adsabs/AstroCLIMB huggingface dataset:
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The count rate (counts s−1 ) distribution of the background of the three telescopes of Insight-HXMT during blank-sky observations. The blue and purple lines represent LE (1−10 keV) and ME (10−30 keV), respectively. The green line is for NaI detector #04 of HE (28−250 keV), for which the spike events were attempted to be removed using HXMTDAS. NaI detector #04 could represent other NaI detectors of HE. The HE detectors are denoted as 00−17 (detector #16 is the blinded detector, which is not used in this work).
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Top: summed light curves of all NaI detectors for a burst candidate that was included in the preliminary bursts list but identified as spikes in this work. T 0 is the trigger time. The blue line is the light curve made with raw data without removing spikes (i.e., Level 1K data), while the orange line is the light curve made with the Level 1L data for which we tried to filter out the spike events using HXMTDAS. However, the residual spike counts are still clearly seen. Bottom: the difference between the raw light curve and the light curve after removing spikes shown in the top panel.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The light curves of 18 NaI detectors of HE. Left: T 0 is the trigger time of a burst candidate that is identified as the SGR J1935+2154 burst. Count increases are seen in all detectors, except for the blinded detector (det #16). Right: light curves for a burst candidate that is identified as a spike in this work. The excess counts are only seen in a few adjacent detectors, which is a characteristic of spikes.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Illustration of burst duration. Light curves of burst #56 are shown in separate panels. The yellow, orange, and blue shaded regions represent the duration of LE, ME, and HE, respectively. The red dashed lines indicate the common duration of the three telescopes defined in this work.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The results of applying the CPG μB (ε) construction and the NPTF ρ(f) construction to the nonuniform spatial distribution scenario. The CPG posteriors are clustered around the injected population, while the NPTF posteriors show a bias toward higher N. The averaging procedure in constructing ρ(f) results in a detector correction that is not representative of any of the bins in the image, as shown by the μB (ε) functions. Left: The recovered posterior for both the CPG μ  B (ε) construction and the NPTF ρ(f) construction. The solid red line shows the (true) injected source-count function. Each of the colored dashed and dotted lines are the 1σ and 2σ HPD regions, respectively, for separate trials. Right: The detector effect correction function for both the CPG μ  B (ε) construction and the NPTF ρ(f) construction (converted to ρ  B (ε) for comparison as described in the text). Here, each colored line corresponds to the function for a bin in the image.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The posterior for the fraction of flux assigned to the point-source population, ω = F PS/(F  P  + F PS), when analyzing data sets generated from purely a Poisson distribution, but analyzed with both a Poisson and point-source template using the CPG likelihood. The median posterior (over multiple random trials, for each bin) is shown by the solid line, while the 16% to 84% quantile range is shown by the fill. The four panels correspond to different prior choices, representative of common choices in the literature. None of the choices of prior result in a uniform posterior for ω; instead, the posterior is biased toward assigning all flux to one model component or another, which could easily be misleading unless accounted for.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: As in Figure 10, but for the anisotropic PSF scenario. The injected population is well recovered by CPG, while the NPTF posteriors are clearly biased toward low N. The cusp structure visible in each μB (ε) is smeared out in ρ  B (ε). Left: the recovered posterior for both the CPG μ  B (ε) construction and the NPTF ρ(f) construction. Right: the detector effect correction function for both the CPG μ  B (ε) construction and the NPTF ρ(f) construction.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: As in Figure 10, but for the variation in sub-bin effective area scenario. The CPG posteriors are clustered around the injected population, while the NPTF posteriors exhibit a small bias toward low N. The bimodal effective area is shown clearly by μ  B (ε), while for ρ  B (ε) this structure is removed by the averaging the effective area, resulting in a single mode. Left: the recovered posterior for both the CPG μ(ε) construction and the NPTF ρ(f) construction. Right: the detector effect correction function for both the CPG μ(ε) construction and the NPTF ρ(f) construction.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: Two separate observations with dashed boundaries form a mosaic. (a) In areas where the observations overlap, the PSF will be an appropriate mixture of the PSF for each observation. Near the edge of the observation, we show an example of how the PSF can be highly distorted in the radial direction, as expected for NuSTAR observations. The mixture forms a cross, with the PSF from the left observation lying diagonally NW–SE and the PSF from the right observation lying diagonally SW–NE. (b) The detector response, κ( x ), is a sum of the response for each observation, and varies smoothly across the mosaic as the response extends outside the observation boundaries. (c) In contrast, the detector efficiency, η( y ), has a sharp transition from unity to zero at the observation boundary, and will generally be nonsmooth across any bin that straddles these boundaries.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: Left: A template has all of its probability concentrated in a single bin, shown as the 2D histogram on the left. As such, all three sources, { x  1,  x  2,  x  3}, are located within this bin. Each has an associated PSF shown as the solid distribution centered on the source location. Top Right: The probability distribution for the number of counts in the central bin. The distribution for conserved flux, as in the NPTF construction, is shown in dotted red. The actual distribution is shown in black, with a smaller mean. Bottom Right: The distribution for an adjacent bin. The red dotted line shows the distribution for the NPTF construction with a zero mean. The black shows the actual distribution, which has a nonzero mean.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The posterior for the fraction of flux assigned to the point-source population, ω = F PS/(F  P  + F PS), under the natural coordinate system. The median posterior (over multiple random trials, for each bin) is shown by the solid line, while the 16% to 84% percentile range is shown by the fill. Ideally, the posterior for ω should be uniform, as the diffuse emission cannot be distinguished from a below-threshold point-source population, and unlike the standard system shown in Figure 6, the new natural coordinate system recovers a uniform posterior—with the exception of the log-uniform N, uniform F priors, as discussed further in the text.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: Bottom: The detector response, κ( x ), varies sharply over bin b. The average detector response for this bin, ﹩{\bar{\kappa }}_{b}﹩, is shown by the dashed line. Top: If the average detector response is used to convert flux to counts, the probability distribution follows the red dotted comb; however, the within-bin variation of the detector response must create two modes in the distribution, shown by the black comb.
Paper: A Compound Poisson Generator Approach to Point-source Inference in Astrophysics
Authors: Gabriel H. Collin, Nicholas L. Rodd, Tyler Erjavec, Kerstin Perez
Figure caption: The posterior for the mean number of sources N, and total flux F  T , under the natural coordinate system for the log-uniform N, uniform F prior scenario. The total flux is tightly constrained for N > 1; however, it becomes completely unconstrained once the mean number of sources is less than one in the whole population (N < 1).
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: the scatter plot of hardness ratio vs. duration. Right: the evolution of hardness ratio of each burst in 28−250 keV and 10−30 keV, 10−30 keV and 1−10 keV. The gray dotted lines represent the time interval of no observation (see also Table 1). The red star is FRB 200428−Associated Burst.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. I. Burst Catalog
Authors: Ce Cai, Wang-Chen Xue, Cheng-Kui Li, Shao-Lin Xiong, Shuang-Nan Zhang, Lin Lin, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Yan-Qiu Zhang, Shuo Xiao, You-Li Tuo, Qi-Bin Yi, Zhi Wei Guo, Sheng Lun Xie, Yi Zhao, Zhen Zhang, Qing-Xin Li, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: Left: the scatter plot of the waiting time and common duration (T bb) for 21 bursts. Right: the scatter plot of the waiting time and fluence (see Paper II) for 21 bursts. The blue and green points represent the two bursts used to obtain the waiting time. The red star is FRB 200428−Associated Burst, which is the latter burst of their pair bursts. The red square is the earlier burst of FRB 200428−Associated Burst.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The comparison of the effective temperatures derived from our method with the APOGEE DR17 spectroscopic values. The top-left panel shows the T eff comparison for dMs, while the top-right panel is for gMs. The bottom-left and bottom-right panels show the residuals’ distributions for dMs and gMs, respectively. The color scale, as well as the contour lines, indicates the number density of each region.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The systematic errors of stellar parameters as functions of the S/N. Red error bars represent the standard deviations in each S/N bin, and the red dots in the center are the means. The yellow dashed lines are linear regressions of the means.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Left panel: the Kiel diagram colored by different metallicity groups of the samples with S/N > 20. Lines correspond to 10 Gyr PARSEC isochrones with [Fe/H] = −0.6, −0.3, and 0.0 dex, respectively. Right panel: the same Kiel diagram but for stars of S/N < 20.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The internal uncertainties in different stellar parameters and S/N values. The values in each box stand for the standard deviation of residuals within each interval.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Same as Figure 10, but for metallicity.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The random errors of stellar parameters as functions of S/N. The dMs (top) and gMs (bottom) are grouped into different temperature bins. The dots represent the standard dispersion in each S/N bin.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The percentage for the stars with S/N below 10, from 10 to 20, 20 to 30, 30 to 40, and above 40.
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: The histograms of [Fe/H] for dMs (top panel) and gMs (bottom panel). The histograms only display the [Fe/H] range from −1.6 dex to 1.0 dex, as there are only a few metal-poor stars ([Fe/H] < −1.6 dex).
Paper: Stellar Atmospheric Parameters of M-type Stars from LAMOST DR8
Authors: Ming-Yi Ding, Jian-Rong Shi, Yue Wu, Hugh R. A. Jones, Hong-Liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Tai-Sheng Yan, Xiao-Jin Xie
Figure caption: Same as Figure 10, but for surface gravity.
Paper: Experimental and Theoretical Radiative Parameters of Highly Excited Odd-parity Levels in Ir II 
Authors: Huiting Ma, Meina Liu, Yidan Geng, Ting Wang, Ziqing Yu, Hongfeng Zheng, Sébastien Gamrath, Pascal Quinet, Zhenwen Dai
Figure caption: A typical fluorescence decay curve of the Ir II 55,852.50 cm−1 level with the fitted convolution curve between the laser pulse and an exponential.
Paper: Experimental and Theoretical Radiative Parameters of Highly Excited Odd-parity Levels in Ir II 
Authors: Huiting Ma, Meina Liu, Yidan Geng, Ting Wang, Ziqing Yu, Hongfeng Zheng, Sébastien Gamrath, Pascal Quinet, Zhenwen Dai
Figure caption: A typical fluorescence decay curve of the Ir II 50,302.01 cm−1 level with an exponential fit.
Paper: Predicting Solar Energetic Particles Using SDO/HMI Vector Magnetic Data Products and a Bidirectional LSTM Network
Authors: Yasser Abduallah, Vania K. Jordanova, Hao Liu, Qin Li, Jason T. L. Wang, Haimin Wang
Figure caption: Collecting and constructing positive and negative data samples on a flaring AR for the FC_S problem where T = 24 hr and making predictions based on the collected data samples. The data samples are collected at a cadence of 12 minutes. Each rectangular box corresponds to 1 hr and contains five data samples. The red vertical line shows the peak time of an M- or X-class flare. (a) The blue rectangular boxes contain data samples that are within the 24 hr prior to the peak time of an M- or X-class flare that produces a CME and an SEP event; these blue data samples belong to the positive class. (b) The green rectangular boxes contain data samples that are within the 24 hr prior to the peak time of an M- or X-class flare that produces a CME but no SEP event; these green data samples belong to the negative class. (c) Illustration of a correct prediction for a test data sample x  t  that is predicted to be positive. (d) Illustration of a correct prediction for a test data sample x  t  that is predicted to be negative. (e) Illustration of a wrong prediction for a test data sample x  t  that is predicted to be negative. (f) Illustration of a wrong prediction for a test data sample x  t  that is predicted to be positive.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Top panels: three snapshots of the AIA 304 Å images, showing the evolution of the C4.2-class flare in AR 12434 on 2015 October 16. The white arrows point to the accompanying minifilament eruption and coronal jet. In panel (a3), the location and total area of the flare are labeled. The remote brightening is outlined by the cyan line. The total length and average distance between the flare and remote brightening are labeled. Middle panels: additional three cases observed in 304 Å. The flare ribbons are fitted with a circle and two ellipses (dashed cyan lines). The centers are pointed by solid arrows. Bottom panels: corresponding LOS magnetograms of the three events observed by HMI.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Percentages of M- and X-class CFs in different groups of area (a), lifetime (b), total length of remote brightening (c), and average distance of remote brightening (d).
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: (a) Locations of the 134 CFs, which are marked with cyan dots (confined flares) and red dots (eruptive flares). The latitudes and longitudes of the Sun are drawn with gray lines. (b) Latitude distribution of the CFs. Positive (negative) latitude means northern (southern) hemisphere.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Distribution of the flare area. The result of the curve fitting using the lognormal function is superposed with a red line. Two values significantly exceeding 5000 Mm2 are excluded in this plot.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Distribution of the equivalent radius of flare ribbons.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Association rates of CFs with remote brightenings (a), type III radio bursts (b), jets (c), minifilament eruptions (d), and CMEs (e) for B-, C-, M-, and X-class flares, respectively.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Proportions of CFs related to remote brightenings, type III radio bursts, jets, minifilament eruptions (FEs), and CMEs.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Scatterplot between the total length (L RB) and average distance (D RB) of remote brightenings. The result of linear fitting is plotted with a red dashed line. The correlation coefficient (∼0.65) is labeled.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Distributions of the total length (L RB) and average distance (D RB) of remote brightenings associated with CFs.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: (a) AIA 304 Å image of the M1.4-class CF occurring in AR 11476 on 2012 May 8. (b) Radio dynamic spectra of the flare recorded by the e-Callisto/BLEN7M station. The arrows point to the type III radio bursts. The white dashed lines mark the start and peak times of the flare.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: (a) SXR light curve (blue line) and 131 Å light curve (orange line) of the C3.0-class flare occurring in AR 11936 on 2013 December 28. The three black dashed lines denote the start, peak, and end times of the flare. (b)–(d) AIA 131 Å images of the flare.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Scatterplot between the area (A CF) and lifetime (τ CF) of CFs. The correlation coefficient is ∼0.50.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Distribution of the lifetime of CFs. The result of curve fitting using the lognormal function is superposed with a red line.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: (a) SXR light curve of the M8.7-class flare occurring in AR 12242 on 2014 December 17. The three black dashed lines denote the start, peak, and end times of the flare. (b)–(d) AIA 131 Å images of the flare.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: Distribution of the peak SXR flux in 1–8 Å. The power-law index α is labeled.
Paper: Statistical Analysis of Circular-ribbon Flares
Authors: Yanjie Zhang, Qingmin Zhang, Dechao Song, Shuting Li, Jun Dai, Zhe Xu, Haisheng Ji
Figure caption: (a) AIA 304 Å image of the M7.3-class flare in AR 12036 on 2014 April 18. (b) WL image of the associated CME at a speed of 1203 km s−1 in the LASCO/C2 FOV.