adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Polarimetric Observations of the Western Hotspot of Pictor A
Authors: Stefano Tugliani, Francesco Massaro, Michela Negro, Raffaella Bonino, Nicolò Cibrario, Luca Latronico, Simone Maldera, Alessandro Paggi, Andrea Tramacere, Eileen T. Meyer, Ioannis Liodakis, Herman L. Marshall, Eric S. Perlman
Figure caption: Top panel: the background-subtracted X-ray spectra of the Pictor A WHS observed in the 2–8 keV energy range for all three DUs of IXPE, computed using an extracting circular region of 32″ radius (see Section 3) for the merged IXPE observations (the spectra for the first observation, i.e., OBSID: 03008601, and for the second one, i.e., OBSID: 03009799, are shown in two separate panels for graphical clarity). The best-fit model is an absorbed power law with column density fixed to the Galactic value NH = 3.64 × 1020 cm−2, with spectral index consistent with those previously found in the literature (see, e.g., A. S. Wilson et al. 2001; M. J. Hardcastle & J. H. Croston 2005). The best-fit model is also shown in all panels. Normalization factors between the three spectra are reported in Table 1. Above 6 keV the X-ray spectrum is completely dominated by the background, thus motivating our choice of excluding it to maximize the signal-to-noise. Bottom panel: the polarization contour plot of the whole ∼2 Msec observation for the XSPEC weighted analysis (A. Di Marco et al. 2022) with background subtraction (blue) and for the MLE method (orange) (contours at 68% and 99% confidence level). The black line represents the jet direction of Pictor A.
Paper: X-Ray Polarimetric Observations of the Western Hotspot of Pictor A
Authors: Stefano Tugliani, Francesco Massaro, Michela Negro, Raffaella Bonino, Nicolò Cibrario, Luca Latronico, Simone Maldera, Alessandro Paggi, Andrea Tramacere, Eileen T. Meyer, Ioannis Liodakis, Herman L. Marshall, Eric S. Perlman
Figure caption: The X-ray image obtained with IXPE (first observation) in the energy range between 2 and 8 keV for detector unit 1 in units of X-ray photons. Radio contours drawn from archival radio map at 4.8 GHz (R. A. Perley et al. 1997) start at the level of 10 mJy and increase by a factor of 4. The radio jet direction is indicated by a red dashed line, computed from the radio intensity peaks of the radio core and the WHS. The direction of the magnetic field lines from optical observations (R. C. Thomson et al. 1995) is represented as a solid black line. PAopt is marked and represents the position angle of the magnetic field. The image has been smoothed with a Gaussian kernel of 3 times the native IXPE pixel size (about 7﹩\mathop{.}\limits^{\unicode{x02033}}﹩2).
Paper: X-Ray Polarimetric Observations of the Western Hotspot of Pictor A
Authors: Stefano Tugliani, Francesco Massaro, Michela Negro, Raffaella Bonino, Nicolò Cibrario, Luca Latronico, Simone Maldera, Alessandro Paggi, Andrea Tramacere, Eileen T. Meyer, Ioannis Liodakis, Herman L. Marshall, Eric S. Perlman
Figure caption: Left panels: blue points show the number of X-ray photons measured in annular circular regions centered on the X-ray intensity peak of the Pictor A WHS, with a difference between outer and inner radii of 4″, as a function of the angular separation from its position: ΔNph(ϑ) = Nph(ϑ + Δϑ) − Nph(ϑ). The error bars are at 1σ. Orange points are evaluated with the same procedure, but for the background region, rescaled to have the same area as the source annular region. Right panels: the signal-to-noise ratio (SNR) computed using net measured X-ray photons divided by its Poisson uncertainty, as a function of the angular separation from the position of the X-ray intensity peak of the Pictor A WHS: ﹩\mathrm{SNR}=\frac{{N}_{\mathrm{ph}}-\lt {N}_{\mathrm{bkg}}\gt }{\sqrt{{N}_{\mathrm{ph}}}}﹩. This figure refers to the whole ∼2 Msec observation.
Paper: Quasiperiodic Slow-propagating Extreme-ultraviolet “Wave” Trains after the Filament Eruption
Authors: Yining Zhang, Ting Li, Weilin Teng, Xinping Zhou, Yijun Hou, Zheng Sun, Xuchun Duan, Yilin Guo, Guiping Zhou
Figure caption: AIA 171 Å time–distance stack plots of the EUV wave trains. Panel (a): time–distance plots along sector “s1” from 18:40 to 19:50 UT. The red and blue solid lines show the normalized GOES SXR flux data at 1–8 Å and the normalized integral intensities in the blue box shown as Figure 1(g) at AIA 131 Å wave band, respectively. The red dashed line is the normalized time derivative curve of the GOES SXR data. Panels (b)–(d): stack plots along sectors “s2,” “s3,” and “s4” from 18:40 to 19:50 UT, respectively. The red dotted lines in panels (b)–(d) denote the multiple wave fronts. The speeds of the waves are printed in red. The blue dashed line “L1” in panel (d) denotes the position to obtain the light curve in Figure 4(a). The green dashed lines in panel (d) denote the gradual and fast phases of the filament elevation, respectively. The speeds of the filament are printed in green.
Paper: Quasiperiodic Slow-propagating Extreme-ultraviolet “Wave” Trains after the Filament Eruption
Authors: Yining Zhang, Ting Li, Weilin Teng, Xinping Zhou, Yijun Hou, Zheng Sun, Xuchun Duan, Yilin Guo, Guiping Zhou
Figure caption: Wavelet analysis of the 171 Å light curve “L1” and GOES SXR time derivative. Panel (a): the red solid and blue dashed lines indicate the original and smoothed light curves “L1” in Figure 3(d), respectively. Panel (b): the wavelet map of the detrended intensity calculated from the difference between the two light curves in panel (a) from 19:00 to 19:50 UT. Panel (c): the corresponding global power. The orange dashed line represents the 95% confidence level, and the blue dashed line represents the period above the 95% confidence level with the maximum power (117.9 s). Panels (d)–(f): similar to panels (a)–(c), but for the GOES SXR time derivative data.
Paper: Quasiperiodic Slow-propagating Extreme-ultraviolet “Wave” Trains after the Filament Eruption
Authors: Yining Zhang, Ting Li, Weilin Teng, Xinping Zhou, Yijun Hou, Zheng Sun, Xuchun Duan, Yilin Guo, Guiping Zhou
Figure caption: Reconstruction of the coronal field of the flux rope and the inclined magnetic arcades before the eruption. Panel (a): reconstruction result as seen from the Earth, superimposed on the corresponding AIA 304 Å image. Panel (b): top view of the reconstructed coronal magnetic field in Cartesian coordinates. The background image represents the radial magnetic field at the photosphere. The white and black colors represent positive and negative magnetic polarities, respectively. The colored lines in panels (a) and (b) represent the magnetic field lines of the flux rope, while gray lines represent the inclined arcades.
Paper: Quasiperiodic Slow-propagating Extreme-ultraviolet “Wave” Trains after the Filament Eruption
Authors: Yining Zhang, Ting Li, Weilin Teng, Xinping Zhou, Yijun Hou, Zheng Sun, Xuchun Duan, Yilin Guo, Guiping Zhou
Figure caption: Schematic representations of the slow EUV wave trains. The blue and pink ellipses with minus and plus signs represent negative and positive magnetic polarities, respectively. The orange lines represent the flux rope. The green curves represent the inclined magnetic arcades above the flux rope. The thick black curves in panels (b) and (c) represent dim wave fronts.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Models with flat density cores (cB) develop large values of mass accretion rate, ﹩\dot{M}\sim 10\,\,{M}_{\odot }\,\,{{\rm{s}}}^{-1}﹩ (panel (a)), and dimensionless magnetic flux (panel (b)) that are favorable for the production of neutron-rich material and outflows (see Figure 2). Once the dimensionless magnetic flux exceeds the critical value, ϕ ∼ 10 (panel (b)), the jet-launching efficiency (panel (c)) and power (panel (d)) surge. Spurred by high ﹩\dot{M}﹩, the ignition radius, Rign (panel (e)), initially rises but drops as ϕ increases (panel (b)) and obstructs ﹩\dot{M}﹩ (panel (a)). Circles and squares mark tjet and tMAD of each model, respectively. To reduce clutter, we smoothed all quantities over Δt = 103 rg/c = 0.02 s.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Meridional cuts of the mass density (left-hand side) and electron fraction (right-hand side) for all models (different columns). The top row displays the system before jet launching (t < tjet), featuring neutron-rich disks where  Ye varies with mass accretion rate and disk magnetization. After the launching of jets and disk winds (tjet < t < tMAD), neutron-rich material is ejected from the disk midplane and carried by the shocked cocoon that engulfs the jets. In the bottom row, magnetic fields are dynamically important (t > tMAD), shortening the accretion timescale and reducing the disk densities, leading to a growing neutrino-cooling timescale, which leads to disk deneutronization and the cessation of neutron-rich outflows.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Density-weighted average electron fraction as a function of radius at various times for different models. The regions with neutron-rich material closely track the ignition radii (white lines). The increase in disk magnetic flux leads to jet launching (yellow dashed lines) and a transition to MAD (red dashed lines). This transition signifies the drop in the accretion timescale and increase in the neutrino-cooling timescale due to decreasing densities, which ultimately ends the neutron-rich phase of the disk.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Unbound mass binned by electron fraction in models with significant mass ejection (excluding pB0) at different times. Unbound mass is characterized according to the Bernoulli criterion in Equation (18), where before jet launching, we omit the magnetic field contribution (b2/ρ term). Stronger fields unbind more low-Ye material, maintaining a nearly flat distribution above the Ye cutoff. Over time, the mixing of low-Ye outflows with the star raises the lower Ye cutoff, resulting in an increased mass at higher Ye values.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Density-weighted average accretion (solid lines) and neutrino-cooling (dashed lines) timescales in the disk at a characteristic radius, r = 10 rg, in all models, as functions of time.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Meridional cuts of the electron neutrino (left-hand side) and antineutrino number density (right-hand side) for all models (different columns). The top row displays the system before jet launching (t < tjet); the middle row shows the system after the launching of jets and disk winds (tjet < t < tMAD); and the bottom row shows the systems after they achieve an MAD state (t > tMAD).
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Time evolution of electron neutrino (panel (a)), antineutrino (panel (b)), and heavy lepton neutrino (panel (c)) luminosities for all models. Neutrino luminosities are calculated as radiative power ﹩{L}_{{\nu }_{i}}=\int \sqrt{-g}(-{R}_{t}^{r})d\theta d\varphi {| }_{r={r}_{{\rm{ext}}}}﹩, measured at an extraction radius rext = 100 rg ≈ 600 km. All quantities are smoothed over Δt = 103 rg/c = 0.02 s.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: The distribution of energy density in a radiative sphere with radius r = 1, for two values of absorption opacities. The emission and absorption are in equilibrium inside the sphere, and the medium outside the sphere is optically thin. The steady-state profiles (red circles) show a good agreement with the analytical solution (red lines).
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Lab frame energy density in the radiative shadow tests, where either a single beam (left) or intersecting plane–parallel beams (right) shine on an optically thick sphere (red dashed circle), producing a shadow.
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: Lab frame energy density of the beams propagating in the curved spacetime of a Schwarzschild BH. Beams propagate along the geodesics (red dashed lines).
Paper: Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis
Authors: Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi, Alexander Tchekhovskoy
Figure caption: The benchmark of νH-AMR, performed using the simulation initialized with the setup of the model cBw  on the grid with total size 200 × 200 × 200 on a single GPU (2 × 2 × 2 blocks with 100 × 100 × 100 cells per block.)