Complexity of the Solar Active Regions","authors":"Tusharkumar N. Bhatt,&nbsp;Rajmal Jain,&nbsp;N. Gopalswamy,&nbsp;Anjali Dwivedi,&nbsp;Anshupriya Singh,&nbsp;Arun Kumar Awasthi,&nbsp;Seiji Yashiro,&nbsp;Walter R. Guevara Day,&nbsp;Pramod K. Chamadia,&nbsp;Krunal Patel,&nbsp;Sneha Chaudhari","doi":"10.1007/s11207-024-02318-7","DOIUrl":"10.1007/s11207-024-02318-7","url":null,"abstract":"<div><p>Type-II radio bursts are believed to occur as a result of the shock driven by flares or coronal mass ejections (CMEs). While the shock waves are important for the acceleration of electrons necessary for the generation of the radio emission, the exact nature of the shock and coronal conditions necessary to produce type-II radio emission is still under debate. In this investigation, we probe the relationship of kinematic characteristics of the type-II radio bursts with the magnetic-field complexity (<i>M</i>_<i>j</i>) of the active regions visible on the photosphere. Our investigation of 64 type-II solar radio bursts, which are associated with flares and CMEs, reveals that <i>M</i>_<i>j</i> is linearly correlated in the logarithmic scale with the starting frequency (<i>f</i>_s) and drift-rate (<span>({Delta f/Delta t})</span>) of type-II radio burst. Further, <i>M</i>_<i>j</i> exhibits a linear correlation with the shock height (<i>r</i>) and electron density (<span>(n_{rm e})</span>) in logarithmic scale. This indicates that high frequency (<i>f</i>_s <span>(geq 100)</span> <span>({rm MH_{z}})</span>) bursts, which occur at the reconnection site near the solar surface, are produced from a strong magnetically complex region. Further, strong and complex magnetic-field regions produce shocks of higher speeds. Based on the derived plasma parameters of the radio bursts and their relationship with <i>f</i>_s as well as with <i>M</i>_<i>j</i>, we propose that the high-frequency type-II bursts were generated in a special situation when the shock is produced due to magnetic reconnection occurring in the low-lying coronal loops. We conclude that type-II radio bursts can occur even in the inner corona as well as in the outer corona; however, it depends on the magnetic complexity of the active region in which the event occurs.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02318-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141192388","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":"Automatic Solar Flare Detection Using the Solar Disk Imager Onboard the ASO-S Mission","authors":"Lei Lu,&nbsp;Zhengyuan Tian,&nbsp;Li Feng,&nbsp;Jiahui Shan,&nbsp;Hui Li,&nbsp;Yang Su,&nbsp;Ying Li,&nbsp;Yu Huang,&nbsp;Youping Li,&nbsp;Jingwei Li,&nbsp;Jie Zhao,&nbsp;Beili Ying,&nbsp;Jianchao Xue,&nbsp;Ping Zhang,&nbsp;Dechao Song,&nbsp;Shuting Li,&nbsp;Guanglu Shi,&nbsp;Yingna Su,&nbsp;Qingmin Zhang,&nbsp;Yunyi Ge,&nbsp;Bo Chen,&nbsp;Qiao Li,&nbsp;Gen Li,&nbsp;Yue Zhou,&nbsp;Jun Tian,&nbsp;Xiaofeng Liu,&nbsp;Zhichen Jing,&nbsp;Weiqun Gan,&nbsp;Kefei Song,&nbsp;Lingping He,&nbsp;Shijun Lei","doi":"10.1007/s11207-024-02310-1","DOIUrl":"10.1007/s11207-024-02310-1","url":null,"abstract":"<div><p>We present an automated solar flare detection software tool to automatically process solar observed images, detect and track solar flares, and finally compile an event catalog. It can identify and track flares that happen simultaneously or temporally close together. The method to identify a flare is based on the local intensity changes in macropixels. The basic characteristics, such as the time and location information of a flare, are determined with a triple-threshold scheme, with the first threshold (global threshold) to determine the occurrence (location) of the flare and the second and third thresholds (local thresholds) to determine the real start and end times of the flare. We have applied this tool to one month of continuous solar ultraviolet (UV) images obtained by the <i>Solar Disk Imager</i> (SDI) onboard the <i>Advanced Space-based Solar Observatory</i> (ASO-S), which show active phenomena such as flares, filaments or prominences, and solar jets. Our automated tool efficiently detected a total number of 226 solar events. After a visual inspection, we found that only one event was misidentified (unrelated to an active event). We compared the detected events with the GOES X-ray flare list and found that our tool can detect 81% of GOES M-class and above flares (29 out of 36), from which we conclude that the intensity increase in SDI UV images can be considered as a good indicator of a solar flare.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02310-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141167461","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":"Seismology of Curved Coronal Loops Using Multiperiodic Kink Oscillations","authors":"Igor Lopin","doi":"10.1007/s11207-024-02305-y","DOIUrl":"10.1007/s11207-024-02305-y","url":null,"abstract":"<div><p>It was shown recently that the model of a semicircular magnetic slab with oblique wave propagation and finite plasma-<span>(beta )</span> supports two fast surface modes, one of which produces vertical and the other horizontal kink-like motions. Their phase speeds (frequencies) depend upon the internal plasma-<span>(beta )</span> and slab aspect ratio. Thus the theory predicts the coexistence of two kink modes with different polarizations and periods in a single oscillating loop. In the present work, we aim to perform some analytical extensions of the developed theory and propose methods for seismological estimation of internal plasma-<span>(beta )</span> and internal Alfvén speed on the bases of multiperiodic kink oscillations of coronal loops. We show that when two fundamental modes of vertically and horizontally polarized kink oscillations with different periods are observed in a single coronal loop, this provides the seismological estimation of the internal plasma-<span>(beta )</span> and Alfvén speed. We also show that the combined effect of a finite plasma-<span>(beta )</span> and a slab curvature modifies the ratio of periods <span>(P_{1}/2P_{2})</span> of the fundamental mode and first overtone of a certain kink oscillation and the internal plasma-<span>(beta )</span> can be estimated using detected <span>(P_{1}/2P_{2})</span>. We also suggest that the strands with different temperatures that constitute the multithermal loops should oscillate with different periods and this may provide an estimate to the internal Alfvén speed in such loops. These findings are applied to a number of observations of multiperiodic coronal loop kink oscillations. Furthermore, a number of unusual observational results and the results of numerical simulations of kink oscillations in curved magnetic loops were interpreted on the bases of the developed theory.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141136374","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}

{"title":"Machine Learning for Reconstruction of Polarity Inversion Lines from Solar Filaments","authors":"Vaclovas Kisielius,&nbsp;Egor Illarionov","doi":"10.1007/s11207-024-02324-9","DOIUrl":"10.1007/s11207-024-02324-9","url":null,"abstract":"<div><p>Solar filaments are well-known tracers of polarity inversion lines that separate two opposite magnetic polarities on the solar photosphere. Because observations of filaments began long before the systematic observations of solar magnetic fields, historical filament catalogs can facilitate the reconstruction of magnetic polarity maps at times when direct magnetic observations were not yet available. In practice, this reconstruction is often ambiguous and typically performed manually. We propose an automatic approach based on a machine-learning model that generates a variety of magnetic polarity maps consistent with filament observations. To evaluate the model and discuss the results, we use the catalog of solar filaments and polarity maps compiled by McIntosh. We realize that the process of manual compilation of polarity maps includes not only information on filaments, but also a large amount of prior information, which is difficult to formalize. To compensate for the lack of prior knowledge for the machine-learning model, we provide it with polarity information at several reference points. We demonstrate that this process, which can be considered as the user-guided reconstruction or superresolution, leads to polarity maps that are reasonably close to hand-drawn ones and additionally allows for uncertainty estimation.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141131314","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}

{"title":"A Study on Magnetic-Sensitivity Wavelength Position of the Working Line Used by the Full-Disk Magnetograph Onboard the Advanced Space Based Solar Observatory (ASO-S/FMG)","authors":"S. Liu,&nbsp;J. T. Su,&nbsp;X. Y. Bai,&nbsp;Y. Y. Deng,&nbsp;J. Chen,&nbsp;Y. L. Song,&nbsp;X. F. Wang,&nbsp;H. Q. Xu,&nbsp;X. Yang,&nbsp;Shahid Idrees","doi":"10.1007/s11207-024-02311-0","DOIUrl":"10.1007/s11207-024-02311-0","url":null,"abstract":"<div><p>Utilizing data from the <i>Solar Magnetism and</i> <i>Activity Telescope</i> (SMAT), analytical solutions of polarized radiative transfer equations, and in-orbit test data for the <i>Full-disk Magnetograph</i> (FMG) onboard the <i>Advanced Space based Solar Observatory</i> (ASO-S), this study reveals the magnetic-sensitivity spectral positions for the Fe <span>i</span> <span>(lambda )</span> 5234.19 Å working line used by FMG. From the experimental data of SMAT, it is found that the most sensitive position is located at the line center for linear polarization (Stokes Q/U), while it is about −0.07 Å away from the line center for circular polarization (Stokes V). Moreover, both the theoretical analysis and the in-orbit test data analysis of FMG confirm the above results. Additionally, the theoretical analysis suggests the presence of distinct spectral pockets (centered at 0.08 – 0.15 Å) from the line, harboring intense magnetic sensitivity across all three Stokes parameters. Striking a balance between high sensitivity for both linear and circular polarization, while capturing additional valuable information, a spectral position of −0.08 Å emerges as the champion for routine FMG magnetic field observations.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141140653","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}

{"title":"A Diffraction Effect Investigation for the Solar Irradiance Absolute Radiometer on the Fengyun-3F Satellite","authors":"Hang Dong,&nbsp;Xiaolong Yi,&nbsp;Peng Zhang,&nbsp;Dongjun Yang,&nbsp;Yuchen Lin,&nbsp;Jin Qi,&nbsp;Wei Fang,&nbsp;Ruidong Jia,&nbsp;Jun Zhou,&nbsp;Xin Ye","doi":"10.1007/s11207-024-02309-8","DOIUrl":"10.1007/s11207-024-02309-8","url":null,"abstract":"<div><p>The measurements of the Total Solar Irradiance (TSI) is a primary means to investigate solar activity and key measurement for understanding global climate change. The aperture diffraction is an error factor for the Solar Irradiance Absolute Radiometer (SIAR) on the Fengyun-3F (FY-3F) satellite. The diffraction effect correction factors can currently only be obtained by simulation, and they are obtained based on a series of approximate conditions that do not allow the accuracy of the diffraction correction results to be assessed. In this paper, we establish the diffraction effect measurement equipment based on the dark imaging technology and the theory of diffraction by Fraunhofer. The total light image and the aperture diffraction images of different angles were obtained by the CCD camera. The images were corrected by linearity, background, and continuity. Then, the diffraction effect curve of diffraction angle can be obtained. Finally, the diffraction correction factor of SIAR/FY-3F can be obtained by the accumulation of multiple apertures and combining the weighted integration of the solar spectrum. The results illustrated that the value of the diffraction correction factor of the SIAR aperture system on the FY-3F satellite is <span>(2.85times 10^{-3})</span>, and the uncertainty of diffraction effect experimental measurement is 4.62%, which reduces the measurement error of the diffraction effect on the total solar irradiance to <span>(1.32times 10^{-4})</span>. This result provides a technical basis for high-precision TSI measurement.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141143681","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}

{"title":"The Catalog of Hvar Observatory Solar Observations","authors":"Mateja Dumbović,&nbsp;Luči Karbonini,&nbsp;Jaša Čalogović,&nbsp;Filip Matković,&nbsp;Karmen Martinić,&nbsp;Akshay Kumar Remeshan,&nbsp;Roman Brajša,&nbsp;Bojan Vršnak","doi":"10.1007/s11207-024-02304-z","DOIUrl":"10.1007/s11207-024-02304-z","url":null,"abstract":"<div><p>We compile the catalog of Hvar Observatory (HVAR) solar observations in the time period corresponding to regular digitally stored chromospheric and photospheric observations 2010 – 2019. We make basic characterization of observed phenomena and compare them to catalogs that are based on full-disk solar images. We compile a catalog of observed active regions (ARs) consisting of 1100 entries, where each AR is classified according to McIntosh and Mt Wilson classifications. We find that HVAR observations are biased towards more frequently observing more complex ARs and observing them in longer time periods, likely related to the small field of view not encompassing the whole solar disk. In H<span>(alpha )</span> observations, we catalog conspicuous filaments/prominences and flares. We characterize filaments according to their location, chirality (if possible), and eruptive signatures. Analysis of the eruptive filaments reveals a slight bias in the HVAR catalog towards observation of partial eruptions, possibly related to the observers’ tendency to observe filaments that already showed some activity. In the flare catalog we focus on their observed eruptive signatures (loops or ribbons) and their shape. In addition, we associate them to GOES soft X-ray flares to determine their corresponding class. We find that HVAR observations seem biased towards more frequently observing stronger flares and observing them in longer time periods. We demonstrate the feasibility of the catalog on a case study of the flare detected on 2 August 2011 in HVAR H<span>(alpha )</span> observations and related Sun-to-Earth phenomena. Through flare–CME–ICME association we demonstrate the agreement of remote and in situ properties. The data used for this study, as well as the catalog, are made publicly available.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141152640","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}

{"title":"Cloud Removal of Full-Disk Solar H(alpha ) Images Based on RPix2PixHD","authors":"Ying Ma,&nbsp;Wei Song,&nbsp;Haoying Sun,&nbsp;Xiangchun Liu,&nbsp;Ganghua Lin","doi":"10.1007/s11207-024-02312-z","DOIUrl":"10.1007/s11207-024-02312-z","url":null,"abstract":"<div><p>Clouds in the sky can significantly affect full-disk observations of the Sun. In cloud-covered full-disk H<span>(alpha )</span> images, certain solar features become obscured, posing challenges for further solar research. Obtaining both cloud-covered and corresponding cloud-free images is often challenging, resulting in poor alignment of image pairs in the dataset, which adversely affects the performance of cloud removal models. We use RPix2PixHD, a novel network designed to translate cloud-covered images into cloud-free ones while mitigating the effects of misaligned data on the model. RPix2PixHD comprises two main components, Pix2PixHD and RegNet. Pix2PixHD includes a multiresolution generator and a multiscale discriminator. The generator takes cloud-covered images as input to produce cloud-free images. RegNet computes a deformation field using the generated cloud-free images and the ground truth cloud-free images. This deformation field is then used to resample the generated cloud-free images, resulting in registered images. The correction loss is calculated based on these registered images and utilized for training the generator, thereby enhancing the model’s cloud removal effectiveness. We conducted cloud removal experiments on full-disk H<span>(alpha )</span> images obtained from the Huairou Solar Observing Station (HSOS). The experimental results demonstrate that RPix2PixHD effectively removes clouds from cloud-covered solar H<span>(alpha )</span> images, successfully restoring solar feature details and outperforming comparative methods.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141050667","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}

{"title":"Rising of Two Crossing Prominences and the Resulting Oscillations","authors":"Hengyuan Wei,&nbsp;Zhenghua Huang,&nbsp;Qingmin Zhang,&nbsp;Ying Li,&nbsp;Hui Fu,&nbsp;Ming Xiong,&nbsp;Lidong Xia,&nbsp;Li Feng,&nbsp;Hui Li,&nbsp;Weiqun Gan","doi":"10.1007/s11207-024-02306-x","DOIUrl":"10.1007/s11207-024-02306-x","url":null,"abstract":"<div><p>Prominences are important features in the solar atmosphere. Their activities often develop into solar eruptions, such as flares and/or coronal mass ejections. We report here on observations of activities of two crossing prominences and the resulting oscillations observed with the Advanced Space-based Solar Observatory (ASO-S) and the Solar Dynamics Observatory. We observed the two crossing prominences rising simultaneously with a speed of about 100 km s⁻¹. The lower-lying prominence consists of threads that show increase of writhe during the rising process. We find evidence that the writhe of the lower-lying prominence is transferred into the overlying one. This transfer of writhe leads to a failure of the eruption of the lower-lying prominence and a shearing motion of the legs of the overlying prominence. The failed eruption of the lower-lying prominence also triggers kink oscillations of its threads, which show periods of about 300 s and amplitudes of less than 10 Mm. Such oscillations are considered to be intrinsic mode and can help to probe the magnetic field of the prominence. Our observations support the idea that the transfer and release of writhe play an important role in confining eruptions of a prominence, and interactions among prominences/filaments might be a crucial aspect of a solar eruption.</p></div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":"299 5","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141044528","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}