adsabs/AstroCLIMB huggingface dataset:
Paper: The Radio Flare and Multiwavelength Afterglow of the Short GRB 231117A: Energy Injection from a Violent Shell Collision
Authors: G. E. Anderson, G. P. Lamb, B. P. Gompertz, L. Rhodes, A. Martin-Carrillo, A. J. van der Horst, A. Rowlinson, M. E. Bell, T.-W. Chen, H. M. Fausey, M. Ferro, P. J. Hancock, S. R. Oates, S. Schulze, R. L. C. Starling, S. Yang, K. Ackley, J. P. Anderson, A. Andersson, J. F. Agüí Fernández, R. Brivio, E. Burns, K. C. Chambers, T. de Boer, V. D'Elia, M. De Pasquale, A. de Ugarte Postigo, Dimple, R. Fender, M. D. Fulton, H. Gao, J. H. Gillanders, D. A. Green, M. Gromadzki, A. Gulati, D. H. Hartmann, M. E. Huber, N. J. Klingler, N. P. M. Kuin, J. K. Leung, A. J. Levan, C.-C. Lin, E. Magnier, D. B. Malesani, P. Minguez, K. P. Mooley, T. Mukherjee, M. Nicholl, P. T. O'Brien, G. Pugliese, A. Rossi, S. D. Ryder, B. Sbarufatti, B. Schneider, F. Schüssler, S. J. Smartt, K. W. Smith, S. Srivastav, D. Steeghs, N. R. Tanvir, C. C. Thoene, S. D. Vergani, R. J. Wainscoat, Z.-N. Wang, R. A. M. J. Wijers, D. Williams-Baldwin, I. Worssam, T. Zafar
Figure caption: Luminosity comparisons of GRB 231117A (gold stars/triangles) and the other radio-detected SGRBs (black circles/triangles) between 5 and 8 GHz (W. Fong et al. 2014, 2015, 2021; T. Laskar et al. 2022; M. Ferro et al. 2023; G. E. Anderson et al. 2024; A. J. Levan et al. 2024; G. Schroeder et al. 2025). The radio-detected short-duration GRB 210726A (blue squares/triangles; G. Schroeder et al. 2024) and GRB 160821B (green large diamonds/triangles; G. P. Lamb et al. 2019; E. Troja et al. 2019) that displayed energy injection (see Section 5.3) are also illustrated (note that GRB 051221A was not detected in this frequency range; A. M. Soderberg et al. 2006). We have also highlighted the long-duration merger GRB 230307A (purple diamonds/triangles; A. J. Levan et al. 2024) that had a long-lived central engine.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Fits and residuals for the models described in Section 4.1.1. The left panel shows all filters for one object, SN 2017cbv. The residuals are plotted both with respect to the full model (squares) and with respect to just the stretched template (diamonds), to visualize the strength of the early excess. Residuals are plotted as the normalized “pull,” defined as (Ldata − Lmodel)/(σdata × σ) (i.e., the number of corrected standard deviations away from the model, with σ being the best-fit value in Table 3). The right panel shows the same style of plot but looking in one filter (g band) across all objects. The variety of early behavior is apparent in the strengths and durations of the discrepancy between the two sets of pulls. The plotted range is only over 10 rest-frame days since first light, but the objects are fit over a larger range to +5 days from peak.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Posteriors for the a and θ parameters from the fits described in Section 4.1.2. The three objects with early excesses (SNe 2017cbv, 2017erp, and 2018yu) are emphasized with a dotted hatch. SN 2018gv also has a hatch to distinguish itself from SN 2017fgc since the two have such similar posteriors. We have included predictions for the companion separations from different classes of donor stars (He star, MS, or RG) from Z.-W. Liu et al. (2015). The top and bottom half of the viewing-angle plot are equivalent, and objects are placed in different halves solely to minimize overlaps between posteriors.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: LCO data of SN 2017cbv compared with the best-fit models described in Sections 4.1 and 4.2 and listed in Tables 3 and 4. All fits were done in magnitude space (top panel), but we show them in color space (B − V, bottom panel) as well. The companion-shocking models fit better in both cases, although the models' earliest B − V colors evolve more than they are observed to do (probably due to oversimplified temperature evolution, as discussed in the text).
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: The multiplicative factor on the companion interaction shock flux, i.e., Equation (4), originally from P. J. Brown et al. (2012). Shock flux is extremely diminished for θ > 135°, which could explain why multiple objects converge to θ = 180° when no obvious excess is detected (see Figure 5), leading to the largest discrepancy between the expected and measured distributions (see Figure 6).
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: The CDF of viewing-angle posteriors compared with the expected distribution. There is not enough evidence to reject the null hypothesis that SNe Ia predominantly arise in single-degenerate systems.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: The same residuals (with respect to the stretch template, g band) as in Figure 3, overplotted together to more easily compare between different objects. We identify objects with residuals in the gray box (earlier than 5 days from first light, stronger than 5σ) as having an early excess, except for SN 2019np for reasons discussed in the text.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Full data set (DLT40+LCO+Swift) for all objects in the sample. Lower limits are included as downward-pointing triangles.
Paper: Early Lightcurves of Type Ia Supernovae Are Consistent with Nondegenerate Progenitor Companions
Authors: J. Burke, M. Andrews, D. A. Howell, D. J. Sand, R. C. Amaro, P. J. Brown, J. E. Andrews, K. A. Bostroem, Y. Dong, J. Haislip, D. Hiramatsu, G. Hosseinzadeh, V. Kouprianov, M. J. Lundquist, C. McCully, C. Pellegrino, D. Reichart, L. Tartaglia, S. Valenti, S. Wyatt, S. Yang
Figure caption: Corner plot of the model described in Section 4.1.1 for SN 2017erp. Errors in the inset lightcurve have been multiplied by the best-fit value of the σ parameter.
Paper: On the Fe XXII Emission in the X-Ray Spectrum of NGC 1068
Authors: M. Z. Buhariwalla, J. M. Miller, L. C. Gallo, J. Mao, J. Raymond, T. Kallman
Figure caption: The Fe XXII doublet viewed in isolation. The red dotted lines indicate the wavelengths of the Fe XXII doublet used by C. W. Mauche et al. (2003, 2004). The first blue dotted–dashed line (11.74 Å) is the result of Fe XXIII emission that can contribute flux to the density diagnostic (H. Chen et al. 2004; G. Y. Liang & G. Zhao 2008). The fit shown includes two Gaussian components (ZAGUSS) at 11.77 and 11.94 Å. The outflow velocity was vout = 280 ± 150 km s−1, and the ratio of the line strengths was ﹩{\rm{R}}{\rm{a}}{\rm{t}}{\rm{i}}{\rm{o}}=0.4{1}_{-0.15}^{+0.17}﹩. The width of each line was measured to be σ = 780 ± 150 km s–1.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: (a): Radial surface brightness profiles of the deprojected galaxy MaNGA 8992-6101 are shown for the g (blue), r (green), and z (red) bands. The average of all available bands at each radius is plotted in black and labeled as “m” (master) in the plot. A 3 pixel-wide pseudoslit is placed along the bar major and minor axes to obtain the mean surface brightness at each radius. The radial profile along the bar major axis is plotted as a thin solid line, while the profile along the bar minor axis is shown as a thick solid line with markers at each radial point. Azimuthally averaged radial profiles are plotted as dashed–dotted lines. Vertical line segments with square caps on both ends indicate the radius corresponding to the maximum difference in surface brightness profiles along the bar major and minor axes, ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩. Triangles indicate the dip radius (RDip) in the radial profile along the bar minor axis for each band. Vertical lines represent the bar radius (Rbar, shown as a dotted line), the radius of the maximum difference between radial profiles along the bar major and minor axes (﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩, solid line), and the dip radius along the bar minor axis (RDip, dashed line). The values of ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩ and RDip are displayed at the bottom right of the plot, where the measurements from the “m” (master) profile are used for further analysis. (b): g-band image of MaNGA 8992-6101. The yellow solid circle marks ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩, while the cyan dashed circle denotes RDip. The black solid bar in the bottom-left corner represents 10″.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: Ratio of dark gap radius to RCR. (a): Histogram of ﹩{\mathrm{log}}({R}_{{\rm{Max}}({\rm{\Delta }}\mu )}/{R}_{{\rm{CR}}})﹩ for all galaxies. The vertical dashed line indicates where ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩ equals RCR, while the region enclosed by the two dotted lines represents the inferred extent of the inner UHR, estimated using Equation (1). (b): Histogram of ﹩{\mathrm{log}}({R}_{{\rm{Dip}}}/{R}_{{\rm{CR}}})﹩ for galaxies exhibiting a single dip. (c): Relation between ﹩{\mathrm{log}}({R}_{{\rm{Max}}({\rm{\Delta }}\mu )}/{R}_{{\rm{CR}}})﹩ and the rotation rate, ﹩{ \mathcal R }﹩. Spearman’s rank correlation coefficient (ρ) and statistical significance (P) are shown in the upper right. A linear fit to the data is displayed as a gray dashed line, with the corresponding equation given in the lower left corner. (d): Relation between ﹩{\mathrm{log}}({R}_{{\rm{Dip}}}/{R}_{{\rm{CR}}})﹩ and ﹩{ \mathcal R }﹩ for galaxies with a single dip.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: Radial surface brightness profiles of galaxies, derived by averaging data over all available g, r, i (if present), and z bands, are shown. Three types of barred galaxies are presented, categorized by the presence of dips along the bar minor axis: (1) no dip, (2) a single dip, and (3) two dips. Thin solid lines represent the radial profiles along the bar major axis, while thick blue lines denote the profiles along the bar minor axis. Azimuthally averaged profiles are indicated by dotted–dashed lines. Dips are marked with red triangles in the profile and the RDip is shown in orange dashed circle in the deprojected image, if any. The maximum differences between the bar major and minor axis profiles are shown as lines with black square caps in the profile and ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩ is shown in black circle in the deprojected image.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: The distribution of ﹩{\mathrm{log}}({R}_{{\rm{Max}}({\rm{\Delta }}\mu )}/{R}_{{\rm{CR}}})﹩ for galaxies grouped by the number of dips in their surface brightness profiles along the bar minor axis: 0 dip (black dashed line), 1 dip (blue solid line), and 2 dips (red solid line). Vertical dotted lines indicate the region of the inner UHR, and the solid line indicates the CR radius. The top-right box shows the results of KS tests between group pairs, including the KS statistic (D) and the associated p-value (P). For example, D01 and P01 refer to the comparison between the 0-dip and 1-dip groups. The high D-value and low p-value for D12 indicate that the 1-dip and 2-dips groups differ significantly in their distributions.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: (a) Histogram of the difference between ﹩{R}_{{\rm{Max}}({\rm{\Delta }}\mu )}﹩ and RDip, normalized by the deprojected bar length, for galaxies exhibiting a single dip. The sample is divided into fast and slow bars. (b) Normalized difference between the two dark gap radii and the bar rotation rate, ﹩{ \mathcal R }﹩, which is RCR/Rbar. Horizontal dashed line divides fast (﹩{ \mathcal R }\,\leqslant \,﹩1.4) and slow (R > 1.4) bars. Data points are color-coded by total stellar mass.
Paper: On the Fe XXII Emission in the X-Ray Spectrum of NGC 1068
Authors: M. Z. Buhariwalla, J. M. Miller, L. C. Gallo, J. Mao, J. Raymond, T. Kallman
Figure caption: Diagnostic curves for the CI-PION model. The solid red, blue, and green curves indicate that for a plasma with kT = 1 keV, the critical density of the diagnostic lines increases as ionization decreases. The dotted red and blue curves are included to illustrate what the curves would look like without temperature manipulation (i.e., in a purely photoionized scenario). The black dashed line is the diagnostic curve produced by a plasma in CIE with a temperature of 1 keV.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: Ratio of dark gap radius to RCR for galaxies exhibiting two dips. The dip radii are ranked by their distance from the galaxy center. (a): Histogram of the ratio of the first dip radius to the RCR, R1st,2Dip/RCR. (b): Histogram of the ratio of the second dip radius to the RCR, R2nd,2Dip/RCR. The vertical dashed line indicates the CR radius (RCR), while the dotted and dashed–dotted lines correspond to the inner UHR and the OLR, respectively.
Paper: Dark Gaps and Resonances in Barred Galaxies
Authors: Taehyun Kim, Dimitri A. Gadotti, Myeong-gu Park, Yun Hee Lee, Francesca Fragkoudi, Minjin Kim, Woong-Tae Kim
Figure caption: Ratio of RDip/RCR for galaxies exhibiting a single dip. The galaxies are classified into five groups and plotted using different colors. Galaxies with an inner ring are shown in the upper panel, while those without an inner ring are presented in the lower panel.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: 3D representation of the magnetic field lines for different magnetic moment configurations. Top row: both stars have aligned magnetic moments (↑ ↑), shown from two perspectives, equatorial plane (left) and top-down along the orbital axis (right). Middle row: a configuration with α1 = 0°, α2 = 45°, ΔΦ = 0°, and λ = −1 (↑ ↙), presented at two snapshots separated by half orbital rotation. Bottom row: a configuration α1 = 90°, α2 = 90°, ΔΦ = 0°, and λ = −1 (→ ←), shown at two snapshots separated by a quarter orbital rotation. The red and blue lines correspond to fields that start and close on the same star. In contrast, the purple lines represent field lines that originate from the north pole of the first star and connect to the south pole of the second star, while the orange lines represent field lines that originate from the north pole of the second star and connect to the south pole of the first star. The black lines correspond to the open magnetic fields. We note that the time coordinate τ < tFinal = −7.7 ms indicates that these cases correspond to simulations with an initial separation of d = 4.64r⋆, larger than the separation used in the rest of the parameter exploration simulations.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The total Poynting flux crossing a spherical surface with radius 13r⋆ for various inclination angle combinations of the two stars, shown for cases with λ = 1 (left) and λ = −1 (right). The dotted line, in both plots, is the orbital average Poynting flux ﹩\overline{\langle L\rangle }﹩ derived from the scaling law of Equation (15) for ∣λ∣ = 1.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Similar to Figure 4. The first and second columns correspond to λ = 1 with the right star having inclination angles of α2 = 45° (↑ ↗) and α2 = 90° (↑ →), respectively. Similarly, the third and fourth columns represent λ = −1, with α2 = 45° (↑ ↙) and α2 = 90° (↑ ←), respectively.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The evolution of the Poynting flux, normalized to L0 (as indicated), crossing a spherical surface of radius 13r⋆ around the system for equal aligned (↑ ↑, left column) and antialigned (↑ ↓, right column) magnetic moments. For the aligned case, ﹩{L}_{0}^{\uparrow \uparrow }=0.36\times 1{0}^{44}{B}_{12}^{2}{r}_{12\,{\rm{km}}}^{2}\,{\rm{erg}}\,{{\rm{s}}}^{-1}\,s{r}^{-1}﹩, while, for the antialigned case, ﹩{L}_{0}^{\uparrow \downarrow }=1.24\times 1{0}^{44}{B}_{12}^{2}{r}_{12\,{\rm{km}}}^{2}\,{\rm{erg}}\,{{\rm{s}}}^{-1}\,s{r}^{-1}﹩. Here, B12 and r12 km are the surface magnetic field (in units of 1012 G) and the stellar radius (in units of 1.2 × 106 cm).
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The magnetospheric structure at τ = −4.27 ms, similar to Figure 8, is shown with increasing absolute values of the magnetic moment ratio from top to bottom. The left column illustrates the impact of the magnetic moment ratio in the antialigned case (α1 = 0°, α2 = 0°) (↑ ↓). The middle and right columns follow the same pattern, but for the configurations α1 = 90°, α2 = 0°, ΔΦ = 0° (→ ↓, middle) and α1 = 90°, α2 = 45°, ΔΦ = 0° (→ ↙, right), respectively.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Snapshots of the Poynting flux evolution over a full rotation of the system, directly corresponding to the magnetospheric configurations and snapshots presented in Figure 6.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: 3D volume rendering of the Poynting flux for the case with α1 = 0°,  α2 = 45°,  λ = −1, and ΔΦ = 0° (↑ ↙) similar to the middle row of Figure 5. (Left) Snapshot at τ = −9.91 ms, and (right) snapshot for τ = −8.6 ms, the two instances are separated by half an orbital period. The color scale represents the local Poynting flux values, while only regions where the Poynting flux multiplied with r2 exceeds a threshold are shown, effectively accounting for the radial decrease in flux with distance and highlighting areas of intrinsically strong emission.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The total Poynting flux crossing a spherical surface of radius 13r⋆ throughout the system evolution for equal antialigned (↑ ↓, solid line) and aligned (↑ ↑, dashed line) magnetic moments.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The polar caps, i.e., instantaneous zones of open flux, of the two stars in a Mollweide projection in the case with α1 = 0°,  α2 = 45°,  λ = −1, and ΔΦ = 0° (↑ ↙) similar to the middle row of Figure 5. The top panel corresponds to τ = −9.91 ms, while the bottom panel shows τ = −8.6 ms, with the two snapshots separated by half an orbital period.
Paper: Accretion Flow Properties of Swift J1727.8–1613 during Its Rising Phase of the Discovery Outburst: Estimation of Mass from Spectrotemporal Study
Authors: Dipak Debnath, Hsiang-Kuang Chang, Sujoy Kumar Nath, Lev Titarchuk
Figure caption: Variation of (a) Insight-HXMT count rates in the SXR (2–4 keV), HXR (4–150 keV), and TXR (2–150 keV) energy bands and (b) the HR (i.e., the ratio between HXR and SXR rates) is shown. (c) The evolution of the frequency of the observed QPOs is presented. Variations of the constant⨂tbabs(diskbb+pexrav) model-fitted parameters, (d) pexrav photon index (Γ), (e) diskbb temperature (Tin), and (f)–(h) model component fluxes and their ratio, are shown in the subsequent panels. Background shades subdivide the evolution of the QPO frequencies into six parts: (1) monotonically rising, (2) roughly constant, (3) monotonically rising, (4) monotonically decreasing, (5) rapidly rising, and (6) sporadically increasing or decreasing. Furthermore, based on the temporal and spectral variations, parts 1–6 are reclassified as HS(ris), HIMS(ris), HIMS(ris), HIMS(dec), HIMS(ris), and SIMS(ris), respectively. The points enclosed in red squares in panel (c) indicate the observations for which detailed PDS and spectral fits are presented in Figures 2 and 3, respectively.