adsabs/AstroCLIMB huggingface dataset:
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Top three panels: Background-subtracted light curves for the 2024 X-ray campaign on MCG-6. From top to bottom: XRISM/Xtend (black, 0.3–12 keV), XMM/EPIC-pn (red, 0.3–12 keV), and NuSTAR/FPMA+FPMB (blue, 3–78 keV). All are shown at a time resolution of 2048 s per bin. Bottom three panels: Hardness ratio versus time for the Xtend (black circles; top), pn (red triangles; middle) and NuSTAR/FPMB (blue squares; bottom) instruments. The HR is calculated by dividing the background-subtracted light curves in the hard and soft bands (H = 2–10 keV for Xtend and pn, 10–50 keV for FPMB; S = 0.5–2 keV for Xtend and pn, 3–10 keV for FPMB). The Xtend and pn HRs have time bins of 512 s, while the FPMB is binned to 2048 s for clarity. Note the green vertical lines marking dips in the light curves that correspond to spikes in the HRs.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Left: The XRISM/Resolve data fit with a simple photoabsorbed power-law model. Note the broad and narrow residuals that are apparent in emission and absorption in the Fe K band. Right: Residuals to the best-fit model for the broadband data (including reflection), refit to the Resolve spectrum. Narrow residuals remain in the Fe K band, indicating the presence of highly ionized gas, particularly in absorption. Because we use Cash statistics to evaluate the goodness of fit, error is calculated as the square root of the model-predicted number of counts.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Top: Best-fit broadband model to the 0.5–55 keV CCD data (total model is in black). The model consists of a three-zone warm absorber modifying a coronal continuum via nthcomp (plotted in gray, separately from the relxilllpCp component for clarity), distant torus reflection via MYtorus (orange; only the line component),and inner disk reflection via relxilllpCp (magenta). Bottom: Ratio of the best-fit broadband model to the data. XRISM/Xtend is in black, XMM/pn is in red, NuSTAR/FPMA is in dark blue, and NuSTAR/FPMB is in light blue.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Left: Time-averaged XRISM/Resolve data (black) and background (red), both from the full array (minus pixels 12 and 27). The background is negligible in this observation. Right: Data divided by detector area for Resolve (black), Xtend (red), XMM/pn (green), and NuSTAR/FPMB (blue). The offsets between detectors are indicative of current calibration differences. No model is applied, but the data points are connected for visual clarity.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Top: Best-fit model to the 2–11 keV XRISM/Resolve data (total model is in black). The model consists of a three-zone low-ionization warm absorber (two gas zones, one dust zone) plus a two-zone high-ionization wind modifying the continuum (gray), distant torus reflection via MYtorus (orange), and inner disk reflection via relxilllpCp (magenta). Fe XXV and Fe XXVI emission lines are also included (blue). Bottom: Ratio of the best-fit model to the data. All remaining features are <3σ.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Left: Broadband data-to-model ratio showing the poor fit of the disk-wind model of G. A. Matzeu et al. (2022) to the joint data set. For visual clarity, only the XMM/pn (red points) and NuSTAR/FPMB data (blue points) are shown. The model is clearly inadequate in the Fe K band and ≥10 keV. Right: Zoom-in of the disk-wind model fit to the Resolve data, which are shown as ratio to a power law as in Figure 7 (black points). The model fit begins to worsen ≥7 keV, coincident with where the blue wing of the broad Fe Kα line from relativistic reflection would appear. The blue hashed vertical lines show, from left to right, the rest-frame positions of the Fe Kα, Fe XXV, and Fe XXVI features in emission and/or absorption.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Top: Best-fit model to the joint analysis of the Resolve, Xtend, pn, FPMA, and FPMB data from 0.5–55 keV. Mean and 1σ-confidence intervals for each of the model’s components derived from the MCMC are shown, estimated from 10,000 realizations of the spectrum drawn from the MCMC posteriors. The model consists of a three-zone low-ionization warm absorber (two gas zones, one dust zone) plus a two-zone high-ionization wind modifying the continuum, distant torus reflection via MYtorus, and inner disk reflection via relxilllpCp. Fe XXV and Fe XXVI emission lines, likely re-emission from the outflowing wind, are also detected. Bottom: Ratio of the best-fit joint model to the data. XRISM/Resolve is in black, XRISM/Xtend is in red, XMM/pn is in green, NuSTAR/FPMA is in dark blue, and NuSTAR/FPMB is in light blue.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Comparison of the Resolve data in the narrow Fe Kα line region (black points) fit with a single Gaussian component (left) versus the MYtorus model (right). MYtorus fits the Resolve data slightly better. The total model is shown in red and the narrow Fe Kα line contribution in blue. Data-to-model ratios are shown in the bottom panel of each plot.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Corner plot showing the posterior distributions for the free parameters in the relxilllpCp inner disk reflection component of the best-fitting model for the joint fit to the Resolve, Xtend, pn, FPMA, and FPMB data. Single parameter distributions are shown on the ends (y-axes show probability density), as well as plots showing the 1σ, 2σ, and 3σ contours for the posterior distributions of parameter pairs.
Paper: A Sharper View of the X-Ray Spectrum of MCG–6-30-15 with XRISM, XMM-Newton, and NuSTAR
Authors: Laura W. Brenneman, Daniel R. Wilkins, Anna Ogorzałek, Daniele Rogantini, Andrew C. Fabian, Javier A. García, Anna Juráňová, Misaki Mizumoto, Hirofumi Noda, Ehud Behar, Rozenn Boissay-Malaquin, Matteo Guainazzi, Takashi Okajima, Erika Hoffman, Noa Keshet, Jelle Kaastra, Erin Kara, Makoto Yamauchi
Figure caption: Zoom-in of Figure 12 (top) showing the Fe K band with the mean and 1σ-confidence intervals for each of the components of the best-fit model derived from the MCMC.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Direct flight ΔV values as a function of launch date for trajectories to 3I/ATLAS from Earth. The color of each point corresponds to the flight time of the mission. The upper and lower panels show direct flight ΔV values from 2025 January 1–2026 March 31, and May 1–2025 November 2, respectively. The minimum postdiscovery ΔV trajectory is 24.0 km s−1 (C 3 = 576 km2 s −2) on 2025 July 1 with a flight time of 137 days. Prediscovery trajectories may have been feasible, requiring ΔV ∼ 7 km s−1 with a flight time of ∼250 days. The shaded region on the upper panel is the region shown in the lower panel.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Similar to Figure 1, but for trajectories to 3I/ATLAS from Mars. Here, the shaded inset region is from 2025 July 1 to 2025 September 25. The minimum energy trajectory for a postdiscovery mission would be launched on 2025 July 1 with a flight time of 94 days and require ΔV = 3.54 km s−1. Prediscovery trajectories would have required ΔV ∼ 3 km s−1 (C3 = 12.5 km2 s−2) with flight times of more than 200 days.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: The orbit of a postdiscovery minimum ΔV mission to 3I/ATLAS sent on 2025 July 1 from the Earth. The spacecraft would encounter 3I/ATLAS on 2025 November 15 and would require ΔV = 24 km s−1. The trajectory for 3I/ATLAS, Earth, and the spacecraft are plotted in purple, blue, and gray, respectively. Markers represent departure location and flyby location, and arrows show the direction of each orbit/trajectory. Points on each trajectory indicate the positions of each object every 30 days.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Similar to Figure 3, except for a minimum ΔV mission to 3I/ATLAS postdiscovery, sent on 2025 July 1 from Mars. This hypothetical trajectory requires a ΔV ∼ 4 km s−1 and a time of flight of 94 days.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Similar to Figure 3, except for a minimum-energy mission to 3I/ATLAS sent from Mars on 2025 August 10. Such a mission would require a ΔV ∼ 6.5 km s−1 and performs a flyby on 2025 October 4 with a time of flight of 54 days.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Mission design contour displaying required ΔV (0–100 km s−1) across Earth departure and 3I/ATLAS arrival dates. The green circles indicates the minimum ΔV on the discovery date, 2025 July 1.
Paper: The Feasibility of a Spacecraft Flyby with the Third Interstellar Object 3I/ATLAS from Earth or Mars
Authors: Atsuhiro Yaginuma, Tessa Frincke, Darryl Z. Seligman, Kathleen Mandt, Daniella N. DellaGiustina, Eloy Peña-Asensio, Aster G. Taylor, Michael C. Nolan
Figure caption: Similar to Figure 2, but from Mars in this case.
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: Temporal correlation results between (a) IBEX Ribbon ENA fluxes at 1.11 keV (D. J. McComas et al. 2024) and (b) the solar wind (SW) dynamic pressure derived from IPS data (C. Porowski et al. 2022) for the southern Ribbon section. (c) The mean correlation curve is shown in black. The peak correlation coefficient is 0.76 (shown as a pink dot), with a corresponding lag time of 3.57 ± 1.0 yr. Ten samples of block bootstrap curves out of 10,000 are shown in color, which are used to calculate the uncertainty of the lag time (i.e., the total time delay). The red dots in panel (b) show the solar wind dynamic pressure, corresponding to the lag time of the black curve in panel (c).
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: Example diagram of the block bootstrap method. Here we assume there are a total of nine data points for illustration purposes. The original data are the IBEX fluxes shown in Figures 5(a) or 6(a), and each data point here stands for 1 yr of IBEX data (which has two points in time: one for ram and another for antiram measurements). Each resample takes a random selection of 3 yr blocks, and then we sort before calculating the correlation curve and the maximum correlation coefficient. This is repeated N times.
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: ENA map at 1.11 keV showing regions of interest. The regions are defined by the magenta lines, labeled “North” and “South.” Each region contains 24 pixels of IBEX data.
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: Same as Figure 3 but for the northern section of the Ribbon. The peak correlation coefficient is 0.76, with a corresponding lag time of 5.66 ± 0.78 yr.
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: IPS-derived solar wind speeds in the northern (blue) and southern (red) sections of the Ribbon. Note that the solar wind speed in the north was averaged over latitudes between 15° and 45°, while in the south the speed was averaged over latitudes between −39° and −21°.
Paper: Distance to the IBEX Ribbon beyond the Heliopause
Authors: E. J. Zirnstein, M. A. Dayeh
Figure caption: IBEX Ribbon-separated “median” maps from D. J. McComas et al. (2024) at 1.11 keV. Pixels in gray have no Ribbon flux.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Analytical fit of the characteristic photon energy that sets the wind base, for the same sample of planets shown in Figure B1 and B2.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: Light curve plots for Mrk 1048 and Mrk 618. The upper panel shows a photometric g-band continuum with labeled data points from each telescope. The middle left and lower left panels display Hβ and Hα emission-line fluxes in arbitrary units, with g-band continuum overlaid. These are mean-subtracted light curves and are matched by normalizing the g-band continuum light curve and shifting the emission-line light curves to the final adopted lag values mentioned in Table 3. The JAVELIN modeling for each light curve is shown in steel blue. For the Hα light curve, we have smoothed it with five consecutive points using the running average method. The upper and lower right panels show the lag histograms from ICCF (teal) and JAVELIN (violet). These plots display the CCF value rvalue on the left (pink) and the probability density (N) of the histograms on the right. The darker pink region of the rvalue curve depicts 80% of the centroid peak that is used to calculate the final ICCF lag. The dashed lines indicate the lags with 16th and 84th percentiles of the lag probability density.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: The Hβ (left) and Hα (right) emission-line plots are shown along with their residuals after fitting for Mrk 1048. The broad component fitting with a double Gaussian is in green, whereas the narrow component fitting is shown in orange. The total line model is overplotted on the original continuum-subtracted spectrum. The Hα emission-line fittings have decomposed the [N II] λ6549, [N II] λ6585, and narrow Hα components.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: The composite spectra from ADFOSC (left) and TANSPEC (right) of Mrk 1048 (top) and Mrk 618 (bottom). The emission-line regions, such as Hγ, Hβ, and Hα, with narrow emission lines [O III] are highlighted.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: The mean and rms spectra for Mrk 1048 (left) and Mrk 618 (right). The solid lines indicate the original spectrum, while the dotted lines are the continuum-subtracted spectrum.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: V-band image of Mrk 1048 and Mrk 618 observed from the HFOSC/HCT with a field of view of ﹩10{\rm{^{\prime} }}\times 10{\rm{^{\prime} }}﹩. The sources are marked, and the nearby comparison stars are shown.
Paper: Spectroscopic Reverberation Mapping for SARM: The Case of Mrk 1048 and Mrk 618
Authors: Shivangi Pandey, Suvendu Rakshit, S. Muneer, Jincen Jose, Ashutosh Tomar, Yan-Rong Li, Jian-Min Wang, C. S. Stalin, Jong-Hak Woo, Romain G. Petrov, James Leftley, Sebastian F. Hönig, Amit Kumar Mandal, Tushar Ubarhande, Shu Wang, Michael Brotherton, Archana Gupta
Figure caption: We simulated light curves for the g-band continuum and the Hβ and Hα emission lines with 1000 independent realizations each. The figure shows the probability distribution of the ratio between the recovered lag and the input ICCF lag (11 days) for the case of the g band versus Hβ for Mrk 1048 with the ICCF method. The quoted median of the distribution is close to unity, indicating that the observed sampling and noise levels are sufficient to recover the intrinsic lag reliably.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Temporal and azimuthal averages of gas density (left half of each panel) and fluid-frame radiation energy density (right half of each panel) for six different models, spanning different accretion rates and black hole spins. Blue streamlines in the left panels trace the magnetic field, while green streamlines in the right panels indicate coordinate-frame radiation flux. The disk body is enclosed by blue dashed lines, marking the contour of zero Bernoulli parameter. Gray solid lines denote the scattering photosphere, and orange dashed lines outline the jet region. Note that no orange dashed lines appear in the two models in the right column (i.e., E07-a3-DL and E09-a3-DL), as these do not form a steady jet.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Radial profiles of (from top to bottom) surface density and midplane angular frequency normalized by the Keplerian value, midplane pressures, disk-averaged stresses, and various timescales. Gray shading denotes the plunging region inside the ISCO. Each column shows the results from a different accretion regime (models E88-a3, E9-a3, and E08-a3). These models all have the same spin (a = 0.3) and are initialized with a single-loop magnetic field configuration.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Poloidal slices of the mass density in radiation-dominated disks with the same spin and roughly the same mass accretion rate, but different initial magnetic field geometries. The left and right columns show models that begin with a double-loop configuration (no vertical magnetic flux at the midplane initially), while the middle column shows a model with a single-loop configuration. From left to right, the models shown are E07-a3-DL, E08-a3, and E09-a3-DL. The bottom row is a zoom-in to the inner regions. Each model is shown at t = 60000rg/c.