adsabs/AstroCLIMB huggingface dataset:
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: the νF(ν) spectra for region I best fit by a COMP model (left), the νF(ν) spectra for region II best fit by a COMP+BB model (middle), and the νF(ν) spectra for subregion IVc best fit by a Band+PL model (right). Bottom: average examples of counts spectrum plots during the Fermi-GBM BTI region of subinterval IVb (Left: t 0 + 243.1 s; middle: t 0 + 244.1 s; and right: t 0 + 265.6 s) achieved by using the PPU-correction method described in Section 3.1. The spike at 511 keV is ignored during the fitting process and does not affect the fit statistic.
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: Uncorrected Fermi-GBM CSPEC data (1.024 s resolution) in the five NaI detectors with viewing angles to GRB 221009A below 60° at trigger time and the evolution of the MVT (﹩{\rm{\Delta }}{t}_{{\rm{\min }}}﹩) obtained from the Fermi-GBM non-BTI regions. The MVT ranges from ∼0.01 to ∼1 s. The decreasing MVT occurs in regions where the count rate is more variable. Bottom: Uncorrected Fermi-GBM CTIME data (0.064 s resolution) for the same two NaI detectors during the first Fermi-GBM BTI region.
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: the light curve of GRB 221009A from 8 keV to 40 MeV before and after PPU correcting in the Fermi-GBM BTI regions. Bottom: short and long GRB E iso (left) and L iso (right) measures of Fermi-GBM-detected GRBs with known redshift values through 2017 (Abbott et al. 2017), with updated spectral measures from Poolakkil et al. (2021). Key GRBs are highlighted. The downward arrows indicate GRBs best fit by a PL spectral model, which must turnover somewhere, so they are shown as upper limits. The E iso plot is supplemented with low- or intermediate-luminosity GRBs with associated supernova from Cano et al. (2017). We do not utilize their luminosity measures as they are averaged (not peak).
Paper: Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow
Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas
Figure caption: Top: background-subtracted and normalized light curves of 0.512 s binned Fermi-GBM TTE data and 1.0 s binned LLE data for the triggering pulse with the higher-energy photons arriving prior to the lower-energy photons. Bottom: the fitted counts spectrum (left), the model spectrum (center), and the posteriors of the model parameters (right) for the mBB function fitted to the triggering pulse.
Paper: Exact Calculation of Nonideal Fields Demonstrates Their Dominance of Injection in Relativistic Reconnection
Authors: Samuel R. Totorica, Seiji Zenitani, Shuichi Matsukiyo, Mami Machida, Kazuhiro Sekiguchi, Amitava Bhattacharjee
Figure caption: (a) Comparison of average fractional contribution of nonideal field to injection for 2D and 3D simulations with σ = 50 and B  G  = 0, at time ω  p  t ≈ 2000. Inset shows the corresponding electron energy spectra, with a power-law spectrum with index α = 2.5 plotted for reference. (b) Magnetic field magnitude in 2D slices of the 3D simulation at ω  p  t ≈ 1200. (i) x–y plane at z/(c/ω  p ) = 31, and (ii) x–z plane at y = 0 (dashed line shows the location of the x–y slice). (c) Convergence studies showing the average fractional contribution of the nonideal field to injection for σ = 50, B  G  = 0 simulations with standard parameters (black), n ppc = 1024 (blue), Δx/(c/ω  p ) = 1/10 (green), and a domain size of L  x /(c/ω  p ) = 2000 and L  y /(c/ω  p ) = 4500 (red). (d) Distribution of injection energies obtained from simulations with varied σ. Dashed blue line shows a fit of the σ = 25 case to the function a ϵ  b  e −ϵ/c . All solid black lines correspond to the 2D simulation with σ = 50 and B  G  = 0.
Paper: Exact Calculation of Nonideal Fields Demonstrates Their Dominance of Injection in Relativistic Reconnection
Authors: Samuel R. Totorica, Seiji Zenitani, Shuichi Matsukiyo, Mami Machida, Kazuhiro Sekiguchi, Amitava Bhattacharjee
Figure caption: (a) Physical quantities from a region of a σ = 50 relativistic reconnection simulation: ideal electric field  E  I (top); nonideal electric field  E  N (middle); ratio of electric and magnetic field magnitudes with color scaled so that only regions satisfying ﹩\left|{\boldsymbol{E}}\right|\gt \left|{\boldsymbol{B}}\right|﹩ are white (bottom). (b) Representative simulation particle trajectory from a σ = 50 simulation of relativistic reconnection plotted over the out-of-plane component of the nonideal electric field with overlaid magnetic field lines. The trajectory corresponds to the shaded times in (c), with the circle showing the position at the beginning of this period and the star showing the position at the time when ϵ  T  = σ/4. (c) Evolution of energy gained by the nonideal (ϵ  N ) and ideal (ϵ  I ) electric fields. (d) Energy gained from the nonideal field (ϵ  N /σ) vs. total energy (ϵ  T /σ) and fractional energy gain from the nonideal electric field, ϵ  N /ϵ  T , vs. total particle energy ϵ  T /σ.
Paper: Exact Calculation of Nonideal Fields Demonstrates Their Dominance of Injection in Relativistic Reconnection
Authors: Samuel R. Totorica, Seiji Zenitani, Shuichi Matsukiyo, Mami Machida, Kazuhiro Sekiguchi, Amitava Bhattacharjee
Figure caption: (a) Electron energy spectra at the end of the simulation (ω  p  t ≈ 2000) for various conditions. Solid lines have B  G  = 0, and dashed lines have σ = 50 and B  G  > 0. Dotted black line shows a power-law spectrum with index α = 2.5 for reference. (b) Average fractional nonideal contribution to energization up to various threshold energies ϵ* for the σ = 50, B  G  = 0 simulation. (c) Average fractional nonideal contribution to energization up to ϵ* = σ/4 for simulations with varied σ and B  G  = 0. (d) Same as (c), but for σ = 50 and varied B  G . All solid black lines correspond to the 2D simulation with σ = 50 and B  G  = 0.
Paper: Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational Instability around an FU Ori Star?
Authors: Philipp Weber, Sebastián Pérez, Alice Zurlo, James Miley, Antonio Hales, Lucas Cieza, David Principe, Miguel Cárcamo, Antonio Garufi, Ágnes Kóspál, Michihiro Takami, Joel Kastner, Zhaohuan Zhu, Jonathan Williams
Figure caption: Applying synthesis imaging reconstruction techniques to the ALMA band 6 data. (a) and (b) show the tclean reduction, (a) using natural weighting (same as in Figure 2) and (b) using Briggs weighting with robust = 0.5. The resulting clean beam sizes are 0.″14 × 0.″20 and 0.″10 × 0.″16, respectively. Panels (c) and (d) show the GPUVMEM reconstruction technique applied to the data. Panel (c) was restored using the clean beam of panel (a); panel (d) shows the image model. In all panels, the clean beam is displayed in translucent white in the bottom right corner. We measure the rms noise, σ, for each image individually, written in the top left corner of each respective image and in units of μJy  beam−1. The contours are shown at levels of 3σ, 4σ, and 5σ. The position of the central star is marked by a +. The GPUVMEM model does not allow a measurement of the rms noise.
Paper: Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational Instability around an FU Ori Star?
Authors: Philipp Weber, Sebastián Pérez, Alice Zurlo, James Miley, Antonio Hales, Lucas Cieza, David Principe, Miguel Cárcamo, Antonio Garufi, Ágnes Kóspál, Michihiro Takami, Joel Kastner, Zhaohuan Zhu, Jonathan Williams
Figure caption: Comparison of ALMA band 6 continuum image in mJy beam−1 using natural weights (left panel) with SPHERE/IRDIS polarized light image (right panel, see Figure 1). Both images are overlaid with contours of the ALMA continuum at levels of 3σ rms, 4σ rms, and 5σ rms (with σ rms = 28 μJy beam−1). The clean beam of the ALMA observation is shown in white in the bottom right corner of the left panel (0.″14 × 0.″20). The arrows in the left panel mark the dust clumps.
Paper: Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational Instability around an FU Ori Star?
Authors: Philipp Weber, Sebastián Pérez, Alice Zurlo, James Miley, Antonio Hales, Lucas Cieza, David Principe, Miguel Cárcamo, Antonio Garufi, Ágnes Kóspál, Michihiro Takami, Joel Kastner, Zhaohuan Zhu, Jonathan Williams
Figure caption: SPHERE/IRDIS linearly polarized intensity (PI) observation of V960 Mon in the H band. PI is normalized to its maximum value (6.6 mJy arcsec−2) and on a logarithmic scale. The frame is centered on the primary, which was covered by the coronagraph displayed by a black circle. The projected scale is shown in the lower right assuming the distance of 2189 pc.
Paper: Spirals and Clumps in V960 Mon: Signs of Planet Formation via Gravitational Instability around an FU Ori Star?
Authors: Philipp Weber, Sebastián Pérez, Alice Zurlo, James Miley, Antonio Hales, Lucas Cieza, David Principe, Miguel Cárcamo, Antonio Garufi, Ágnes Kóspál, Michihiro Takami, Joel Kastner, Zhaohuan Zhu, Jonathan Williams
Figure caption: Fitting consistent spirals to the images: the left panel shows the ALMA data with the 3σ rms, 4σ rms, and 5σ rms contours. The white crosses represent the data points used for tracing the spiral arm. The black curve corresponds to a function fitted to the deprojected data points, which are then reprojected onto the image plane. The SPHERE observation in the right panel includes the same white crosses delineating the millimeter spiral. Additionally, the yellow crosses represent the projection of the white crosses onto the scattering surface, assuming the function for the scattering height, h scat, described in the text.
Paper: Distribution of s-, r-, and p-process Nuclides in the Early Solar System Inferred from Sr Isotope Anomalies in Meteorites
Authors: Jonas M. Schneider, Christoph Burkhardt, Thorsten Kleine
Figure caption: Schematic plots illustrating the mixing model of this study. (a) Plot of μ 50Ti vs. μ 54Cr showing the location of the three components used in the mixing model: IC, NClow, NChigh. Fractions f IC,NC and fIC,CC can be calculated by assuming that NChigh and CI are mixtures of NClow and IC (see text for details). (b) Plot of μ 94Mo vs. Δ95Mo. For definition of Δ95Mo see text. Variations in Δ95Mo reflect r-process variations, whereas variations in μ 94Mo mostly reflect s-process variation. The position of the mixing end-members IC and NClow are indicated, as well as the resulting compositions of NChigh and CI. For details about the model see text.
Paper: Distribution of s-, r-, and p-process Nuclides in the Early Solar System Inferred from Sr Isotope Anomalies in Meteorites
Authors: Jonas M. Schneider, Christoph Burkhardt, Thorsten Kleine
Figure caption: Expected μ 84Sr anomalies for enstatite chondrites (EC), ordinary chondrites (OC), angrites, and ureilites resulting from only s- and only (r, p)-process variations. These variations lead to μ 84Sr variations of opposite sign but similar magnitude, and so no resolvable μ 84Sr variations remain among NC meteorites. Measured μ 84Sr values for EC, OC, and angrites are shown for comparison and are well reproduced by the model. There are no μ 84Sr data for ureilites, but they are also predicted to have μ 84Sr ≈ 0. Gray band represents the inner solar system average μ 84Sr = 5±4 (95% conf.). Data are summarized in Table A2.
Paper: Distribution of s-, r-, and p-process Nuclides in the Early Solar System Inferred from Sr Isotope Anomalies in Meteorites
Authors: Jonas M. Schneider, Christoph Burkhardt, Thorsten Kleine
Figure caption: Average μ 84Sr values of terrestrial, lunar, and meteoritic samples measured in this study. Uncertainties are 95% conf. for n ≥ 4 and 2 s.d. for n < 4. Gray box represents inner average of μ 84Sr = 5±4 (95% conf.). Arrows indicate effect of excesses and deficits in s-, r-, and p-process Sr on μ 84Sr.
Paper: Distribution of s-, r-, and p-process Nuclides in the Early Solar System Inferred from Sr Isotope Anomalies in Meteorites
Authors: Jonas M. Schneider, Christoph Burkhardt, Thorsten Kleine
Figure caption: Fraction of IC material in the NC and CC reservoirs calculated using Equations (1) and (3). Data used in these calculations are summarized in Table A1.
Paper: Collapsar Black Holes Are Likely Born Slowly Spinning
Authors: Ore Gottlieb, Jonatan Jacquemin-Ide, Beverly Lowell, Alexander Tchekhovskoy, Enrico Ramirez-Ruiz
Figure caption: Smoothed time evolution of the numerical models, as measured at 3r  g . (a) The mass accretion rate onto the BH drops moderately over time, owing to suppression by the jet structure. (b) The jet launching efficiency is in a good agreement with Lowell et al. (2023), featuring η ≃ 0.5, 0.02, and 0.005 for a = 0.8, 0.2, and 0.1, respectively. (c) Given the similar ﹩\dot{m}﹩ in all models, BHs with a = 0.1 power jets that are two orders of magnitude less luminous than jets from BHs with a = 0.8, having L  j  ≈ 1050 erg s−1 that is comparable with the characteristic GRB luminosity. The vertical dashed lines represent the breakout time of the outflow from the star, after which the luminosity can be observed. (d) Accreted mass. The differences in the mass accretion rate (solid lines) lead to less total accreted mass onto the BH when the jet launching and propagation are more efficient. The high efficiency η ≃ 0.5 when a = 0.8 indicates that half of the accreted mass is expelled as outflows, resulting in BH mass gain that is only half of the total accreted mass (dashed line).
Paper: Collapsar Black Holes Are Likely Born Slowly Spinning
Authors: Ore Gottlieb, Jonatan Jacquemin-Ide, Beverly Lowell, Alexander Tchekhovskoy, Enrico Ramirez-Ruiz
Figure caption: 3D rendering of the jet magnetization after breakout in models a8δ0 (top), a1δ0 (middle), and a1δ1 (bottom) at t = t  s . While all jets find their way out from the star (dark blue), in model a8δ0 the jet retains a mild magnetization and features a stratified structure, whereas in models a1δ0 and a1δ1 the jets fail to remain intact as they lose most of their energy to mixing with the star.
Paper: Collapsar Black Holes Are Likely Born Slowly Spinning
Authors: Ore Gottlieb, Jonatan Jacquemin-Ide, Beverly Lowell, Alexander Tchekhovskoy, Enrico Ramirez-Ruiz
Figure caption: Radial profiles of the asymptotic proper velocity (a) and magnetization (b) of the jets inside the star, calculated by the maximum value at each radius at time t  s . The powerful jet (model a8δ0) maintains relativistic velocities and mild magnetization, whereas the weaker jets undergo strong mixing with the star so they exhibit a mildly relativistic breakout with a low magnetization.
Paper: Demonstrating Photon Ring Existence with Single-baseline Polarimetry
Authors: Daniel C. M. Palumbo, George N. Wong, Andrew Chael, Michael D. Johnson
Figure caption: Phases of the time-averaged ﹩{\breve{\beta }}_{2}﹩ for the M87* and Sgr A* simulations sampled along the u and v axes in the Fourier domain, along with the time-averaged image-domain 230 GHz decomposed phases from the simulation, unscattered in the Sgr A* case. In the M87* simulation, the u axis is nearly aligned with the jet, whereas in the Sgr A* simulation, u is aligned with the line of nodes, so any “jet” would be aligned with v. Observations of each snapshot are computed without thermal noise, assuming known right–left gain ratios and leakage terms albeit with unknown absolute amplitude or phase calibration; values of ﹩\breve{e}﹩ and ﹩\breve{b}﹩ are then each averaged to produce the mean ﹩{\breve{\beta }}_{2}﹩. Increasing frequency is most impactful in pushing the indirect image-dominated regime to the left, near 15 Gλ at 690 GHz. Dashed green lines show the Earth-diameter baseline at each frequency, while solid magenta lines show the geostationary orbital radius, which is dominated by the indirect image at all frequencies after averaging. The direct and indirect image values ﹩\angle {\breve{\beta }}_{2}﹩ are each nearly achromatic, suggesting that the emission region does not change significantly over frequency.
Paper: Demonstrating Photon Ring Existence with Single-baseline Polarimetry
Authors: Daniel C. M. Palumbo, George N. Wong, Andrew Chael, Michael D. Johnson
Figure caption: Spiral quotient phase for scattered snapshots of the same Sgr A* GRMHD fluid frame at four frequencies. The dashed green circle shows Earth-diameter baselines at each frequency. Images are scattered by the same (frequency-dependent) scattering screen looking toward the galactic center. Refractive scattering distributes diffuse polarization structure into higher spatial frequencies, outshining the photon ring phase at 230 GHz.