adsabs/AstroCLIMB huggingface dataset:
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: The reconstruction of the CME event on 2012 August 2 overlaid on the running-difference images of STEREO-A/COR2 (left) and SOHO/LASCO C2 (right). The blue wire frames in the images depict the reconstructed GCS geometry.
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: Sketch of the algorithm workflow. Our algorithm consists of three steps: region acquisition, model construction, and function optimization. A and B in the top right plot represent the different geometries observed from two viewpoints, and the plot is adopted from the work of M. Mierla et al. (2009).
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: The reconstruction of the CME event on 2012 November 9.
Paper: Automatic 3D Reconstruction of Coronal Mass Ejections Based on Dual-viewpoint Observations and Machine Learning
Authors: Rongpei Lin, 荣沛 林, Yi Yang, 易 杨, Fang Shen, 芳 沈, Gilbert Pi, Yucong Li, 雨淙 李
Figure caption: The reconstruction of the CME event on 2012 January 8.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: Mean proper-motion vectors overlaid on the QSF finding chart. QSFs are indicated with contours, and those with filled contours have optical counterparts (B.-C. Koo et al. 2018). The filled QSFs without vectors are those for which proper motions could not be determined due to their location in complex environments. The vector scale is provided in the bottom left corner. The background blue contour outlines the main ejecta shell, traced by [Fe II] emission (Figure 1), while the filled blue star symbol marks the explosion center.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: (Left) Proper-motion map of Knot 24 as shown in Figure 2. The background image is the 2014 HST F625W image, with contours indicating the brightness distribution. The inset displays the average [Fe II] 1.644 μm spectrum of Knot 24 adapted from B.-C. Koo et al. (2020). North is up, and east is to the left. (Right) A schematic figure describing the key features of Knot 24 and its surrounding environment.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: (a) R.A. component of the proper motion of QSFs vs. their projected distance from the expansion center along R.A. The solid line represents the least-squares fit. (b) Same as (a), but for the decl. component of the proper motion. Blue symbols indicate Group 1 QSFs, while magenta symbols represent Group 2 QSFs.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: (a) vLOS vs. r⊥. The solid line represents the relationship when the QSFs are confined to a thin spherical shell near the SN blast wave at r = 170″ and expand radially at 300 km s−1. (b) vLOS vs. vμ. The solid lines represent the relationship when the QSFs expand radially at 100 or 300 km s−1. In both panels, the dotted horizontal lines mark the systemic LOS velocity of the Cas A SNR. Blue symbols indicate Group 1 QSFs, while magenta symbols represent Group 2 QSFs. Radial velocities are adopted from A. Alarie et al. (2014) (see Table 2).
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: (a) Proper-motion angle (θμ) vs. P.A. angle of QSFs (θ). The solid line indicates θμ= θ. (b) The difference θμ − θ vs. the projected distance of QSFs from the explosion center. The dotted lines indicate θμ − θ  = ​​​​±30°. Blue symbols indicate Group 1 QSFs, while magenta symbols represent Group 2 QSFs. The error bar with an arrowhead indicates continuation beyond the plotted range for a data point with an uncertainty exceeding the axis limits.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: (a) Comparison of our measured values of μα and those of S. van den Bergh & K. Kamper (1985). (b) Similar comparison for μδ. For the μδ values from van den Bergh and Kamper, we subtracted 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩008 to account for the proper motion of reference stars in their work (S. van den Bergh & K. Kamper 1985). In both panels, the dashed line indicates where the two measured values are equal.
Paper: Proper Motion of Dense Circumstellar Knots in the Supernova Remnant Cassiopeia A
Authors: Bon-Chul Koo, Sang Bum Ko, Christopher F. McKee, Carl Heiles, Robert A. Fesen, Ji Yeon Seok, Hyun-Jeong Kim, Sung-Chul Yoon
Figure caption: Proper motion of QSFs vs. the projected distance of QSFs from the explosion center. Blue symbols indicate Group 1 QSFs, while magenta symbols represent Group 2 QSFs.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Comparison of bump parameter distributions (top panels) and composite spectra (bottom panels) of quasars with and without BALs and NALs.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Redshift vs. 2175 Å bump strength for different dust absorber populations. The quasar-associated 2175 Å dust absorbers are represented by black points. The blue circles indicate dust bumps observed in the MW, the navy circles denote bumps in the SMC, while the cyan and green circles correspond to those in the LMC average and LMC 2 supershell, respectively. The purple squares represent the average values at different redshifts, revealing a general trend of decreasing 2175 Å bump strength with increasing redshift. For comparison, 2175 Å dust absorbers associated with other absorption systems and GRB afterglows are also shown: the red triangles represent the dust bumps detected in C I absorbers, the orange triangles correspond to those found in Mg II absorbers, while the maroon triangles mark the bumps identified in Ca II absorbers. The olive stars denote the 2175 Å bumps observed in GRB optical afterglows.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Top: comparison of bump parameters with 2175 Å bumps in the MW (blue circles), the LMC average (cyan circles), the LMC 2 supershell (green circles), and the SMC (navy circles). The quasar-associated 2175 Å dust absorbers are labeled with black points. Bottom: the colored plots display the average extinction curves with errors of quasar-associated 2175 Å dust absorbers at four different redshift bins. The extinction curves in the MW, LMC average, LMC 2 supershell, and SMC are also plotted for comparison.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Best-fit extinction models for two rejected candidates reported by P. Jiang et al. (2011). The annotations are the same as those in Figure 1.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Redshift distribution of the quasar-associated 2175 Å dust absorbers (black curve), with that of the DR16Q quasars (gray curve) overplotted for comparison.
Paper: The Quasar-associated 2175 Å Dust Absorbers in the SDSS DR16 Quasar Catalog
Authors: Shaohua Zhang, Yuchong Luo, Shangchun Xie, Chao Gao, Zhijian Luo, Chenggang Shu, Hubing Xiao
Figure caption: Distribution of quasar-associated 2175 Å dust absorbers in equatorial coordinates (map centered at R.A. = 8 hr).
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: Classification of sensitivity in response curves (cyan) in signal injection experiments by detection thresholds (DT, red), beyond which output exceeds expectation values from background (gray). Background is defined following time randomization of data, effectively equivalent to noise without signal (when noise is white). Faded cyan and gray bands indicate ±1σd and ±1σr, respectively. DTμ and DTσ indicate the smallest signal amplitudes α at which the cyan band departs from the black line and gray band, respectively, here highlighted by red dots. DTs facilitate the ranking of different methods of analysis.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: Schematic of a two-channel pipeline processing data ﹩\left({\boldsymbol{p}},{\boldsymbol{q}}\right)﹩ from detectors ﹩\left({D}_{1},{D}_{2}\right)﹩, across different junctures Ji (i  = 1, 2, 3) for cross correlation. Cross correlations can be performed by direct cross correlations (DCC), Pearson coefficients (PC), and excess probability ratio (EPR), discussed in the present work, applied to raw data for DCC or PC (Section 2) at J1, PC and EPR at J2 following a filter (F1), or further down the pipeline by EPR following a second filter (F2). For EPR applied to real or complex-valued data ﹩\left({\boldsymbol{p}},{\boldsymbol{q}}\right)﹩, these filters may include a threshold (Equation (1)) for conversion into Boolean data, or filters for signal amplification prior to cutoff application.
Paper: Efficient Searches for Small Signals across Two-channel Noisy Data: A Challenge in Big-data Observations
Authors: Maryam Aghaei Abchouyeh, Maurice H. P. M. van Putten, Seyong Kim
Figure caption: (Left) Data reduction shown by the fraction of data remaining after the cutoff (Equation (1)) as a function of κ for a given background noise. Results shown cover the three backgrounds of Gaussian, Poisson, and uniform distributions in the absence of a common signal. The yellow dashed curve shows the result for the Gaussian background, which nicely matches the theoretical complementary error function (red dashed line). (Right) Essentially the same data reductions appear in the presence of signals, here studied across 15 different combinations of backgrounds and signals at strength α = 0.5 (Section 4.1). The yellow dashed line shows the result for a Gaussian signal in a Gaussian background (G-G). The exchange of leading curve between the uniform background to Poisson background between the left and right panels is notable.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: Spectra of 10 types of Hα emission line.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: An example of the YSO candidates, which exhibit [N II] emission lines, [S II] emission lines, an [O I] emission line, and a He I emission line.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: The structure of the Bi-LSTM-CNN model and the structure of the corresponding LSTM unit and CNN unit.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: Examples of samples with new Hα emission-line features.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: Confusion matrix of the Li absorption line identification model.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: An example of a YSO spectrum and the corresponding Li absorption line.
Paper: A Catalog of Hα Emission-line Stars and 785 Newly Identified Young Stellar Object Candidates from LAMOST Based on a Deep Learning Method
Authors: Lei Tan, 磊 谈, Ying Mei, 盈 梅, Jiale Qian, 家乐 钱, Xiaolong Wang, 小龙 王, Yue Cui, Aixin Huang, 爱新 黄, Feng Wang, 锋 王, Hui Deng, 辉 邓, Chao Liu, 超 刘, Huanbin Chi, 焕斌 迟
Figure caption: Confusion matrix of the Hα emission-line star identification model.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Distributions of orbital and stellar parameters for EA-type (cyan), EB-type (magenta), and EW-type (gold) eclipsing binaries in our sample. Left panel: orbital period vs. metallicity [Fe/H]. Middle panel: Teff vs. ﹩{\mathrm{log}}\,g﹩. Right panel: orbital period vs. Teff. The three subtypes exhibit distinct clustering behaviors, with EW systems consistently occupying the short-period, low-temperature, and high-gravity regime, consistent with their contact binary nature. Density centers are marked with filled star symbols.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Teff–logg diagram color coded by metallicity [Fe/H] for the eclipsing binary sample. Most systems lie along the main sequence, while a subset extends toward the giant branch. The color gradient reveals systematic metallicity variation across evolutionary stages.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Left panel: distribution of eclipsing binaries observed by LAMOST in the Galaxy. Right panel: statistics of eclipsing binaries with multiple observations by LAMOST.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Top-left panel: distribution of chromospheric emission index ﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ vs. orbital period (in logarithmic scale) for the sample. Color scale indicates the number of sources per hexagonal bin in logarithmic scale. Top-right panel: scatter plot of ﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ vs. ﹩{\mathrm{log}}\,{P}_{{\mathrm{orb}}}﹩ with median values binned in steps of 0.125 dex (red curve), and a best-fit linear trend (black dashed line) given by y = ​​−0.25x −4.38. A weak but significant negative correlation is observed between chromospheric activity and orbital period. Bottom panel: same diagram as panel (a), but shown separately for EA-type (left), EB-type (middle), and EW-type (right) systems. EW binaries form a compact distribution near the saturation limit (﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }\approx -4.1﹩), whereas EA and EB binaries exhibit a broader spread over both saturated and unsaturated regimes.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Top-left panel: distribution of ﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ vs. ﹩{\mathrm{logRo}}﹩ for the sample. Color indicates the number of sources per hexagonal bin on a logarithmic scale. Top-right panel: shown as a scatter plot with binned median values overlaid in red. Chromospheric activity rises with decreasing Ro and saturates near ﹩{\mathrm{logRo}}\sim -1.3﹩ to –1.6, followed by a slight decline toward the fastest rotators. Bottom panel: median trends of ﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ vs. ﹩{\mathrm{log}}\,Ro﹩ for EA-type (left) and EW-type (right) binaries. EW systems show a broader saturation plateau and reach peak activity at a smaller Rossby number (﹩{\mathrm{logRo}}\approx -1.6﹩), compared to EA systems (﹩{\mathrm{logRo}}\approx -1.3﹩), consistent with delayed saturation in contact systems with a common convective envelope.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: EW﹩{}_{{\rm{H}}\alpha }^{{\prime} }﹩ vs. Teff for eclipsing binaries. Left panel: color coded by eclipsing binaries subtype, with density centers marked. Right panel: density map of the full sample. A clear decrease in EW﹩{}_{{\rm{H}}\alpha }^{{\prime} }﹩ with increasing temperature is seen, with most active stars clustering around 5000–6000 K.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Top-left panel: mass distribution of flaring systems. Top-right panel: distribution of bolometric flare energy (Ebol). Bottom-left panel: distribution of flare durations. Bottom-right panel: flare amplitude distributions. EA, EB, and EW systems are shown in cyan, magenta, and gold, respectively.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Left panel: photometric modulation amplitude Reff vs. Teff. Right panel: Reff vs. orbital period. EA, EB, and EW types are color coded. The spot amplitudes show weak trends with both parameters and large intrinsic scatter.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Correlation between photometric modulation amplitude Reff and bolometric flare energy (﹩{\mathrm{log}}\,{E}_{{\mathrm{bol}}}﹩) for EA (left), EB (middle), and EW (right) systems. All types show increasing trends, with the clearest relation seen in EA-type binaries.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Normalized distributions of bolometric flare energy (﹩{\mathrm{log}}\,{E}_{{\mathrm{bol}}}﹩) for EA (blue), EB (orange), and EW (green) systems. All three types show similar energy ranges, with EA systems skewed toward higher energies.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: FFDs for EA (left), EB (middle), and EW (right) binaries. Solid lines indicate the best-fit power-law model with slope indices α labeled. Vertical dashed lines mark the fitting thresholds.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Distribution of ﹩{\mathrm{log}}\,{R}_{{\rm{H}}\alpha }^{{\prime} }﹩ for EA, EB, and EW systems. EW-type binaries show a broader and more extended tail toward higher activity levels.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Left panel: fraction of flare active systems by EB subtype. Middle panel: fraction of flares across Teff bins. Right panel: fraction of flares across mass bins. Flare occurrence is highest in cool, low-mass stars and peaks in EB-type systems.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Bolometric flare energy as a function of Teff (left) and stellar mass (right). All subtypes exhibit rising trends, with energy increasing steeply toward higher Teff and mass.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Number of flaring vs. total eclipsing binaries binned by Teff for EA, EB, and EW types.
Paper: Physical Parameters and Chromospheric Activity of Eclipsing Binaries Observed by the LAMOST DR10 Survey
Authors: Ansong Shi, Li-yun Zhang, Tianhao Su, Yinpeng Wang, Qi An, Xianming L. Han, Prabhakar Misra, Linyan Jiang, Rui Guo, Qingfeng Pi
Figure caption: Same as Figure 17, but binned by stellar mass.