adsabs/AstroCLIMB huggingface dataset:
Paper: Typhon: A Polar Stream from the Outer Halo Raining through the Solar Neighborhood
Authors: Wassim Tenachi, Pierre-Antoine Oria, Rodrigo Ibata, Benoit Famaey, Zhen Yuan, Anke Arentsen, Nicolas Martin, Akshara Viswanathan
Figure caption: Trajectories of the sample members of Typhon during a 5  Gyr backward integration in the McMillan (2017) potential in Galactic Cartesian coordinates. Trajectories of the seven stars whose metallicity is available through LAMOST DR8 (Wang et al. 2022) are colored in yellow.
Paper: A Robust Test of the Existence of Primordial Black Holes in Galactic Dark Matter Halos
Authors: Marek Abramowicz, Michał Bejger, Andrzej Udalski, Maciek Wielgus
Figure caption: Absolute number of LBHs in a model galaxy of 13 Gyr age as a function of M PBH and ξ. Majority of LBHs are created in the galactic bulge. The continuous lines correspond to the total integrated number of LBHs in the galaxy, while the dashed lines represent the LBHs created in the galactic disk. If one fixes ξ and assumes M PBH to be n times smaller, then there is necessarily n times more PBHs flying around, so it is n times easier for a PBH to collide with an NS. Thus, there is about n times more LBHs formed. Therefore, in the regime N NS ≫ N LBH we have the ﹩{N}_{\mathrm{LBH}}\propto {M}_{\mathrm{PBH}}^{-1}﹩ scaling.
Paper: Atomic Gas Dominates the Baryonic Mass of Star-forming Galaxies at z ≈ 1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The stellar-mass distributions of the galaxies in the three redshift intervals. Panel (A) shows the stellar-mass distributions of the blue galaxies of the xGASS sample (blue histogram; Catinella et al. 2018) and those of the xCOLD GASS sample (green histogram; Saintonge et al. 2017). Panels (B) and (C) show the stellar-mass distributions of the GMRT-CATz1 subsamples at z = 0.74–1.25 and z = 1.25–1.45 (blue histograms; C22a). All average quantities reported in this work, for the three subsamples at z ≈ 0, z ≈ 1.0, and z ≈ 1.3, were computed with weights such that the stellar-mass distribution of each subsample is identical to that of the subsample at z = 1.25–1.45 (the orange histogram in each panel). The number of galaxies in each subsample is listed in each panel.
Paper: Atomic Gas Dominates the Baryonic Mass of Star-forming Galaxies at z ≈ 1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The ratio of the average atomic gas mass to the average molecular gas mass in stellar-mass-matched samples of star-forming galaxies at z ≈ 0, z ≈ 1.0, and z ≈ 1.3. The blue circle shows the estimated value of 〈M Atom〉/〈M Mol〉   in star-forming galaxies at z ≈ 0 (Saintonge et al. 2017; Catinella et al. 2018). The red squares show estimates of 〈M Atom〉/〈M Mol〉  in star-forming galaxies at two redshift intervals z = 0.74–1.25 and z = 1.25–1.45. The error bars along the y-axis show the 68.3% confidence intervals on 〈M Atom〉/〈M Mol 〉. The dashed line indicates 〈M Atom〉/〈M Mol〉 = 1 It is clear that the average atomic gas mass in star-forming galaxies is higher than the average molecular gas mass over the past 9 Gyr.
Paper: Atomic Gas Dominates the Baryonic Mass of Star-forming Galaxies at z ≈ 1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift evolution of (A) the ratios of the average atomic gas mass and the average molecular gas mass to the average stellar mass, and (B) the ratios of the average atomic gas mass, the average molecular gas mass, and the average stellar mass to the average baryonic mass. In both panels, all plotted values are for stellar-mass-matched samples of galaxies with 〈M ⋆〉 ≈ 1010 M ⊙ at z ≈ 0, z ≈ 1.0, and z ≈ 1.3. The error bars along the y-axis show the 1σ uncertainties in the estimates. See the text for discussion.
Paper: Atomic Gas Dominates the Baryonic Mass of Star-forming Galaxies at z ≈ 1.3
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The stacked HI 21 cm  spectra of blue star-forming galaxies at z = 0.74–1.25 (left panel) and z = 1.25–1.45 (right panel) from C22b. The stacked HI 21 cm  spectrum of each panel was obtained by stacking the individual HI 21 cm  spectra of the galaxies in the subsample, using weights to ensure that the stellar-mass distributions of the two subsamples are identical. The dashed curve in each panel shows the 1σ rms noise error on each 90 km s−1 velocity channel of the stacked HI 21 cm  spectrum.
Paper: Hubble Space Telescope Imaging Reveals That SN 2015bh Is Much Fainter than Its Progenitor
Authors: Jacob E. Jencson, David J. Sand, Jennifer E. Andrews, Nathan Smith, Jay Strader, Mojgan Aghakhanloo, Jeniveve Pearson, Stefano Valenti
Figure caption: HST imaging of the site of SN 2015bh. In the top row, we show a sequence of available F814W imaging, where the instrument and date of each image are indicated at the top of each panel and the location of SN 2015bh indicated by the white crosshairs. The first three panels from the left in the bottom row show the same sequence in F555W. All of these panels are oriented N up and E left and are 4″ on a side. The bottom, rightmost panel shows a zoom-in to a 5 pixel (0.″25) box around SN 2015bh (indicated by the orange square in the upper, rightmost panel) in the 2019 F814W image. The 1σ confidence regions on the position of SN 2015bh measured from the 2017 F814W and F555W images are shown as the red solid ellipse and yellow dashed ellipse, respectively (see Appendix C). The position of the source detected by DOLPHOT in the 2019 F814W image, indicated by the white cross, is consistent with both measurements of the position of SN 2015bh.
Paper: Discovery of γ-Ray Pulsations from PSR J1835–3259B in the Globular Cluster NGC 6652
Authors: Pengfei Zhang, Yi Xing, Zhongxiang Wang
Figure caption:  γ-ray spectrum at 0.1–500 GeV obtained from the data for NGC 6652. The best-fit LP and PLEC models are shown as yellow dashed and blue solid lines respectively. The error range of the latter is also shown as the light blue region. A testing PLEC4 model is shown as the red dashed–dotted line (see Section 2.2).
Paper: A 2D Model for Coronal Bright Points: Association with Spicules, UV Bursts, Surges, and EUV Coronal Jets
Authors: D. Nóbrega-Siverio, F. Moreno-Insertis
Figure caption: Initial condition. Top: average stratification for the temperature and density. Bottom: imposed magnetic field configuration indicating some of its major features following the terminology used in 3D null points (Priest & Titov 1996). Red circle: region with B < 1 G centered on the null point, (x 0, z 0) = (32, 8) Mm. Gray dashed line: solar surface at z = 0.
Paper: A 2D Model for Coronal Bright Points: Association with Spicules, UV Bursts, Surges, and EUV Coronal Jets
Authors: D. Nóbrega-Siverio, F. Moreno-Insertis
Figure caption: Chromospheric analysis. Left: spacetime maps for . Right: corresponding density . Dashed lines: CBP’s main polarities (see also Figure 3). Red solid lines: fan surface at z = 1.5 Mm in the main stage.
Paper: Solar Chromospheric Network as a Source for Solar Wind Switchbacks
Authors: Jeongwoo Lee, Vasyl Yurchyshyn, Haimin Wang, Xu Yang, Wenda Cao, Juan Carlos Martínez Oliveros
Figure caption: EUV images of SDO/AIA and Hα images of GST/VIS. (a) SDO/AIA 193 Å image of the northern coronal hole on 2020 June 17 17:21:10UT, with the FOV outlined by a white box. (b) The AIA 171 Å image in the ROI. (c) GST/VIS Hα image overlaid with an HMI magnetic field (red/blue contours in the levels of ±30 G). (d) Hα–0.8 Å image overlaid with Hα+0.8 Å image (red contours). (e) Hα+0.8 Å image with contours.
Paper: Solar Chromospheric Network as a Source for Solar Wind Switchbacks
Authors: Jeongwoo Lee, Vasyl Yurchyshyn, Haimin Wang, Xu Yang, Wenda Cao, Juan Carlos Martínez Oliveros
Figure caption: Proposed hypothesis for the transformation of solar flux tubes into SBs in space. (a) An inverted Hα image showing three SGs (marked with dotted lines) and two hypothetical trajectories of PSP (red arrows). (b) Flux tubes (represented by lines) rooted along the network boundary expand into space. (c) Flux tubes are allowed to randomly walk to fill up the magnetic funnel yet rooted along the network boundary. (d) Locations of flux tubes on the x–y plane at the height of PSP are plotted (colored dots) together with the trajectory of the network boundary (white curve). (e) Proposed transformation of a flux tube to an SB: initially a straight flux tube (green) with a dense section (red) turns itself over to form an S-shaped kink with the aspect ratio as high as that of the dense section.
Paper: Solar Chromospheric Network as a Source for Solar Wind Switchbacks
Authors: Jeongwoo Lee, Vasyl Yurchyshyn, Haimin Wang, Xu Yang, Wenda Cao, Juan Carlos Martínez Oliveros
Figure caption: Geometrical parameters of flux tubes on SG boundary. The panels in the left-hand side show the lengths (widths) of flux tubes marked with red (white) bars in an inverted Hα image (a), histograms of length (b) and width (c) of flux tubes, and interdistances between nearby flux tubes (d), and those between all pairs of flux tubes (e). The panels in the right-hand side (f)–(j) are the same as (a)–(e) for a different time frame.
Paper: Solar Chromospheric Network as a Source for Solar Wind Switchbacks
Authors: Jeongwoo Lee, Vasyl Yurchyshyn, Haimin Wang, Xu Yang, Wenda Cao, Juan Carlos Martínez Oliveros
Figure caption: Distributions of geometrical parameters. Scatterplots of (a) length of flux tubes vs. their widths and (b) interdistance between nearby flux tubes vs. widths. Middle column shows the histograms of length of the dark section of flux tubes (c) and the interdistance of all pairs of flux tubes (d). Right column shows the measured length-to-diameter ratio of flux tubes (e) and a model aspect ratio (f). The model calculation of the aspect ratio starts with the nominal initial value of one in the Sun and traces its evolution through its transit to space under four combinations of assumptions on the radial and lateral expansion.
Paper: The Discovery of the 528.6 Hz Accreting Millisecond X-Ray Pulsar MAXI J1816–195
Authors: Peter Bult, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Jérôme Chenevez, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Giulio C. Mancuso, Christian Malacaria, Mason Ng, Andrea Sanna, Tod E. Strohmayer, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Outburst evolution of MAXI J1816 relative to 2022 June 7 (MJD 59737). The top panel shows the 0.5–10 keV count-rate as a function of time, with each point representing a single NICER pointing. The X-ray bursts have been removed from this data, but their onset times are marked with red crosses. The second panel shows the fractional pulse amplitude in the 0.5–10 keV range using triangles to indicate the 95% upper limits for nondetections. Finally, the two bottom panels give the phase residuals relative to a constant frequency and flux-bias adjusted timing model (see Table 1).
Paper: The Discovery of the 528.6 Hz Accreting Millisecond X-Ray Pulsar MAXI J1816–195
Authors: Peter Bult, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Jérôme Chenevez, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Giulio C. Mancuso, Christian Malacaria, Mason Ng, Andrea Sanna, Tod E. Strohmayer, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Light curves of the 15 X-ray bursts observed from MAXI J1816. These light curves are calculated in the 0.5–10 keV energy range at 1 s resolution, with the preburst count-rate subtracted. In each panel a different subset of the bursts are highlighted in color (with the burst number as in Table 2), while the remaining bursts are shown in gray for comparison.
Paper: The Discovery of the 528.6 Hz Accreting Millisecond X-Ray Pulsar MAXI J1816–195
Authors: Peter Bult, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Jérôme Chenevez, Elizabeth C. Ferrara, Keith C. Gendreau, Sebastien Guillot, Tolga Güver, Wataru Iwakiri, Gaurava K. Jaisawal, Giulio C. Mancuso, Christian Malacaria, Mason Ng, Andrea Sanna, Tod E. Strohmayer, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Mass–radius relation of the companion star from the binary ephemeris (solid line) compared to the theoretical mass–radius relation of a zero-age main-sequence star (dotted line).
Paper: MIGHTEE-HI: Evolution of HI Scaling Relations of Star-forming Galaxies at z < 0.5 
Authors: Francesco Sinigaglia, Giulia Rodighiero, Ed Elson, Mattia Vaccari, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Tom Oosterloo, Romeel Davé, Mara Salvato, Maarten Baes, Sabine Bellstedt, Laura Bisigello, Jordan D. Collier, Robin H. W. Cook, Luke J. M. Davies, Jacinta Delhaize, Simon P. Driver, Caroline Foster, Sushma Kurapati, Claudia del P. Lagos, Christopher Lidman, Pavel E. Mancera Piña, Martin J. Meyer, K. Moses Mogotsi, Hengxing Pan, Anastasia A. Ponomareva, Isabella Prandoni, Sambatriniaina H. A. Rajohnson, Aaron S. G. Robotham, Mario G. Santos, Srikrishna Sekhar, Kristine Spekkens, Jessica E. Thorne, Jan M. van der Hulst, O. Ivy Wong
Figure caption: Star-forming galaxy H I scaling relations: ﹩{\mathrm{log}}_{10}({M}_{{\rm{H}}\,{\rm\small{I}}})\mbox{--}{\mathrm{log}}_{10}({M}_{* })﹩ (top left), ﹩{\mathrm{log}}_{10}({f}_{{\rm{H}}\,{\rm\small{I}}})\mbox{--}{\mathrm{log}}_{10}({M}_{* })﹩ (top right), ﹩{\mathrm{log}}_{10}({M}_{{\rm{H}}\,{\rm\small{I}}})\mbox{--}{\mathrm{log}}_{10}(\mathrm{SFR})﹩ (bottom left), and ﹩{\mathrm{log}}_{10}({f}_{{\rm{H}}\,{\rm\small{I}}})\mbox{--}{\mathrm{log}}_{10}(\mathrm{sSFR})﹩. Our H I-stacking results at median redshift z ∼ 0.37 are displayed as red squares. Uncertainties on red squares along the x-axis, not shown for the sake of clarity of visualization, correspond to the width of the bins. The red dashed line represents the fit to our data. Our reference results at z ∼ 0 (G21, Guo et al. 2021) are plotted as a blue solid line. Green dotted and yellow dashed‒dotted lines show the predictions of the SIMBA cosmological hydrodynamic simulation at z = 0 and z = 0.4, respectively, for comparison. Shaded regions indicate 1σ uncertainties.
Paper: MIGHTEE-HI: Evolution of HI Scaling Relations of Star-forming Galaxies at z < 0.5 
Authors: Francesco Sinigaglia, Giulia Rodighiero, Ed Elson, Mattia Vaccari, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Tom Oosterloo, Romeel Davé, Mara Salvato, Maarten Baes, Sabine Bellstedt, Laura Bisigello, Jordan D. Collier, Robin H. W. Cook, Luke J. M. Davies, Jacinta Delhaize, Simon P. Driver, Caroline Foster, Sushma Kurapati, Claudia del P. Lagos, Christopher Lidman, Pavel E. Mancera Piña, Martin J. Meyer, K. Moses Mogotsi, Hengxing Pan, Anastasia A. Ponomareva, Isabella Prandoni, Sambatriniaina H. A. Rajohnson, Aaron S. G. Robotham, Mario G. Santos, Srikrishna Sekhar, Kristine Spekkens, Jessica E. Thorne, Jan M. van der Hulst, O. Ivy Wong
Figure caption: Stacked M H I spectra obtained in different intervals of M * (top row), SFR (mid row), and sSFR (bottom row). The title of each panel indicates the corresponding interval of galaxy properties. Lines and colors follow the same scheme as Figure 2.
Paper: MIGHTEE-HI: Evolution of HI Scaling Relations of Star-forming Galaxies at z < 0.5 
Authors: Francesco Sinigaglia, Giulia Rodighiero, Ed Elson, Mattia Vaccari, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Tom Oosterloo, Romeel Davé, Mara Salvato, Maarten Baes, Sabine Bellstedt, Laura Bisigello, Jordan D. Collier, Robin H. W. Cook, Luke J. M. Davies, Jacinta Delhaize, Simon P. Driver, Caroline Foster, Sushma Kurapati, Claudia del P. Lagos, Christopher Lidman, Pavel E. Mancera Piña, Martin J. Meyer, K. Moses Mogotsi, Hengxing Pan, Anastasia A. Ponomareva, Isabella Prandoni, Sambatriniaina H. A. Rajohnson, Aaron S. G. Robotham, Mario G. Santos, Srikrishna Sekhar, Kristine Spekkens, Jessica E. Thorne, Jan M. van der Hulst, O. Ivy Wong
Figure caption: Stacked M H I spectrum obtained in the full 0.23 < z < 0.49 redshift range we investigate in this paper. The blue solid line and the blue shaded region show the stacked spectrum and the associated jackknife uncertainties, respectively. The orange solid line and the gray shaded area indicate the reference spectrum (see text) and σ rms, respectively. The red dashed and dashed‒dotted horizontal lines mark the 3σ rms and 5σ rms noise levels, respectively. The green vertical line shows the velocity integration limits in the M H I computation.
Paper: Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4
Authors: Marta De Simone, Cecilia Ceccarelli, Claudio Codella, Brian E. Svoboda, Claire J. Chandler, Mathilde Bouvier, Satoshi Yamamoto, Nami Sakai, Yao-Lun Yang, Paola Caselli, Bertrand Lefloch, Hauyu Baobab Liu, Ana López-Sepulcre, Laurent Loinard, Jaime E. Pineda, Leonardo Testi
Figure caption: Top panels: NH3 velocity-integrated maps (from −30 to +45 km s−1 with respect to the v sys to include all the hyperfine components) toward IRAS 4A1, 4A2, and 4B in color scale starting from 3σ, with green first contour and steps of 3σ (σ = 4.4 mJy beam−1), overlapped with the continuum in white contours (from 50σ with steps of 100σ). Bottom panels: CH3OH velocity-integrated maps toward IRAS 4B (from −2 to +2 km s−1 with respect to the v sys) in color scale starting from 3σ, with green first contour and steps of 3σ (σ = 1.6 mJy beam−1 km s−1) overlapped with the continuum in white contours (from 50σ with steps of 100σ). The CH3OH maps for 4A1 and 4A2 are reported in De Simone et al. (2020). The stars mark the protostar positions. Synthesized beams are in the lower corners.
Paper: Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4
Authors: Marta De Simone, Cecilia Ceccarelli, Claudio Codella, Brian E. Svoboda, Claire J. Chandler, Mathilde Bouvier, Satoshi Yamamoto, Nami Sakai, Yao-Lun Yang, Paola Caselli, Bertrand Lefloch, Hauyu Baobab Liu, Ana López-Sepulcre, Laurent Loinard, Jaime E. Pineda, Leonardo Testi
Figure caption: Theoretical predictions of NH3/CH3OH abundance ratio vs. the precollapse dust temperature at different timescales (time = (0.1, 0.3, 1, 3)105 yr, in panels (a), (b), (c), and (d), respectively) and H2 density (n                         ﹩{}_{{{\rm{H}}}_{2}}=(0.1,1,10){10}^{5}﹩ cm−3, in red, magenta, and blue respectively), obtained with the GRAINOBLE code. Blue, gray, and orange bands represent the NH3/CH3OH values derived from the LVG analysis in 4A2, 4B, and 4A1, respectively.
Paper: Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4
Authors: Marta De Simone, Cecilia Ceccarelli, Claudio Codella, Brian E. Svoboda, Claire J. Chandler, Mathilde Bouvier, Satoshi Yamamoto, Nami Sakai, Yao-Lun Yang, Paola Caselli, Bertrand Lefloch, Hauyu Baobab Liu, Ana López-Sepulcre, Laurent Loinard, Jaime E. Pineda, Leonardo Testi
Figure caption: Scheme of the interplay between the gas phase and grain surface chemistry for the NH3 formation (adapted from Tinacci et al. 2022b). The release of H, N, N2, and NH3 into the gas phase is regulated by their respective binding energies. BE stands for binding energy.
Paper: Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4
Authors: Marta De Simone, Cecilia Ceccarelli, Claudio Codella, Brian E. Svoboda, Claire J. Chandler, Mathilde Bouvier, Satoshi Yamamoto, Nami Sakai, Yao-Lun Yang, Paola Caselli, Bertrand Lefloch, Hauyu Baobab Liu, Ana López-Sepulcre, Laurent Loinard, Jaime E. Pineda, Leonardo Testi
Figure caption: Scheme of the CH3OH and NH3 line analysis performed to compute the NH3/CH3OH abundance ratio in the three protostars. The CH3OH lines at centimeter wavelengths (red flag) are the ones observed at 25 GHz with the VLA (this work). The CH3OH lines at millimeter wavelengths (blue flag) and its isotopologues CH3OHisot (green flag) are from Taquet et al. (2015) for 4A2 using CH3OHisot = 13CH3OH, and from Yang et al. (2021) for 4B using CH3OHisot = CH3 18OH. For 4A1 we do not have millimeter methanol detections. All the computations and predictions of column density N, temperature T, density n, and size θ are performed with a non-LTE LVG method.
Paper: Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4
Authors: Marta De Simone, Cecilia Ceccarelli, Claudio Codella, Brian E. Svoboda, Claire J. Chandler, Mathilde Bouvier, Satoshi Yamamoto, Nami Sakai, Yao-Lun Yang, Paola Caselli, Bertrand Lefloch, Hauyu Baobab Liu, Ana López-Sepulcre, Laurent Loinard, Jaime E. Pineda, Leonardo Testi
Figure caption: Left panels: NH3 lines (marked in each panel) detected toward the continuum peak of IRAS 4B (black), 4A1 (orange), and 4A2 (blue). The red curves show the best hyperfine fits. Right panel: CH3OH lines (marked on each spectrum) detected in the VLA K band toward 4B. The red curves show the best Gaussian fits. In all panels, each spectrum is shifted by 12 K from the previous one, the vertical dotted black lines report the v sys (6.7 km s−1), and the horizontal green dashed lines show the 3σ level.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: A transverse slice through density with magnetic field lines shown in black for our model with poloidal magnetic flux (RADPOL, left) and model with toroidal magnetic flux (RADTOR, right) right before enabling the radiation transport. While the RADTOR simulation forms a thin accretion disk with a constant scale height, the inner disk in the RADPOL simulation enters the MAD state, and accretion proceeds through nonaxisymmetric RTI modes.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: A transverse slice through RADPOL. The right hemisphere shows a zoom-in of the left hemisphere. The mesh-block boundaries are illustrated using white lines. Each mesh block has N  r  × N  θ  × N  ϕ  = 36 × 36 × 102 cells.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: The presence of a large-scale poloidal magnetic flux leads to the development of a two-phase medium: a low-density, thick, hot corona-like accretion flow with patches of cold gas floating through it (top row, model RADPOL) within r ≲ 20r  g . In contrast, in the absence of the poloidal magnetic flux the cold, thin flow extends down to the black hole (bottom row, model RADTOR). The three columns, from left to right, show vertical slices through the density, ion temperature, and electron temperature; the right hemispheres show zoom-ins on the left hemispheres. Magnetic field lines are shown in black, jet boundary in white (p mag = ρ c 2), and the last scattering surface in pink (τ es = 1, integrated in the vertical direction). In RADPOL, the accretion disk transitions into a magnetic-pressure-supported corona within r ≲ 20r  g , which decouples into a two-temperature plasma of hot, radiating, electrons and very hot, nonradiating, ions. Optically thick patches of cold gas, visible as high-density regions with τ es ≳ 1 within r ≲ 25r  g , cover a significant fraction of the surface area in the corona near the midplane. In RADTOR the plasma in the disk remains strongly coupled and optically thick. Even above the photosphere, the plasma is much colder than in RADPOL.