adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: The parameter region in which the mass accretion onto a seed BH would be suppressed on the plane of ambient temperature T ∞ and the maximum photon energy of the irradiation flux ﹩{E}_{\max }﹩ (shaded region). The spectral index of the irradiation flux and the BH mass are set as α = 1 and M BH = 3 × 105  M ⊙, respectively.
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: Schematic picture of the thermal structure around a Bondi-accreting seed BH. R B and R Comp are the Bondi radius and Compton radius (see Section 3.2), respectively.
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: Mean photon energy of the irradiation flux, 〈ϵ〉, as a function of maximum photon energy, ﹩{E}_{\max }﹩, in cases with α = 1.0, 1.1, and 1.2 is  shown. The minimum photon energy is fixed as 13.6 eV.
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: Same as Figure 2 but with α = 1.2 and M BH = 3 × 105  M ⊙.
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: Same as Figure 2 but with α = 1.2 and M BH = 7 × 105  M ⊙.
Paper: Effects of Heat Conduction on Blocking off the Super-Eddington Growth of Black Holes at High Redshift
Authors: Norita Kawanaka, Kazunori Kohri
Figure caption: Same as Figure 2 but with α = 1 and M BH = 7 × 105  M ⊙.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Typical spectra of the real frequencies. Panels (a) and (b) show two real frequencies f 1 = 17.597 day−1 and f 3 = 31.428 day−1; panels (c) and (d) show two modulation terms f 8 = 0.065 day−1 and f 9 = 1.693 day−1, respectively.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Amplitude spectra of KIC 9845907 using the SC data. The upper panel shows the amplitude spectrum in the 0–100 c/day range. The lower panel represents the distribution of detected 85 frequencies.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: A 2 day section of the Kepler SC light curve of KIC 9845907. The amplitude of the light curve is about 0.1 mag. BJD is barycentric Julian date.
Paper: Dynamics of Threads Wrapping a Filament's Leg Prior to the Eruption on 2021 October 28
Authors: Yue Fang, Jun Zhang, Yi Bi, Zhiping Song
Figure caption: Overview of AR 12887 and the X-class flare. (a): GOES 1–8 Å light curve on 2021 October 28. An X-class flare is highlighted by an orange bar. (b1): GONG Hα wave band image showing the two filaments (F1 and F2) in this AR. The cyan square (FOV1) outlines the FOV of Figures 3(a1)–(a5), (b1)–(b2), Figure 4(a), and Figure 6. (b2): HMI LOS magnetogram displaying the magnetic fields in this AR. The purple square (FOV2) outlines the FOV of Figures 2(a1)–(a5). The two yellow curves denote the locations of F1 and F2, and the white arrows in (b1) and (b2) denote the east part of F1. Contours of the magnetic fields (N1, P1, N2, and P2) where footpoints of F1 and F2 are anchored in separately are overlaid on (b1) and (b2). (b3): AIA 304 Å image showing the X-class flare produced by the two filaments’ eruption. Black arrows indicate that some material from the erupted F1 fell on P1.
Paper: Dynamics of Threads Wrapping a Filament's Leg Prior to the Eruption on 2021 October 28
Authors: Yue Fang, Jun Zhang, Yi Bi, Zhiping Song
Figure caption: Formation of F2 and material flows in F1. (a1)–(a5): Sequence of 304 Å images displaying the formation of F2. The arrow in (a3) indicates the appearance of the dark ribbon. The yellow and cyan dotted curves in (a5) denote F1 and F2, respectively; (b): HMI LOS magnetogram. The cyan curve denotes the location of F2. Green and blue contours in (a4), (a5), and (b) mark magnetic fields (P2, N1, and N2) saturated in ±500 G; (c1)–(c3): enlarged 304 Å images showing the material flows in the F1. The curve fa-fb in (c1) marks the position of the time–distance plot in (d). The arrows in (c2) and (c3) indicate bright materials; (d): time–distance plot of 304 Å images showing the flows in F1.
Paper: Dynamics of Threads Wrapping a Filament's Leg Prior to the Eruption on 2021 October 28
Authors: Yue Fang, Jun Zhang, Yi Bi, Zhiping Song
Figure caption: (a1)–(a5): Sequence of HMI LOS magnetograms displaying the magnetic evolution of N1 and P2 before the X-class flare onset. The blue and green contours represent the magnetic fields N1 and P2 saturated in ±500 G. Yellow and red plus symbols denote the center of N1 and P2, respectively. Yellow dotted lines represent the major axis of N1; (b): linear velocity (blue diamonds) and angular velocity (red triangles) of N1 from 01:00 UT on October 27 to 16:00 UT on October 28.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: (a)–(e) Contours: emission region of the H13CO+ (1-0) line in three velocity intervals. The background image is the H13CO+ emission in (−1.5,+1.5) km s−1 (red-center component). For the blue-wing component, the contour levels are 4, 6, and 8 times of the rms level (0.3 K km s−1). For the other components, the contour levels are 10%–90% in 20% steps of the peak intensity, which is 15, 11, and 3 K km s−1 for the blue-center, red-center, and red-wing, respectively. The green arrows label the mass transfer flow directions onto the main filament (Chen21). The green circles label the possible arrival points of the transfer flows onto the filament. (f) PV plot and intensity profile along the major axis of the main filament. The sampling direction is labeled in dashed line in panel (a). The vertical dashed lines denote the projected offset of the three dense cores on the sampling direction. The horizontal dotted line represents the average systemic velocity of the filament.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: (a) The velocity-integrated intensity of the H13CO+ (1-0) line (false-color) and 3 mm continuum. The contour levels are 4σ rms (1.6 mJy beam−1) to 84σ rms (peak) in step of 16σ rms. (b) The H13CO+ and CH3OH emission regions around the main filament, overlaid on the IRAC-RGB image (3.6, 4.5, and 8.0 μm bands). The H13CO+ contours are 15%–90% in 15% steps of the peak intensity (8.5 K km s−1). The CH3OH contours are 10%–90% in 20% steps of the peak intensity (18.7 K km s−1). The dashed circles label the area of each core. (c) Upper and lower panels: the spectra at the selected core centers. The blue and red shaded areas indicate the velocity ranges of the two velocity components, respectively. The vertical dashed line denotes the division between the blueshift (core M1) and main-filament components.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: Left column: the emission regions of the blue- (contours) and redshifted (false-color) components in CCH and ﹩{{\rm{H}}}^{13}\mathrm{CN}﹩ (1-0) lines. The contour levels are 20%–90% of the peak intensity. Right column: the PV diagrams of the two molecular lines. the ﹩{{\rm{H}}}^{13}\mathrm{CN}﹩ emission at v lsr = 2–4 km s−1 is from another hyperfine component (HFC) of F = 1–1. The HFCs of ﹩{{\rm{H}}}^{13}\mathrm{CN}﹩ are separated for 6–7 km s−1 and would not blend with each other. The CCH (1-0) emission shows an additional small blueshift wing around M3, which should correspond to the transfer flow onto the filament (Chen21). This feature is not seen in other lines probably because of their lower optical depths.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: (a) The ridge lines of the two velocity components, blue component in blue line and dots, red-center component (main filament) in yellow line and dots. The dot size is proportional to the integrated intensity. The arrows denote the projected moving direction of each component expected on the sky plane. (b) The transverse offset and velocity difference between the ridge lines of the two components along the filament axis. In the lower panel, the blue and red dots represent the peak radial-velocity profile of the two components, respectively. The gray dots represent ∣v blue − v red∣. (c) A schematic view of the gas motion on the filament and cores.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: The peak velocity and line-width distributions of the two components as observed in three molecular lines. The velocity ranges to measure the blueshift-core and main-filament components are (−4, − 1.5) and (−1.5, 2) km s−1, respectively. Left two columns: the radial-velocity distributions of the two components. Right two columns: the line-width distributions of the two components.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Top: radius of the expanding shells, R sh, as a function of time in different inclinations above and below the accretion disk: θ = 0 ray points along the rotation axis of the disk in the upper hemisphere, and θ = π points along the rotation axis in the opposite direction (Figure 4). Bottom: the expansion velocity of the shell, v sh, along the same directions. The outflow is asymmetric with respect to the disk midplane.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Shell velocity, v sh, along various rays, as a function of the shell radius, R sh. The escape velocity from the region is shown for M( < R sh), which is the total mass within R sh, i.e., the gas, the sink, and the DM interior to the shell radius (black solid line).
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Evolution of the specific angular momentum of accreting gas on a scale of 0.01 pc normalized by the circular specific angular momentum.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Accelerations acting on the shell: thermal pressure gradient, radiation, and gravitational acceleration profiles as a function of radius, R, along the θ = π ray, at t ∼ 1000 yr (top) and t = 3.2 × 103 yr (bottom).
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Ionization fraction profiles measured along the θ = π ray at a few representative times.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Performance of machine-learning approaches in identifying CMR filaments. The first column displays the combined dust emission, which includes the emission from both CMR filaments and the turbulent cloud. The second column shows the ground truth, i.e., the actual location of the CMR filaments. The CMR filaments are defined by applying a density cutoff (n > 500 cm−3) during the radiative transfer process. This cutoff excludes the low-density ambient gas and focuses solely on the dense structure of CMR filaments. Additionally, we exclude dense structures that are distant from the collision site, as they do not belong to the CMR filaments. The third and fourth columns illustrate the predicted locations of CMR filaments from CASI-2D and the diffusion model, respectively.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: The ROC curves for the predictions made by CASI-2D (left) and the changes in the TPR and FPR as the prediction threshold is adjusted (right). By selecting a threshold of 0.01, a relatively high TPR of 80% can be achieved, while keeping the FPR below 2%.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: The ROC curves for the predictions made by the diffusion model (left) and the changes in the TPR and FPR as the prediction threshold is adjusted (right). By selecting a threshold of 0.8, a relatively high TPR of >70% can be achieved, while keeping the FPR below 5%.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: An illustration of the process of combining CMR filament dust emission with turbulent cloud dust emission maps. The upper left panel displays the CMR filament dust emission map, while the upper right panel shows the turbulent cloud dust emission map. The lower left panel represents the Gaussian random noise map, and the lower right panel showcases the combination of these three maps.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Distribution of the center frequency (ν 0) and spectral width (Δν) of the FRB 20220912A bursts fitted by Gaussian functions. The blue dots and lines in the figure represent bursts with peak frequency falling within the range of 1–1.5 GHz, and the fitting bandwidth exceeds 100 MHz when the peak frequency is below 1.05 GHz or above 1.45 GHz. The orange dots correspond to bursts that do not meet these conditions. (A) The distribution of the center frequency. (B) The scatterplot of the center frequency and spectral width. The white contours show the 2D KDE illustrating the spatial distribution of the center frequency and spectral width. The light yellow and light blue backgrounds indicate the observed (1–1.5 GHz) and effective (0.5 GHz) bandwidths of the FAST telescope, respectively. (C) The spectral width distribution fitted by a lognormal function with a peak value at 181 MHz.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: The Δν/ν 0 distribution of FRB 20220912A. (A) The cumulative distribution function of Δν/ν 0. (B) The differential probability distribution of Δν/ν 0. For both panels, the blue lines and red lines are defined under two filtering criteria, i.e., the Gaussian fit standard deviation error δ σ is smaller than the standard deviation σ itself (blue), and FWHM of the burst spectrum is completely within the range of 1.05–1.45 GHz (red).
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: The proportion of bursts with circular polarization from repeating FRBs varies with RM. The red error bars are given by the Poisson counting error of the statistical counts. The error bar on FRB 20121102A is smaller than the symbol size.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Sixteen bright bursts from FRB 20220912A with circular polarization reversal over time or/and frequency. (A) Polarization position angle (PA). (B) Polarization profiles of the bursts, with the black, red, and blue lines representing the total intensity, linear polarization, and circular polarization, respectively. (C) Stokes I. (D) Stokes V.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Bandwidth fitting examples of the FRB 20220912A bursts.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Four bright bursts from FRB 20220912A with circular polarization oscillating over frequency. (A) Polarization degree. (B) PA.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Two bursts with the highest circular polarization degrees. The black, red, and blue lines respectively represent the burst’s total intensity, linear polarization, and circular polarization profiles.
Paper: FAST Observations of FRB 20220912A: Burst Properties and Polarization Characteristics
Authors: Yong-Kun Zhang, Di Li, Bing Zhang, Shuo Cao, Yi Feng, Wei-Yang Wang, Yuanhong Qu, Jia-Rui Niu, Wei-Wei Zhu, Jin-Lin Han, Peng Jiang, Ke-Jia Lee, Dong-Zi Li, Rui Luo, Chen-Hui Niu, Chao-Wei Tsai, Pei Wang, Fa-Yin Wang, Zi-Wei Wu, Heng Xu, Yuan-Pei Yang, Jun-Shuo Zhang, De-Jiang Zhou, Yu-Hao Zhu
Figure caption: Power-law fitting (red line) to the synthetic spectrum of FRB 20220912A.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Duration and overlap of historical magnetogram instruments and the corresponding flares captured by them. Top: sample magnetograms from each instrument on the given date, as well as the number of M or X flares recorded within a 24 hr window.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Left: breakdown of daily samples by instrument. Right: breakdown of flaring versus nonflaring sample days contained in the data set.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: The CNN+LR architecture, where the dashed black box indicates the CNN alone. A 128 × 128 magnetogram is fed through a series of 2D convolutions (all kernels of size 3 × 3), batch normalization, nonlinear activation, and max pooling. The flattened output is then fed through two dense layers to produce a probability of flaring. When scalar features are included, they are concatenated with this 1 × 1 CNN output and fed through another dense layer to obtain a final flaring probability.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Comparison of metrics evaluated on the holdout set using the probability-calibrated LR models on varying input feature sets. (Left) The BSS, APS, and Gini index are metrics to be maximized with optimal values of 1. (Right) The MSE, ECE, and MCE are metrics to be minimized with optimal values of zero.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Comparison of metrics evaluated on the holdout set using the different probability-calibrated models. (Left) The BSS, APS, and Gini index are metrics to be maximized with optimal values of 1. (Right) The MSE, ECE, and MCE are metrics to be minimized with optimal values of zero.
Paper: Probabilistic Solar Flare Forecasting Using Historical Magnetogram Data
Authors: Kiera van der Sande, Andrés Muñoz-Jaramillo, Subhamoy Chatterjee
Figure caption: Yearly training, validation, holdout, and test splits for the five ensemble members (left), along with the corresponding 24 hr flare climatology distributions and N/P ratios (right). Note that test B is the 2016–2017 data, not depicted on the yearly split.