adsabs/AstroCLIMB huggingface dataset:
Paper: Intense Hard X-Ray Emissions in C-class Flares: A Statistical Study with ASO-S/HXI Data
Authors: Changxue Chen, Yang Su, Wei Chen, Jingwei Li, Fu Yu, Weiqun Gan
Figure caption: Distribution and correlation of flare parameters. (a) The spatial distribution of energetic C-class flares (ECFs), where larger scatter points represent larger SXR fluxes, and the color of the scatter points closer to red represents larger HXR count rate. (b) The heliocentric angle distribution of ECFs, which is obtained by transforming the coordinates in panel (a). (c) Statistical distribution of 30–50 keV count rate with ECFs. (d) Distribution of SXR 1–8 Å flux, where dark yellow and blue represent the results of ECFs and normal C-class flares (NCFs), respectively. (e) Distribution of duration derived from 10 to 20 keV. (f) Distribution of rise time derived from 10 to 20 keV and 30 to 50 keV (only in ECFs, shown as red step plots). The cyan dashed line represents the power-law fit for the 30–50 keV data, with the corresponding index indicated. (g) Scaling of duration with flare importance. Color-coded scatter points show NCFs (blue) and ECFs (red), with luminance gradients correlating to rise time (a darker hue means a longer rise time). The correlation between the duration and SXR flux with two types of flares is shown in the legend, and the corresponding regression lines are also overlaid on the scatter plot. (h) Scaling of 10–20 keV flux with flare importance. The luminance gradients of points correlate to durations, with darker hues representing longer durations. (i) Scaling of 30–50 keV flux with flare importance. The luminance gradients of points correlate to durations, with darker hues representing longer durations.
Paper: Intense Hard X-Ray Emissions in C-class Flares: A Statistical Study with ASO-S/HXI Data
Authors: Changxue Chen, Yang Su, Wei Chen, Jingwei Li, Fu Yu, Weiqun Gan
Figure caption: The correlation between energetic C-class flares (ECFs) and other phenomena. (a) The proportion of ECFs and normal C-class flares (NCFs) in C-class flares. (b) Correlation between ECFs and CMEs, jets, and type III bursts. The presence or absence of relevant phenomena is indicated in blue and gray, respectively, and their quantities are marked accordingly. The pie chart represents the intersection of various phenomena from the outside to the inside, with different color depths. For example, a dark blue color in the center of the chart indicates that five CMEs occur simultaneously with both jets and type III bursts. (c) Correlation between jets, type III bursts, and 360 nm brightening in ECFs. (d)–(f) The statistical distribution between the duration, temperature, and nonthermal electron power-law index corresponding to ECFs with and without an open magnetic field. The purple and gold bars indicate the presence and absence of an open magnetic field, respectively.
Paper: Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection
Authors: Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou, Surui Yao
Figure caption: The AIA 304 Å images illustrate the splitting of the filament and several small jets observed during the splitting process. The white box in panel (a) represents the field of view shown in panels (b)–(e), while the dashed line indicates the path used for the time–distance plot in panel (f). Panels (b)–(e) highlight some small jets observed during the splitting process, labeled as S1–S6. In panel (e), the dashed lines indicate the movement of brightened plasma blobs perpendicular to the filament axis. In panel (f), the black dashed lines show the bidirectional flow of plasma along the filament toward both footpoints, while the white dashed line indicates the structure as observed at 00:08 UT.
Paper: Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection
Authors: Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou, Surui Yao
Figure caption: Panels (a) and (b) display the time–distance diagrams derived from the AIA 304 Å and STEREO-B 195 Å images. The dashed lines trace the movement of the upper branch. Panel (c) displays the time–distance plot, which was used to track the kinematic evolution of the erupting cavity.
Paper: Intense Hard X-Ray Emissions in C-class Flares: A Statistical Study with ASO-S/HXI Data
Authors: Changxue Chen, Yang Su, Wei Chen, Jingwei Li, Fu Yu, Weiqun Gan
Figure caption: The morphology of different types of flares. The top panel (a) displays four cases of flares without accompanying CMEs, each representing a distinct category (types A, B, C, and D). The specific characteristics of each category are detailed in the main text. The middle panel (b) presents all five cases of flares associated with CMEs. The background images in panels (a) and (b) are both AIA 131 Å images, while ​the contours in red, cyan, and purple represent 75%, 30%, and 15% of the peak intensity in the HXI 20–40 keV image, respectively.​​​​​ The orange contour indicates the 10% maximum intensity in the AIA 1600 Å  image, with the centroid corresponding to the flare ribbons marked with a black plus sign. The bottom panel (c) corresponds to panel (b) and shows the CME observation from LASCO C2. The two dashed lines roughly indicate the ejection direction of the CME.
Paper: Intense Hard X-Ray Emissions in C-class Flares: A Statistical Study with ASO-S/HXI Data
Authors: Changxue Chen, Yang Su, Wei Chen, Jingwei Li, Fu Yu, Weiqun Gan
Figure caption: The distribution and correlation of spectral fitting parameters. (a)–(f) The statistical distributions of emission measure (EM), temperature (T), flux of 50 keV nonthermal electrons (F50), nonthermal electron power-law index (δ), low-energy cutoff (Ec), and nonthermal electron energy flux (Fnth), with the corresponding mean and median values given in the legends. (g)–(i) The scaling of F50, δ and Fnth with SXR flux. Their correlations are given in the legend, and the corresponding regression lines are also overlaid on the scatter plot.
Paper: Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection
Authors: Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou, Surui Yao
Figure caption: Results of the FLCT velocity field calculation. Panels (a) and (b) display an overview of the position for both footpoints. The black dashed boxes represent the fields of view for panels (c)–(f) and (g) and (h), respectively. Panels (c) and (d) show the location of the eastern footpoint, with circles indicating several brightening flows directed toward it. Combined with panels (e) and (f), these reveal that the eastern footpoint is situated within a strong positive-polarity network cell, and its corresponding velocity field is displayed in panels (e) and (f). Panel (g) shows the position of the western footpoint, where circles on the right highlight significant brightening flows converging toward it, while circles on the left indicate a portion of the flow entering the sunspot. Combined with panel (h), this suggests that the western footpoint roots in a negative-polarity network cell located west of the sunspot. The velocity field associated with the western footpoint is presented in panel (h), clearly exhibiting a vortex motion, the magnified views of which are shown in panels (i) and (j).
Paper: Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection
Authors: Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou, Surui Yao
Figure caption: The dashed line in panel (a) indicates the orientation of the PIL, along which the decay index was calculated. Panel (b) presents the decay index values, averaged along the section of the PIL shown in panel (a), derived from the extrapolated magnetic field at 23:24 UT on August 29.
Paper: Tides Tighten the Hycean Habitable Zone
Authors: Joseph R. Livesey, Juliette Becker, Susanna L. Widicus Weaver
Figure caption:  ﹩{\dot{E}}_{\,\rm{tide}\,}﹩ as a function of semimajor axis and eccentricity for a hycean, synchronously rotating planet with k2 = 0.3, Q = 2, mp = 7 M⊕, and Rp = 1.7 R⊕ orbiting a 0.12 M⊙ star. The contours correspond to the total tidal heating of Io due to Jupiter (∼1015 W) and that of Earth due to the Moon (∼1012 W).
Paper: Tides Tighten the Hycean Habitable Zone
Authors: Joseph R. Livesey, Juliette Becker, Susanna L. Widicus Weaver
Figure caption: The HHZ (blue shaded regions) and dark HHZ (red shaded regions) around a 0.12 M⊙ star for a 7 M⊕, 1.7 R⊕ hycean planet with tidal quality factor Q = 2. The low-opacity contours show the HZ locations without tidal heating (cf. N. Madhusudhan et al. 2021), and the high-opacity contours show the HZ location for our model where tidal heating is included. The dotted and dashed lines denote the optimistic and conservative HZ limits, respectively, for Earth-like planets according to the model of R. K. Kopparapu et al. (2013). The conservative HZ is bounded by their “Recent Venus” and “Early Mars” cases, while the optimistic HZ is bounded by their “Runaway Greenhouse” and “Maximum Greenhouse” cases.
Paper: Candidate Spectral Lines at 6 and 15 MeV from GRB 200829A and GRB 160905A
Authors: Tong-Lei Liao, Shuo Xiao, Shao-Lin Xiong, Yan-Qiu Zhang, Wang-Chen Xue, Jiao-Jiao Yang, Zheng-Huo Jiang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Figure caption: Light curve of the prompt emission and temporal evolution of GS parameters, where the left and right figures represent GRB 160905A and GRB 200829A, respectively. The top panels represent the light curve, where the blue area is the analysis interval T90 and the purple area is the source analysis interval determined by BB algorithm; the second and third panels represent the line central energy and width, respectively; the bottom panel shows the flux evolution of the GS.
Paper: Tides Tighten the Hycean Habitable Zone
Authors: Joseph R. Livesey, Juliette Becker, Susanna L. Widicus Weaver
Figure caption: The rms forced eccentricity erms for a planet with zero free eccentricity and accompanied by an outer companion in the secular formulation. Note that erms does not depend upon the mass of the inner planet in this simple model.
Paper: Tides Tighten the Hycean Habitable Zone
Authors: Joseph R. Livesey, Juliette Becker, Susanna L. Widicus Weaver
Figure caption: Similarly to Figure 2, the HHZ and dark HHZ around stars of various mass for a 7 M⊕, 1.7 R⊕ hycean planet with tidal quality factor Q = 2. Here we use an orbital eccentricity e = 0.1 throughout: about the value for the hycean candidate planet K2-18 b, whose location in this parameter space is indicated by the blue dot. The dashed line at 0.12 M⊙ points out the stellar mass used in Section 2 and Figure 2. Clearly, the effect of tides on the extent of the HZ becomes negligible at high stellar masses.
Paper: Candidate Spectral Lines at 6 and 15 MeV from GRB 200829A and GRB 160905A
Authors: Tong-Lei Liao, Shuo Xiao, Shao-Lin Xiong, Yan-Qiu Zhang, Wang-Chen Xue, Jiao-Jiao Yang, Zheng-Huo Jiang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Figure caption: The left plot (GRB 160905A) and the right plot (GRB 200829A) present the results of simulations used to assess the significance of the Gaussian lines. The red and blue lines represent the simulation results and the χ2 distribution with 3 degrees of freedom, respectively. The black dashed line indicates the ΔPGstat from the observed data.
Paper: Candidate Spectral Lines at 6 and 15 MeV from GRB 200829A and GRB 160905A
Authors: Tong-Lei Liao, Shuo Xiao, Shao-Lin Xiong, Yan-Qiu Zhang, Wang-Chen Xue, Jiao-Jiao Yang, Zheng-Huo Jiang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Figure caption: Time-integrated spectrum of GRB 160905 in the T90 time interval. The left panel shows the fitting results of the optimal continuum spectral model SBPL. The right panel shows the fitting results with the additional GS, with the line central energy Eμ = ﹩14991.4{6}_{-520.19}^{+538.34}﹩ keV, line width Eσ = ﹩1231.0{6}_{-483.60}^{+644.38}﹩ keV, and the ΔAICSBPL - SBPL+GS = 17.0.
Paper: Candidate Spectral Lines at 6 and 15 MeV from GRB 200829A and GRB 160905A
Authors: Tong-Lei Liao, Shuo Xiao, Shao-Lin Xiong, Yan-Qiu Zhang, Wang-Chen Xue, Jiao-Jiao Yang, Zheng-Huo Jiang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Figure caption: Similar to Figure 2 but for GRB 200829A. The central energy Eμ = ﹩5876.6{8}_{-1358.79}^{+858.10}﹩ keV, width Eσ = ﹩2430.1{4}_{-845.28}^{+534.13}﹩ keV, and the ΔAIC2SBPL - 2SBPL+GS = 20.6.
Paper: Candidate Spectral Lines at 6 and 15 MeV from GRB 200829A and GRB 160905A
Authors: Tong-Lei Liao, Shuo Xiao, Shao-Lin Xiong, Yan-Qiu Zhang, Wang-Chen Xue, Jiao-Jiao Yang, Zheng-Huo Jiang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang
Figure caption: The left and right panels show the light curves in the energy range of best-fit line central energy plus or minus the 2σ line width of GRB 160905A and GRB 200829A, respectively.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: A nonlinear simulation of the solar interior shows the Lamb-like wave among the standing waves. The simulation results demonstrate that f-modes propagate within the Sun, driven by convective excitation, even at low values of ℓ. (A) A snapshot of horizontal velocities, with values normalized at each radius by their rms. (B) The power spectrum of the horizontal velocity in the radiative zone displays peaks corresponding to normal modes. Red, blue, and green symbols indicate the numerically computed frequencies for linear standing p-modes, f-modes, and g-modes, respectively. The frequencies of the normal modes show excellent agreement with linear theory. At the surface and in observations, the power spectrum is noisier due to convection and granulation. (C) When a normal mode frequency is selected, the radial profile of the horizontal displacement from the simulation (solid line) aligns perfectly with the numerically computed linear eigenfunction of the corresponding mode (dotted line). Displayed here are the profiles for a mixed f/g-mode (blue) and three pure f-modes (yellow, orange, and red). The corresponding modes are marked by matching-colored boxes in the power spectrum in panel (B).
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Normal linear adiabatic modes of oscillations. (A) Model and (B) frequencies of a fictitious star with Sdeformed(r) = 10 S⊙(r). The spectrum show that the low-ℓ part of the f-branch consists of bulk modes localized where S = 0. The radial ξr and horizontal ξh displacements are represented by dotted and solid lines, respectively. (C) Model and (D) frequencies of the modes of our solar model for the first two hundred of harmonic degree ℓ. Linear theory predicts frequencies matching observed modes (colored symbols indicate data from T. Larson & J. Schou 2008; R. Kiefer & A.-M. Broomhall 2021). Lamb-like modes are difficult to identify when the f-branch penetrates the g-band.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Identification of mixed f/g-modes in the solar spectrum. The ℓ = 4 Lamb-like wave couples with the g5-mode to form a mixed mode. (A) The average position 〈r〉 of the g-modes defined in the main text is close to the maximum of the buoyancy frequency N2, except for two: they result from the coupling of the f-mode and the g5-mode, which thus have more amplitude in the outer layers. (B) The period spacing ΔP = Pn+1 − Pn shows a dip at the fifth g-mode. (C) The kernel K of the f/g5 mixed mode, in dark blue, shows significant amplitude in the solar core (r/R⊙ < 0.2), implying a significant sensitivity to the core rotation rate. Dark crosses are data points for Ω from M. J. Thompson et al. (2003) obtained observationally. (D) Representation of the horizontal displacement ξh of the mixed mode at frequency 265 μHz in the Sun (red for positive, blue for negative, linear scale). It has amplitude at the surface, as well as in the deep interior.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Displacements of the Lamb-like wave for increasing values of S(r). (A) Three deformed profiles of S(r). (B) Displacements of the n = 0, ℓ = 4 modes for the three profiles. As the values of S increase, the wave becomes more localized around the point where S cancels (black dashed line). The horizontal displacement is also larger, consistent with the analysis of A. Leclerc et al. (2022).
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Effective potential of Equation (E1) for the p- and f-modes in the high-frequency limit. In the case ℓ = 6, the minimum of the potential in the Sun is at the surface. In the fictitious star discussed in the main text for which S(r) = 10 S⊙(r), the minimum is located inside the bulk of the star, where the f-mode is much more closely described by a Lamb-like mode.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Evolution of the total kinetic energy in the simulation over time. The convective instability begins to develop around 2 × 105 s and then saturates as the convective layer fully develops. The simulation reaches a dynamical steady state once the plateau in kinetic energy is reached, around 3 × 106 s. The wave analysis is performed after that time.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Modes of different types are located in different regions of the Sun. Red and blue are regions of positive and negative horizontal displacement ξh. (A) is the n = 1, ℓ = 4 p-mode, (B) is the n = 35, ℓ = 4 g-mode, (C) is the ℓ = 10 f-mode, and (D) is the mixed f/g5-mode discussed in the main text.
Paper: A Core-sensitive Mixed f/g-mode of the Sun Predicted by Wave Topology and Hydrodynamical Simulation
Authors: Arthur Le Saux, Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille
Figure caption: Amplitude of standing modes. To estimate the surface amplitude of a mode, we compute its linear eigenfunction (dashed red lines) and fix its amplitude at r = 0.6 Rstar with the one measured in the MUSIC simulations (blue lines). We can then extrapolate the amplitude of the mode at r = Rstar.
Paper: The Double Tidal Disruption Event AT 2022dbl Implies that at Least Some “Standard” Optical Tidal Disruption Events Are Partial Disruptions
Authors: Lydia Makrygianni, Iair Arcavi, Megan Newsome, Ananya Bandopadhyay, Eric R. Coughlin, Itai Linial, Brenna Mockler, Eliot Quataert, Chris Nixon, Benjamin Godson, Miika Pursiainen, Giorgos Leloudas, K. Decker French, Adi Zitrin, Sara Faris, Marco C. Lam, Assaf Horesh, Itai Sfaradi, Michael Fausnaugh, Ehud Nakar, Kendall Ackley, Moira Andrews, Panos Charalampopoulos, Benjamin D. R. Davies, Yael Dgany, Martin J. Dyer, Joseph Farah, Rob Fender, David A. Green, D. Andrew Howell, Thomas Killestein, Niilo Koivisto, Joseph Lyman, Curtis McCully, Morgan A. Mitchell, Estefania Padilla Gonzalez, Lauren Rhodes, Anwesha Sahu, Giacomo Terreran, Ben Warwick
Figure caption: Our full spectral series of AT 2022dbl together with the host-galaxy spectrum from SDSS. Lines that characterize various subtypes of optical-ultraviolet TDEs are marked. Phases are noted in days relative to the peak luminosity of the first flare.
Paper: The Double Tidal Disruption Event AT 2022dbl Implies that at Least Some “Standard” Optical Tidal Disruption Events Are Partial Disruptions
Authors: Lydia Makrygianni, Iair Arcavi, Megan Newsome, Ananya Bandopadhyay, Eric R. Coughlin, Itai Linial, Brenna Mockler, Eliot Quataert, Chris Nixon, Benjamin Godson, Miika Pursiainen, Giorgos Leloudas, K. Decker French, Adi Zitrin, Sara Faris, Marco C. Lam, Assaf Horesh, Itai Sfaradi, Michael Fausnaugh, Ehud Nakar, Kendall Ackley, Moira Andrews, Panos Charalampopoulos, Benjamin D. R. Davies, Yael Dgany, Martin J. Dyer, Joseph Farah, Rob Fender, David A. Green, D. Andrew Howell, Thomas Killestein, Niilo Koivisto, Joseph Lyman, Curtis McCully, Morgan A. Mitchell, Estefania Padilla Gonzalez, Lauren Rhodes, Anwesha Sahu, Giacomo Terreran, Ben Warwick
Figure caption: Optical and ultraviolet host-subtracted light curves of AT 2022dbl normalized to each peak time and shifted in magnitude for clarity (both flares are shifted by the same amount per band; top). Both flares are very similar to each other in the optical bands and show some differences in the ultraviolet. No earlier flares were detected in the ∼1500 days preceding the first flare (bottom). Error bars denote 1σ uncertainties, and triangles denote 3σ nondetection upper limits.
Paper: The Double Tidal Disruption Event AT 2022dbl Implies that at Least Some “Standard” Optical Tidal Disruption Events Are Partial Disruptions
Authors: Lydia Makrygianni, Iair Arcavi, Megan Newsome, Ananya Bandopadhyay, Eric R. Coughlin, Itai Linial, Brenna Mockler, Eliot Quataert, Chris Nixon, Benjamin Godson, Miika Pursiainen, Giorgos Leloudas, K. Decker French, Adi Zitrin, Sara Faris, Marco C. Lam, Assaf Horesh, Itai Sfaradi, Michael Fausnaugh, Ehud Nakar, Kendall Ackley, Moira Andrews, Panos Charalampopoulos, Benjamin D. R. Davies, Yael Dgany, Martin J. Dyer, Joseph Farah, Rob Fender, David A. Green, D. Andrew Howell, Thomas Killestein, Niilo Koivisto, Joseph Lyman, Curtis McCully, Morgan A. Mitchell, Estefania Padilla Gonzalez, Lauren Rhodes, Anwesha Sahu, Giacomo Terreran, Ben Warwick
Figure caption: Mass fallback rates (left axes) are shown for the first, second, and third pericenter passages of a 3 M⊙ terminal-age main-sequence (TAMS) star on a bound orbit around a 106 M⊙ black hole having a pericenter distance of Rp ∼ Rt with eccentricity e = 0.995, consistent with an orbital period of ∼700 days (top), and for the first and second pericenter passages of a 1 M⊙ zero-age main-sequence (ZAMS) star having a pericenter distance Rp ∼ Rt/1.4 with an orbital eccentricity e = 0.997, consistent with the same orbital period (bottom). In the latter case, the star is fully disrupted on the second passage. The bolometric luminosities of the two flares (right axes) are overlaid with different efficiency parameters ϵ in each case to match the mass fallback rate, assuming the luminosity is entirely powered by mass fallback with a constant efficiency. The late-time bump in the 1 M⊙ first passage mass fallback rate is due to the less-bound debris returning after one orbital period and is much smaller than the fallback rate due to the bound debris from the second passage. The current data are not able to distinguish between these two types of scenarios. This could be determined by the existence of a third flare. Error bars denote 1σ uncertainties.