adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Posterior distribution of the apparent isotropic luminosity for the isotropic model. The solid and dashed vertical lines are the 90th and 50th percentiles of the distribution, respectively.
Paper: Large-scale Linear Magnetic Holes with Magnetic Mirror Properties in Hybrid Simulations of Solar Wind Turbulence
Authors: Giuseppe Arrò, Francesco Califano, Francesco Pucci, Tomas Karlsson, Hui Li
Figure caption: Magnetic field magnitude at ﹩t=543.5\,{{\rm{\Omega }}}_{i}^{-1}﹩ (a) with a zoom into an MH (b); magnetic field components and mirror threshold Γ (c), ion density, ion temperature components, and B 2/2 + P  i  ,⊥ (d) over the red dashed line in panel (b); 3D isosurfaces of f  i  (e) and δ f  i  (f) at the red dot in panel (b) with local magnetic field (red arrow) and loss cone (green surface); magnetic field magnitude (g) and Θ (h) distributions in the (T  i,⊥/T  i,∥ − 1, β  i,⊥) plane with the mirror threshold (black dashed line). The magnetic field, density, temperature, and B 2/2 + P  i,⊥ are in units of B 0, n 0, T 0, and ﹩{B}_{0}^{2}/2+{n}_{0}\,{T}_{0}﹩, respectively.
Paper: Large-scale Linear Magnetic Holes with Magnetic Mirror Properties in Hybrid Simulations of Solar Wind Turbulence
Authors: Giuseppe Arrò, Francesco Califano, Francesco Pucci, Tomas Karlsson, Hui Li
Figure caption: Magnetic field magnitude (in units of B 0; (a)–(d)), mirror threshold Γ ((e)–(h)), and Θ ((i)–(l)) at different times, showing the MH formation (with isolines indicating the in-plane magnetic field). Each column corresponds to a different time, given in the column title.
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: Particle distribution and magnetic fields upstream of the shock at t = 65 (Θ Bn  = 50°). From the top, V  x  − x phase-space distributions of (a) PUIs, (b) SWIs, (c) electrons; magnetic field components of (d) B  x , (e) B  y , (f) B  z ; and velocity distributions of PUIs at (g) x = 200, (h) x = 300, and (i) x = 400. In panels (a)–(c) and (g)–(i), only the particles at y ≈ L  y /2 are counted. The color bars in panels (a)–(c) denote phase-space density (in an arbitrary unit). The color bar in panels (g)–(i) denotes velocity space density (in an arbitrary unit). The dashed lines in panels (g)–(i) represent the direction of local (upstream) magnetic field, B 0.
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: Structure of a PUI-mediated oblique shock at t = 125 (Θ Bn  = 50°). From the top, the first three panels denote magnetic field B  x , B  y , B  z ; the next three denote electric field E  x , E  y , E  z ; and the last three indicate density of PUIs (N PUI), SWIs (N SWI), and electrons (N  e ).
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: (a) Energy distributions of downstream PUIs at various shock angles and times. Each distribution (solid line) is divided into the two dashed lines indicating SWIs (lower energy) and PUIs (higher energy). Energy history of an accelerated PUI is shown by the rainbow colored lines as a function of (b) space and (c) time. The line color denotes time.
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: Electrostatic potential for Θ Bn  = 50° (black) and Θ Bn  = 70° (gray) at t = 50 along y ≈ 27. The gray line is shifted horizontally in x to align the overshoot position with that of the black line.
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: Linear dispersion relation of oblique resonant instability driven by BS-PUIs.
Paper: Injection Process of Pickup Ion Acceleration at an Oblique Heliospheric Termination Shock
Authors: Shuichi Matsukiyo, Yosuke Matsumoto
Figure caption: Linear dispersion relation of oblique resonant instability driven by BS-PUIs with different background ion beta, β  i . The solid and dashed lines indicate real and imaginary parts of frequency, respectively.
Paper: Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Authors: Xiao-Jin Xie, Jianrong Shi, Hong-Liang Yan, Tian-Yi Chen, Carlos Allende Prieto, Timothy C. Beers, Shuai Liu, Chun-Qian Li, Ming-Yi Ding, Yao-Jia Tang, Ruizhi Zhang, Renjing Xie
Figure caption: Comparison of abundance ratios in J0206+4941 (red star) with MW field stars (gray circles). The abundance ratios of the MW stars come from Venn et al. (2004), Bensby et al. (2014), Battistini & Bensby (2016), Forsberg et al. (2019), and Holmbeck et al. (2020). The black dashed line is the solar reference line. The orange dashed line in the [Eu/Fe] vs. [Fe/H] panel indicates the r-II limit (+0.7) as defined by Holmbeck et al. (2020).
Paper: Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Authors: Xiao-Jin Xie, Jianrong Shi, Hong-Liang Yan, Tian-Yi Chen, Carlos Allende Prieto, Timothy C. Beers, Shuai Liu, Chun-Qian Li, Ming-Yi Ding, Yao-Jia Tang, Ruizhi Zhang, Renjing Xie
Figure caption: Spectral synthesis for the abundance determinations of Sr, Ba, La, Ce, Eu, and Th. The red line indicates the best-fit synthesis for the line(s) of interest. The blue shaded regions indicate ±0.30 dex deviations from the best fit. The gray dashed lines indicate synthetic spectra in the absence of the element of interest.
Paper: Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Authors: Xiao-Jin Xie, Jianrong Shi, Hong-Liang Yan, Tian-Yi Chen, Carlos Allende Prieto, Timothy C. Beers, Shuai Liu, Chun-Qian Li, Ming-Yi Ding, Yao-Jia Tang, Ruizhi Zhang, Renjing Xie
Figure caption: The heavy-element abundances of J0206+4941 are shown in the top panel, with the solar r-process pattern, abundances of HD 222925 (Roederer et al. 2022b), and 2MASS J22132050-5137385 (Roederer et al. 2024) normalized to match the Eu abundance of J0206+4941. Residuals between J0206+4941 and the solar r-process pattern, HD 222925, and 2MASS J22132050-5137385 are shown in the lower panels.
Paper: Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Authors: Xiao-Jin Xie, Jianrong Shi, Hong-Liang Yan, Tian-Yi Chen, Carlos Allende Prieto, Timothy C. Beers, Shuai Liu, Chun-Qian Li, Ming-Yi Ding, Yao-Jia Tang, Ruizhi Zhang, Renjing Xie
Figure caption: Comparison of high-resolution spectra of J0206+4941 and a moderately RPE (r-I) star, HD 124897 ([Eu/Fe] = +0.45; Forsberg et al. 2019) with similar stellar parameters. The lines of heavy elements are labeled in red, and lines of lighter elements are labeled in black. The stellar parameters (T eff, log g, [Fe/H], ξ) are shown in the legend.
Paper: Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Authors: Xiao-Jin Xie, Jianrong Shi, Hong-Liang Yan, Tian-Yi Chen, Carlos Allende Prieto, Timothy C. Beers, Shuai Liu, Chun-Qian Li, Ming-Yi Ding, Yao-Jia Tang, Ruizhi Zhang, Renjing Xie
Figure caption: Toomre diagram for J0206+4941. The MW thin-disk stars (pink triangles) and thick-disk stars (blue circles) are from Bensby et al. (2003) and Venn et al. (2004), respectively.
Paper: Enhanced Efficiency of Solar Wind Electron Interaction with Whistlers Caused by Switchback-related Magnetic Dips
Authors: Tien Vo, Oleksiy V. Agapitov, Kyung-Eun Choi, Cynthia A. Cattell, Jack Redepenning, Lucas Colomban
Figure caption: Transition from QL diffusion to nonlinear energization and scattering. (a) 						Average energization and (b) scattering in terms of parallel kinetic energy 							W ∥,0 and wave amplitude 							B  w /B 0. 						The heatmaps are generated by averaging over the perpendicular direction for 						plots such as Figures 2(g)–(h) with 							B  h /B 0 						= 0.3, ω/Ω e  						= 0.1, and different values of 								B  w /B 0. 						The areas bounded by solid and dashed white curves (corresponding to the 						start and end of the wave region discussed in Figure 1(b)) denote the range of resonant energies. 						The crosses on the ordinate of panels (a)–(b) are energies at which 						the diffusion coefficients in panels (c)–(d) are calculated in 						corresponding colors. (c) Normalize momentum and (d) pitch-angle diffusion 						coefficients. In panels (a)–(d), vertical dashed lines are an 						approximated boundary between linear and nonlinear regimes (see Equation 							(2)). (e) 						Illustration of how a resonance island (dotted curves) tends toward lower 						velocities between z = −R and 							z = R (wave region defined in 						Figure 2). The overlap of all 						the islands is a broadened effective island (gray area) of width 							ΔV = 								ΔV  g  + 							ΔV  w . The thick solid 						and dashed curves correspond to similarly formatted curves in panels 						(a)–(b) and Figure 2.
Paper: Enhanced Efficiency of Solar Wind Electron Interaction with Whistlers Caused by Switchback-related Magnetic Dips
Authors: Tien Vo, Oleksiy V. Agapitov, Kyung-Eun Choi, Cynthia A. Cattell, Jack Redepenning, Lucas Colomban
Figure caption: Response of antisunward (ASW) electrons interacting with sunward (SW) 						parallel whistler at a hyperbolic gradient. (a) Background field (arrowed 						lines) and wave profile (colors). The line thickness indicates magnitude. 						(b) Background and wave field profile along x = 0. 						Left axis (black): B 0,z . Right 						axis (red): 							B  w,x . The 						red arrow indicates the propagation direction. The Gaussian envelope is 						centered at z = 0, with one sigma (width) 							σ/R = 0.5. (c) Left axis: 						parallel electron velocity. Right axis: corresponding parallel electron 						energy. The dashed curve denotes resonant velocity/energy. (d) Pitch angle. 						(e) Change in kinetic energy. Vertical solid and dashed lines in panels 						(a)–(e) denote a region containing two sigmas of the wave envelope 						called the “wave region.” (f) Trajectories in velocity space 							(V ∥, 						V ⊥). Initial and final values are marked 						with white and red circles. Dashed gray circular lines are constant-energy 						surfaces in the wave frame. The black arrow indicates the direction of the 						mirror force (see the main text). (g) Energization and (h) scattering in 						terms of initial conditions in velocity space 							(V ∥,0, 							V ⊥,0). Vertical solid and dashed lines 						in panels (f)–(h) are resonant velocities (see panel (c)) at 							z = − R, 							R, corresponding to similarly formatted vertical lines 						in panels (a)–(e). Shaded areas are the trap cone at 							z = R. Note: while panels (f) 						and (g)–(h) share the same abscissa, the former plots instantaneous 						parallel velocity and the latter initial parallel velocity.
Paper: Enhanced Efficiency of Solar Wind Electron Interaction with Whistlers Caused by Switchback-related Magnetic Dips
Authors: Tien Vo, Oleksiy V. Agapitov, Kyung-Eun Choi, Cynthia A. Cattell, Jack Redepenning, Lucas Colomban
Figure caption: PSP observations of whistler waves and solar wind parameters. (a)–(c) 						The magnetic dip near the switchback boundary recorded by PSP on 2018 						November 4, as shown by Agapitov et al. (2020). (a) Magnetic field magnitude (black) 						and components (red: R, green: T, and blue: N) from FIELD/MAG in RTN 						coordinates. (b) Proton velocity components from SWEAP/SPC in the same 						format as panel (a). (c) Total magnetic spectrum from the SCM waveforms. The 						white curve is the lower hybrid frequency f lh. 						(d) The local magnetic field at the trailing interval of panel (a). (e) 						Magnetic and (f) electric field perturbations from waveform data in 						spacecraft XYZ coordinates (black: X, 						blue: Y, and red: Z). (g) Spectrogram of 						panel (e). White curves are 							0.1f  ce  and 							f lh, respectively. (h)–(i) Pitch-angle 						distributions of suprathermal electrons and differential energy fluxes from 						PSP SWEAP/SPE during the time interval (h) T 1 						(red horizontal bar above panel (a)) and (i) T 2 						(gray horizontal bar above panel (a)).
Paper: Enhanced Efficiency of Solar Wind Electron Interaction with Whistlers Caused by Switchback-related Magnetic Dips
Authors: Tien Vo, Oleksiy V. Agapitov, Kyung-Eun Choi, Cynthia A. Cattell, Jack Redepenning, Lucas Colomban
Figure caption: Changes in a realistic electron distribution function after interaction with 						sunward (SW) whistlers at the edge of a Gaussian dip. (a) Example background 						and wave field profiles along x = 0. Left axis 						(black): ∣ B  0∣. Right axis 						(red): B  w,x . 						Black and red arrows indicate, respectively, the background field and wave 						propagation direction. (b)–(c) Initial (dashed black contours) and 						final (colors with black contours) electron distribution functions in a 						field profile such as that in panel (a). In panels (b)–(c), 							B  w /B 0 						= 0.01. In panel (b), 							B  h /B 0 						= 0.3. In panel (c), 							B  h /B 0 						= 0.8. In columns (1), (2), (3), and (4), 								ω/Ω e  = 						0.05, 0.1, 0.15, and 0.2, respectively. The initial distribution is taken 						from Figure 1(i). Solid and 						dashed white curves indicate the wave resonance conditions, in the same 						format as previous figures. Black crosses denote the trap angle.
Paper: Enhanced Efficiency of Solar Wind Electron Interaction with Whistlers Caused by Switchback-related Magnetic Dips
Authors: Tien Vo, Oleksiy V. Agapitov, Kyung-Eun Choi, Cynthia A. Cattell, Jack Redepenning, Lucas Colomban
Figure caption: Transition from uniform to inhomogeneous background field. In the same format 						as Figure 3, average (a) 						energization and (b) scattering in terms of parallel kinetic energy 							W ∥,0 and field depletion 							B  h /B 0 						(magnetic gradient) for 							B  w /B 0 						= 5 × 10−3 and 								ω/Ω e  = 						0.1. The areas bounded by solid and dashed white curves indicate resonant 						energies in the wave region. The black cross on the ordinate of panels 						(a)–(b) is the energy at which the diffusion coefficients in panels 						(c)–(d) are calculated. (c) Normalized momentum and (d) pitch-angle 						diffusion coefficients. Vertical dashed lines in panels (a)–(d) are a 						critical value at which NL effects are dominant (see Equation (2)).
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Positions of significant atomic lines and molecular bands in the SpeX+MagE spectrum (0.3–0.9 μm). The emission lines and molecules that are predominantly responsible for certain absorption features are indicated at the relevant wavelengths.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Positions of significant atomic lines and molecular bands in the SpeX+MagE spectrum (0.9–2.4 μm). Some spectral regions with high telluric contamination are shaded.
Paper: Prospects for the Detection of the Sgr A* Photon Ring with Next-generation Event Horizon Telescope Polarimetry
Authors: Kaitlyn M. Shavelle, Daniel C. M. Palumbo
Figure caption: Top row: semianalytic KerrBAM model images corresponding to face-on viewing of the axisymmetric velocity and magnetic field geometries with a normal midplane crossing an optical depth of 0.5. Bottom row: corresponding distribution of the spiral phase ﹩\angle {\breve{\beta }}_{2}﹩, indicating no flip in the left two columns due to either the artificial removal of the photon ring (left) or the lack of a handed spiral in polarization (middle). However, in the rightmost column in which radial and toroidal velocities and magnetic fields are present and the photon ring is permitted, the spiraling polarization flips in the photon ring, leading to a detectable transition in polarimetric phases. Here and elsewhere in the Letter, sky-domain images of the accretion flow are shown in linear intensity scale with overlaid tick marks showing the electric vector position angle (EVPA), while the Fourier-domain phase signal is shown in blue–red periodic color.
Paper: Prospects for the Detection of the Sgr A* Photon Ring with Next-generation Event Horizon Telescope Polarimetry
Authors: Kaitlyn M. Shavelle, Daniel C. M. Palumbo
Figure caption: Impact of scattering and (u, v) track averaging on the ﹩\angle {\breve{\beta }}_{2}﹩ signal. Left panels: temporal distributions of ﹩\angle {\breve{\beta }}_{2}(v)﹩ for the unscattered (top) and scattered (bottom) Sgr A* movie between 4 and 14 Gλ, sampled along the v-axis. Right panels: noiseless baseline-averaged values of ﹩{\breve{\beta }}_{2}﹩ for unscattered (top) and scattered (bottom) experiments corresponding to the (u, v) tracks later used for the synthetic data in Figure 4 and onward. In the left column, horizontal lines show the maximum, median, and minimum of each distribution. In the right column, error bars show only intrinsic variation along the track, which spans both time and Fourier space; points with no error bars come from tracks containing only one data point.
Paper: Prospects for the Detection of the Sgr A* Photon Ring with Next-generation Event Horizon Telescope Polarimetry
Authors: Kaitlyn M. Shavelle, Daniel C. M. Palumbo
Figure caption: Averaging of ﹩\angle {\breve{\beta }}_{2}﹩ across baselines for individual and multiple nights. Left column: full single-scan phases ﹩\angle {\breve{\beta }}_{2}﹩. Middle column: phases and associated errors after averaging the complex ﹩{\breve{\beta }}_{2}﹩ along each baseline each night. Right column: same as the middle column, but baselines are averaged together across 10 nights of observation.
Paper: Understanding the Variability of Helium Abundance in the Solar Corona Using Three-fluid Modeling and Ultraviolet Observations
Authors: Leon Ofman, Yogesh, Silvio Giordano
Figure caption: The cross-sectional cut of the variables at r = 1.75 R  s  for the model run shown in Figure 3 (solid: protons; dashes: He++ ions; dotted–dashed: electrons). (a) The outflow velocities V  r . (b) The densities normalized by the values at maximal θ. (c) Proton, He++, and electron temperatures.
Paper: Prospects for the Detection of the Sgr A* Photon Ring with Next-generation Event Horizon Telescope Polarimetry
Authors: Kaitlyn M. Shavelle, Daniel C. M. Palumbo
Figure caption: Impact of scattering on the observed polarimetric spiral phase from one 345 GHz frame of the GRMHD simulation of Sgr A* used throughout this Letter. Left panels: unscattered. Right panels: scattered. Top row: the images and phase signal from photons corresponding only to the n = 0 image. Bottom row: all n are permitted. Because ﹩{\breve{\beta }}_{2}﹩ is an inteferometric quotient, it is invariant to the convolutional nature of diffractive scattering in the noise-free limit and is affected only by refractive scattering on the longest baselines accessible from the ground.
Paper: Understanding the Variability of Helium Abundance in the Solar Corona Using Three-fluid Modeling and Ultraviolet Observations
Authors: Leon Ofman, Yogesh, Silvio Giordano
Figure caption: The results of the 3D three-fluid model of the tilted streamer belt shown in the θ−ϕ [rad] plane at the height of r = 1.5 R  s . The densities are normalized in terms of n  e0 = 5 × 108 cm−3. Left panel: the normalized proton density. Right panel: the normalized density of the He++ ions. The dashed green line marks the longitude of the θ−r plane cuts in Figure 3.
Paper: Prospects for the Detection of the Sgr A* Photon Ring with Next-generation Event Horizon Telescope Polarimetry
Authors: Kaitlyn M. Shavelle, Daniel C. M. Palumbo
Figure caption: Impact of an increasing noise factor on the ﹩{\breve{\beta }}_{2}﹩ observable for an example campaign. The top row shows a single example night of observation, averaged along single baselines; the bottom shows the full 10-night averages of each baseline. Our long-baseline photon ring detection metric, SNRPR, is at the top right of each plot, evaluated from the red points identified by the algorithm in Section 3.2. As thermal noise is increased, some points disappear as they become polarimetric nondetections.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: A corner plot of the inferred parameters of the 1-comp model. Here “t1,” “rstar,” “dist,” “scale,” and “logf” represent the temperature of the quiescent component, the star’s radius, the star’s distance, the scaling parameter, and additional noise present in the data, respectively. The model was constructed using the SPHINX spectral grid and NIRSpec data.
Paper: Updated Spectral Characteristics for the Ultracool Dwarf TRAPPIST-1
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Michaël Gillon, Julien de Wit, Adam J. Burgasser, Laetitia Delrez, Aishwarya Iyer, Elsa Ducrot
Figure caption: Gravity-sensitive spectral features in in the NIRISS spectrum.
Paper: Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine
Authors: Jin-Ping Zhu, Liang-Duan Liu, Yun-Wei Yu, Ilya Mandel, Ryosuke Hirai, Bing Zhang, Aming Chen
Figure caption: Bolometric lightcurves based on the best fit to the multiband lightcurves of SN 2018kyt. The blue dashed, blue dotted, green dashed, and green dotted lines represent the contributions from the magnetar injection from the polar ejecta, the magnetar injection from the equatorial evaporated material and ejecta, radioactive heating, and interaction between the evaporated material and ejecta, respectively. The solid red line is the total luminosity.
Paper: Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine
Authors: Jin-Ping Zhu, Liang-Duan Liu, Yun-Wei Yu, Ilya Mandel, Ryosuke Hirai, Bing Zhang, Aming Chen
Figure caption: Best fits (solid lines) to multiwavelength lightcurves of selected bumpy SLSNe (dots with error bars) in our magnetar–star binary engine model. The label in each panel shows the different bands represented by different colors.
Paper: Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine
Authors: Jin-Ping Zhu, Liang-Duan Liu, Yun-Wei Yu, Ilya Mandel, Ryosuke Hirai, Bing Zhang, Aming Chen
Figure caption: An illustration of the physical stages of the magnetar–star binary engine.
Paper: Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine
Authors: Jin-Ping Zhu, Liang-Duan Liu, Yun-Wei Yu, Ilya Mandel, Ryosuke Hirai, Bing Zhang, Aming Chen
Figure caption: Posteriors on the fit parameters for SN 2018kyt. Medians with 16% and 84% quantiles are labeled.