adsabs/AstroCLIMB huggingface dataset:
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Left panel: the upper subplot shows the mass recovery ratio as a function of the multiplicity N SC of the ground-truth superclusters. Each gray point represents a ground-truth supercluster in our six simulation boxes. The red curve shows the median as a function of N SC. The fraction of ground-truth superclusters that are not detected f missed is shown in the lower right corner. The lower subplot shows a 2D histogram between the detected multiplicity and the ground-truth multiplicity. Normalization is set such that each column sums up to unity. Right panel: same as left panel, but at redshift z = 0.50.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: The confirmed count, purity, and completeness as a function of hyperparameters ﹩({\rm{\Delta }}z,{w}_{\mathrm{thres}},{N}_{\min })﹩ for the  DEmP  examination described in Section 2.3. Top row: the confirmed count of CAMIRA clusters as a function of the minimum member N min. Curves of different colors represent different membership probability thresholds w thres adopted. Middle row: same as the top row, but for the purity defined in Table 7. Bottom row: same as the top row, but for the completeness defined in Table 7. The size of redshift interval Δz = 0.01 and Δz = 0.02 are used for the left and right columns, respectively.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Supercluster total mass M tot distribution in the unperturbed mock catalog (left column) and perturbed mock catalog (right column). The top and bottom rows show distributions at redshift z = 0.9 and z = 0.6, respectively. In each panel, the gray histogram shows the M tot distribution of the ground-truth superclusters. The red dashed histogram and blue dotted histogram are M tot distributions obtained by the mass-weighted linking length and the unweighted linking length, respectively.
Paper: Formation of Jupiter-mass Binary Objects through Photoerosion of Fragmenting Cores
Authors: Jessica L. Diamond, Richard J. Parker
Figure caption: Separation distribution of the JuMBOs (the black histogram). For comparison, we show the Gaussian fits to the separation distributions of various stellar and substellar binary populations. The fit to the brown dwarf–brown dwarf binaries (A. J. Burgasser et al. 2007; I. Thies & P. Kroupa 2007) is shown by the dotted–dashed orange line, the fit to the M-dwarf binaries (C. Bergfors et al. 2010; M. Janson et al. 2012) is shown by the dashed blue line, the fit to the G-dwarf (solar-type) binaries (D. Raghavan et al. 2010) is shown by the solid red line, and the fit to the A-type binaries (R. J. De Rosa et al. 2014) is shown by the dotted green line.
Paper: Formation of Jupiter-mass Binary Objects through Photoerosion of Fragmenting Cores
Authors: Jessica L. Diamond, Richard J. Parker
Figure caption: Radii of H II regions around six massive stars in the ONC, as well as the H II region driven by the combined flux of three massive stars within the Trapezium system (the black circles). The locations of the observed JuMBOs are shown by the black crosses. The two panels show the sizes of the H II regions for different assumed densities of hydrogen nuclei. Panel (a) shows the HII  regions for the lower density (﹩{n}_{0}={10}^{3}{{\rm{cm}}}^{-3}﹩), and panel (b) shows the HII regions for the higher density (﹩{n}_{0}={10}^{4}{\rm{c}}{{\rm{m}}}^{-3}﹩).
Paper: Formation of Jupiter-mass Binary Objects through Photoerosion of Fragmenting Cores
Authors: Jessica L. Diamond, Richard J. Parker
Figure caption: Histograms of the initial core mass distributions (open histograms), the masses, M 3, of the final objects following photoerosion of the cores (pink histograms), and the observed JuMBO masses (black histograms). We show the distributions for the two different hydrogen densities. Panel (a) shows the results for lower hydrogen densities (﹩{n}_{0}={10}^{3}{\rm{c}}{{\rm{m}}}^{-3}﹩), and panel (b) shows the results for higher hydrogen densities (﹩{n}_{0}={10}^{4}{\rm{c}}{{\rm{m}}}^{-3}﹩).
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: Mass accretion phenomenon has been demonstrated throughout the evolution epoch. The top panel denotes the possible candidates for the evolving protostars that may escape the cloud (denoted in red), merge with others (denoted in blue), and roam around within the cloud (denoted in green), respectively. The middle panel represents that the maximum accretion rate approaches a value ≈10−2–10−3 M ⊙ yr−1 for the protostars staying inside. This is consistent with existing results from simulations (see e.g., T. Abel et al. 2002; T. H. Greif et al. 2011; J. Dutta 2016a; M. A. Latif et al. 2022). The black-dashed line stands for the total accretion rate by all the protostars. The bottom panel shows the variation in the mass evolution in which we observe both low (≲2 M ⊙) and high mass (in the range of ≈6–75 M ⊙) protostars in our simulation. The high-mass protostars generally correspond to the ones that stay within and keep on accreting mass. The notation M tot, represented by the black-dashed line, manifests the total mass in protostars.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: Top panel demonstrates the variation of the angular velocity with the number density of the cloud, shown by the brown line. We fit this variation (black-dashed line) with a power-law characteristic (Ω ∼ n 0.5). The purple line represents the variation of the same as a function of the total enclosed mass that comprises both gas and protostars. In the middle panel, the escape velocity (v esc) has been numerically calculated (represented by the black line), which corresponds to the logarithmic fit (﹩{v}_{\mathrm{esc}}\approx 13.66-1.998\mathrm{log}[r/\mathrm{au}]﹩) denoted by the purple line. We observe a deviation within the very central regime. Hence, the fit corresponds to the escape velocity at a radial distance r ≳ 30 au. The bottom panel shows the distribution of the initial radial distance (purple markers) and three components of the velocity v  r , v  ϕ , v  z  (brown markers) corresponding to the initial mass of the protostars.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: Mass and radial distance of the four protostars that are left over (out of the 10 at the beginning of our simulation) as a consequence of the merger events, are plotted at the end of our simulation. The scatter diagram shows that three protostars are likely to move away (denoted by red marker) from the potential well of the cloud. It is to be noted that the ejected protostars accommodate two low-mass protostars (M p2 ≈ 0.35 M ⊙ and M p5 ≈ 0.72 M ⊙) and another protostar with a slightly higher mass (M p9 ≈ 1.44 M ⊙), respectively. These low-mass protostars may possibly go through the ZAMS phase, and hence remain as the probable candidates to survive for a longer period of time. The other one (denoted by green markers) seems to remain inside the cloud as a high-mass protostar.
Paper: Formation of Jupiter-mass Binary Objects through Photoerosion of Fragmenting Cores
Authors: Jessica L. Diamond, Richard J. Parker
Figure caption: Product of star formation efficiency and core mass, ϵ M  c , against final JuMBO mass, M 3, shown by the purple circles. The primary mass of the binary, m  p , if it had been allowed to form without mass loss due to photoerosion, against final JuMBO mass M 3, is shown by the pink asterisks. The lower and upper limits on the JuMBO masses from S. G. Pearson & M. J. McCaughrean (2023) are shown by the vertical black lines, and the upper limits to the primary masses, m  p , of M-type (blue), G-type (red), and A-type (green) binaries are shown by the horizontal lines. Panel (a) shows the results for lower hydrogen densities (﹩{n}_{0}={10}^{3}{\rm{c}}{{\rm{m}}}^{-3}﹩), and panel (b) shows the results for higher hydrogen densities (﹩{n}_{0}={10}^{4}{\rm{c}}{{\rm{m}}}^{-3}﹩).
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The trajectories of all the protostars in the x − y plane have been visualized in the central regime of ≈1000 au at an epoch t ≈ 20.22 kyr (left-hand panel). The zoomed-in version (i.e., boxsize ≈300 au) on the right-hand panel clearly depicts the dynamics of all the protostars that escape (denoted in red), merge (denoted in blue), and roam around (denoted in green), respectively. The yellow markers represent the four different sites where the merger event took place for the following protostars: the first merger took place at an epoch t ≈ 0.0098 kyr between p6 and p8 protostars, denoted by (p6–p8 pair). The second, third, fourth, fifth, and the sixth took place at t ≈ 8.81 kyr for (p6–p10 pair), t ≈ 9.6 kyr for (p4–p6 pair), t ≈ 19.68 kyr for (p6–p7 pair), t ≈ 146.7 kyr for (p1–p4 pair), and t ≈ 169.3 kyr for (p1–p3 pair), respectively.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The mass function is depicted for three distinct values of the parameter f ≈ 1, 0.5, 0.1, which represents the fraction of the incoming energy radiated away by the protostar, at the end of the simulation. The lower value (i.e., f ≈ 0.1 in bottom panel) corresponds to the existence of only two protostars. This is because the dynamical friction leads to more inward dragging of the protostars, consequently resulting in an increased number of mergers. In contrast, as f approaches higher values (f ≈ 0.5, 1, in the middle and top panels, respectively), we observe a comparatively higher number of protostars in our simulation.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The phase space diagram (r 2 − v  r  plot, where r 2 represents the distance between the pair) demonstrates the development of two binary systems in our simulation. The upper and lower panels markedly illustrate the formation of the first binary pair, denoted by “p4–p6,” and the second binary pair, denoted by “p1–p4,” respectively. The protostar p4 is likely to be merged with its counterpart p6 at t ≈ 9.6 kyr. Later, it forms another binary pair with the protostar p1 at an epoch close to 40 kyr. The second pair also seems to end up merged at t ≈ 146 kyr.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The time evolution of the mass function can be envisaged from four different epochs (t ≈ 0, 9.75 × 102, 1.0 × 105, 9.98 × 105 yr, respectively) from the top to the bottom panel. It is to be noted that the peaks of the mass function gradually migrate toward the higher end of the mass spectrum over time as a consequence of continuous mass accretion. This is expected because there is no formation of new protostars in our model.
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Comparison between the properties of 500 synthetic planetary systems from long-term N-body simulations and our ML-based giant-impact emulator (which is ∼104 faster than full N-body simulations). The masses, spacings, and orbital inclinations of the planets in the ML-predicted systems agree well with those from N-body simulations (top row). System-level properties of the ML-predicted systems also agree with the N-body systems (bottom row), although we find the ML-predicted systems to be somewhat less dynamically excited. The 1D Wasserstein distance ﹩{ \mathcal W }﹩ between the two distributions are reported in each panel. Our ML-based model outperforms a non-ML baseline model, whose predictions agree less well with the true N-body distributions (for the quantities shown in the top-left to the bottom-right panels, ﹩{ \mathcal W }﹩ = 0.281, 0.507, 2.293, 0.038, 0.096, 2.048).
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: The light curve of KIC 8840638 in SC. Top panel: the whole light curve of Q14.2. Middle panel: the zoom-in light curve of Q14.2 with 4.4 days. Bottom panel: the zoom-in light curve of Q14.2 with 1.0 day.
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Schematic of the iterative giant-impact emulator. At each step, instability times for subtrios of planets are predicted using SPOCKII (M. Cranmer et al. 2021). Then, with the ML model presented in this work, we predict the collisional outcome of the planet trio with the shortest instability time, replace the trio with the two new planets, and repeat until SPOCKII identifies the system as long-term stable.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: Amplitude spectra for the rectified SC data of KIC 8840638 up to 80 day−1. (a) A zoom-in amplitude spectrum in the low-frequency region of 0 day−1 < ν < 4 day−1. (b) A zoom-in amplitude spectrum in the high-frequency region of 23 day−1 < ν < 28 day−1; red (blue) dashed lines indicate f 5 (f 7) and combinations with f orb. (c) A zoom-in amplitude spectrum in the high-frequency region of 50 day−1 < ν < 65 day−1.
Paper: Accelerating Giant-impact Simulations with Machine Learning
Authors: Caleb Lammers, Miles Cranmer, Sam Hadden, Shirley Ho, Norman Murray, Daniel Tamayo
Figure caption: Performance of three non-ML baseline classification models on the 200 validation systems, for comparison with our ML model (Figure 2). From top to bottom, the baseline model predictions rely on the mass ratios of the planets, the amount of angular momentum required for the planets’s orbits to cross, and the normalized eccentricity of the planets. The baseline models predict three logits, which are converted to probabilities using a softmax function (see Appendix B). Despite leveraging dynamics-inspired metrics, the predictions of all three baseline models are poor.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: The SED fitting result. Upper panel: cyan points are the observed fluxes, and red diamonds are the synthetic fluxes. The black spectrum is the best-fit SED model, while the green and blue curves are the model spectra of primary and secondary stars, respectively. Lower panel: the residuals of SED fitting. The photometric observations in different bands are sorted in the order of Table 3.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: The marginalized posterior probability distributions of temperatures, radii, and V-band extinction in the SED fitting. The vertical dashed lines are located at the 16th, 50th, and 84th percentiles.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: The folded orbital phase diagram of KIC 8840638 with the detected frequency f 1. One hundred time bins are shown in an orbital phase.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: Evolutionary tracks of KIC 8840638. Blue lines and points represent the primary (gainer) star, while red lines and points represent the secondary (donor) star. Filled circles are located at the positions with the same age (5.59 Gyr) in the theoretical calculations. Panel (1): evolutionary tracks of the two components on the Hertzsprung–Russell diagram. Initiating from the square points, the component stars follow the theoretical evolution trajectory to the filled circles. The stars represent the PHOEBE results, and the error bars are 3 times the corresponding errors. Panel (2): theoretical mass evolution curves of the components over time. The blue straight line represents the expected value of M 1 (see Table 4), with dashed lines above and below indicating the upper and lower errors, respectively, while the red lines correspond to those parameters of M 2. Panel (3): theoretical orbital period evolution curves of the components over time. The black dashed line represents the observed period of KIC 8840638. Panel (4): a zoom-in on the initial moment (gray box in panel (3)) of the orbital period evolution caused by mass transfer.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: Left panel: FT (black), HFD (gray), and AC (blue) functions of the independent peaks lower than 40 day−1 found in this work. The red dotted–dashed line marks the position of Δν = 36.5 ± 0.1 μHz. Right panel: echelle diagram of the frequencies showing a clear ridge around ﹩\nu \,\mathrm{mod}\,{\rm{\Delta }}\nu =4\mu \mathrm{Hz}﹩.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: Model fitting parameters for the binary light curve of KIC 8840638. Corner distributions provide the posterior probabilities of the nine modifiable parameters projected in two dimensions. The vertical dashed lines in one-dimensional distributions indicate the percentiles of 16% (black dashed lines), 50% (red dashed–dotted lines), and 84% (black dashed lines), while the uncertainty displayed above corresponds to the 68th percentile. The mean value (50th percentile) of each parameter is marked with a red dot in the two-dimensional plots.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: Echelle diagram modulo the orbital frequency.
Paper: KIC 8840638: A Newly Discovered Eclipsing Binary with δ Scuti–Type Oscillations
Authors: Tao-Zhi Yang, Zhao-Yu Zuo, Jun-Hui Liu, Deng-Kai Jiang, Zhi-Xiang Zhang, Qin-jie Tang, Antonio García Hernández
Figure caption: The normalized and phase-folded light curve of KIC 8840638 with the PHOEBE model fitting result. The corresponding residuals are plotted in the lower panel.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The lensing bands of the KN BH are shown under several representative BH parameters and observation angles. Top panel: BH spin is set to a = 0.8 and charge to Q = 0.3. Bottom panel: the BH spin remains a = 0.8, but the charge is increased to Q = 0.5. From left to right, the observation inclination angles are set to 17 deg, 75 deg, and 150 deg. The dark gray and light gray regions represent light rays that intersect the null geodesic and the equatorial plane of the BH once and twice, respectively. The critical curve is depicted as a white line, and the innermost region corresponds to the “inner shadow” of a KN BH. The mass of BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The direct (blue lines) and secondary (red lines) orbits of the KN BH are shown under several representative BH parameters and observation inclination angles. The mass of the BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: Inner shadow of the KN BH under several representative observation inclination angles. Left panel: observation angle θ 0 = 17 deg. Middle panel: observation angle θ 0 = 75 deg. Right panel: Observation angle θ 0 = 150 deg. The mass of the BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: Ray trajectories around KN BHs on the (α, β) plane. Set the mass of the BH to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The shadow of the KN BH under several representative BH parameters using the numerical ray-tracing method. Left panel: BH spin a = 0.8 and charge Q = 0.3. Middle panel: BH spin a = 0.8 and charge Q = 0.5. Right panel: BH spin a = 0.94 and charge Q = 0.3. The mass of the BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption:                       ﹩\tilde{r}﹩ is depicted as a function of ﹩\tilde{\eta }﹩. The intersection points of the solid lines with the x-axis represent the positions of the roots. The solid blue line corresponds to Q = 0.3, while the solid red line indicates Q = 0.5. The dashed line shows the location of the event horizon. The mass of the KN BH is set to M = 1, and the spin is a = 0.8.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: Fisheye camera field of view with m × m pixels.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The effective potential function of the KN BH is determined by setting the BH’s mass to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: Inner shadow of the KN BH with the BH mass set to M = 1.