adsabs/AstroCLIMB huggingface dataset:
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Mean-versus-variance plots of the sorted (in ascending order) directional differential flux for Parker Spiral (PS), Earth Pointing (EP), North Pointing (NP), and Intermediate (IM) detectors of AL1-ASPEX-STEPS during the observational period from 2024 January to November . The vertical red dashed line in each panel represents the threshold value of the flux below which the fluxes are considered as the quiet time flux and beyond which the fluxes are considered to be associated with transient events. The threshold values are also mentioned. The corresponding energy range is written at the top of each panel.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral index values shown in each subplot for the PS (a)–(e), IM (f)–(j), EP (k)–(o), and NP (p)–(t) detectors of AL1-ASPEX-STEPS.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral indices value mentioned in each subplot for the Parker Spiral (PS) detector of AL1-ASPEX-STEPS.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral indices value mentioned in each subplot for North Pointing (NP) detector of AL1-ASPEX-STEPS.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral indices value mentioned in each subplot for the Intermediate (IM) detector of AL1-ASPEX-STEPS.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral indices value mentioned in each subplot for Earth pointing (EP) detector of AL1-ASPEX-STEPS.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of 3He/4He, Fe/O, and C/O ratios as measured by ULEIS/ACE in the energy range spanning from 0.1 to 1.2 MeV n−1. The pink shaded regions represent the same quiet periods that are analyzed using the ASPEX-STEPS data. The horizontal lines represent averaged abundances measured in different heliosphere particle populations—CIR abundance (G. M. Mason et al. 2008); 3He-rich or ISEP (G. Mason 2007; D. V. Reames 2021) events; GSEP (G. Mason 2007; D. V. Reames 2021) events; Solar Wind (SW) value (J. Geiss & G. Gloeckler 1998). Black dots in each subplot represent the average value of abundance ratios during quiet periods with 1σ error bar.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Direction cosines of the PS, IM, NP, and EP detectors in nominal configuration (panels (a)–(h)) and in rotated configuration (panels (i)–(p)) of AL1-ASPEX-STEPS. In plots (a)–(p), the blue dot and yellow dot represent the Earth and the Sun, respectively. Red and green arrows represent the directions of PS, IM, NP, and EP detectors in the XY- and XZ-planes of the GSE coordinate system, respectively. The length of an arrow is decided by the corresponding values of direction cosines.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral indices value mentioned in each subplot for the PS, IM, and NP detectors of AL1-ASPEX-STEPS during the rotated period.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Panels (a) and (b) are the time evolution of disk precession and tilt angles of the models T25a094HD (black), T25a094wSANE (yellow), T25a094sSANE (green), and T25a094nMAD (blue). The integration for the total angular momentum of the torus uses a criterion of ρ > 10−4. For comparison, we plot the evolutions of precession and tilt angles of model T25a094nMAD in the red solid line with a criterion of ρ > 10−2. The global disk tilt and precession angles use mass density-weighted averages integrated from 20 to 200 rg. Details on the notion of the models can be found in Table 1.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Distributions of time-averaged logarithmic density on the x–z-plane of the rapidly rotating BH model T25a094nMAD and nonrotating BH model T25a0nMAD with a = 0.9375 and a = 0 in panels (a) and (b), respectively. The streamlines in each panel are the time-averaged poloidal magnetic field lines. The time averaging range is from t = 14,000 to 15,000 M. The blue arrow in the zoomed-in part of panel (a) shows the BH spin direction.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Evolution and radial profiles of jet and disk precession and tilt angles. Panels (a) and (b) depict the time evolution of the precession and tilt angles for the disk (black) and the jet (red) for the strongly magnetized model T25a094nMAD. Panels (c) and (d) show the radial profiles of the disk’s precession and tilt angles for the model T25a094nMAD, with different colors indicating different averaging time ranges.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: 3D volume rendering of the jet (colored by magnetization σ) and accretion disk (colored by density ρ) in the strongly magnetized model T25a094nMADH, shown at two different time snapshots: (a) t = 3000 M and (b) t = 17,160 M. The retrograde precession of the jet–disk system is visible as a counterrotation to the BH spin axis (positive z-direction).
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: This figure presents the radial profiles of the ratio of the magnetic to LT precession rates, ∣ΩMag/ΩLT∣, for simulations (a) T25a094nMAD (left) and (b) T25a094wSANE (right). Each colored line depicts the time-averaged profile over the interval indicated in the legend. These profiles are calculated from the simulation data by averaging values within radially binned shells, where each bin spans eight cells in the radial direction.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Mass advection and radial spreading in the high-spin (a* = 0.9), high-resolution MAD simulation. As an illustrative case, the top panels track all particles crossing the radial shell 10 ≤ r < 10.5 GM/c2. Each trajectory is time shifted so that its passage through the shell is aligned, and the resulting histogram of radial positions as a function of time offset is shown in the top-left panel. The top-right panel displays the corresponding (unnormalized) radial distribution as it evolves with time. The ensemble of trajectories demonstrates that material in the MAD disk is subject to both rapid inward advection and strong radial mixing. The mean particle trajectory (solid white line, top panel) indicates a systematic inward drift consistent with the net advection rate, while the growing spread (dashed white lines) reflects the rate of radial mixing. This spreading occurs on timescales much shorter than the global accretion time, suggesting strong mixing in the flow. The inferred advection velocity vr = ur/ut (bottom left) is consistent over t = 15,000–40,000 GM/c3 (black line) and matches the radial velocity profile measured directly from the GRMHD fluid variables (bottom right, dashed black). Agreement between tracer-based and fluid-based measurements confirms that the tracer population reliably follows the mass flow. Advection rates cannot be measured at small radii because particles are no longer evolved after crossing the event horizon.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Rest-mass plasma density across simulations and times. Colors span logarithmically over 5 orders of magnitude and are normalized across the entire figure rather than per panel. Each panel shows a vertical slice through the rcyl–z plane, evaluated in Kerr–Schild coordinates. Top row: initial condition for the usual Fishbone–Moncrief torus with rin = 20 and ﹩{r}_{{\rm{\max }}}=41﹩ across five black hole spins of −0.9, −0.5, 0, 0.5, and 0.9, where negative numbers indicate that the plasma rotates counter to the spin of the central black hole. Notice that the size of the initial torus depends on the angular momentum of the central black hole, but the same fluid initial condition is used for both MAD and SANE configurations. Middle and bottom rows: zoomed-in representation of the time evolution of plasma, with lines showing the axisymmetrized magnetic field overplotted in black for a* = 0.9 MAD (middle) and SANE (bottom) simulations. The plasma is evaluated on an azimuthal slice. The leftmost panels show the initial condition at t = 0 GM/c3, and the subsequent columns show the simulation at times t = 25,000, 50,000, 75,000, and 100,000 GM/c3.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Comparison of accretion rates from GRMHD fluid variables (dark) and from tracer particles crossing the event horizon (light red) for representative high-spin a* = 0.9 MAD (top) and SANE (bottom) simulations at both 16/8 and 8/8 resolutions (see main text). For the higher-resolution runs, the tracer-based rate is sampled twice as frequently, while the fluid accretion rate is a summary statistic reported with the same output cadence across simulations. The close agreement between tracer- and fluid-based measurements confirms that the tracer population accurately captures the mass inflow and that the initial particle distribution was appropriately chosen to follow the fluid dynamics.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Evolution of tracer particles over time in the high-spin prograde a* = 0.9 MAD simulation. Each panel shows the positions of tracer particles within a narrow wedge about the midplane (∣z/r∣ ≤ 0.1), colored according to their cylindrical radius at the initial time. The white-filled circle at the origin marks the black hole event horizon. White rings overlaid on each panel indicate the initial radial boundaries between colored bins. As time progresses, the tracer population becomes increasingly mixed, demonstrating the radial redistribution of material as it is accreted toward the black hole.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Time evolution of density averaged MRI quality factors 〈Q(r,θ,ϕ)〉 for models T25a094wSANE, T25a094sSANE, T25a094nMAD, and T25a094nMADH are shown in panels (a) to (d), respectively. The black, blue, and red lines represent 〈Q(r)〉, 〈Q(θ)〉, and 〈Q(ϕ)〉, respectively.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Panels (a), (b), and (c) show the time evolutions of disk size, accretion rate, and scaled magnetic flux rate, respectively, for different models: T25a094HD (black), T25a094wSANE (yellow), T25a094sSANE (green), and T25a094nMAD (blue).
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Panels (a) and (c) display the mesh grid configuration with parameters lin_frac = 0.9 and smoothness = 0.02, corresponding to models T25a094nMAD and T25a094nMADH, respectively. In contrast, panel (b) shows the mesh grid used for the other MHD models, which employs lin_frac = 0.8 and smoothness = 0.03.
Paper: Magnetically Driven Retrograde Precession in Misaligned Black Hole Accretion Flows
Authors: Hong-Xuan Jiang, Yosuke Mizuno, Dong Lai, Indu K. Dihingia, Christian M. Fromm
Figure caption: Comparison of the disk precession angle ﹩{{ \mathcal P }}_{{\rm{disk}}}﹩ and tilt angle ﹩{{ \mathcal T }}_{{\rm{disk}}}﹩ from simulations T25a094nMAD (standard resolution) and T25a094nMADH (higher resolution).
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Evolution of the initial source location for matter accreting through the event horizon across simulations. Top: mean initial cylindrical radius rcyl of accreting material as a function of time for MAD (left) and SANE (right) models. In MADs, the mean source radius moves outward rapidly as the inner disk drains quickly; in SANEs, the shift is slower and more gradual. Bottom: instantaneous rate of change of the mean source radius, computed from the slopes of the curves in the top panels. MADs begin with steep slopes, reflecting rapid early draining, while SANEs evolve more slowly. All SANE models show a feature near t ≈ 20,000 GM/c3, corresponding to when accretion begins to tap the initial peak of the torus mass distribution (this behavior is seen across resolutions). Reference power-law scalings are overplotted: rcyl = 0.25 t2/3 for MADs and rcyl = 0.7 t1/2 for SANEs. The continued outward drift of the mean source radius reflects progressive depletion of the initial torus rather than a stationary inflow. Nonetheless, the well-defined draining trends in both MAD and SANE models enable a rough estimate of an effective inflow time as a function of radius, with MADs exhibiting systematically shorter timescales than SANEs at comparable radii.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Evolution of radial position for particles that pass through the radial bin 10.2 ≤ rcyl < 10.3 GM/c2, aligned such that t = 0 corresponds to that crossing. Data computed for the high-spin a* = 0.9 MAD simulation shown in Figure 4. Left: distribution of particle positions in cylindrical radius rcyl at time t0 = −5 GM/c3 (horizontal axis) compared to t1 = 5, 10, 15, 20 GM/c3 (vertical axis). The white-shaded band marks the kinematically allowed region for particles moving on ballistic trajectories between t0 and t1 while passing through the reference bin. The widening of the distribution beyond this band indicates the presence of mixing and turbulent dispersion beyond simple advection. Right panels: evolution of the distribution function over time relative to the distribution at t1 = 0 (blue; other colors at t1 = 5, 10, 15, 20 GM/c3) for three representative initial locations: rcyl = 10.25, 10.5, and 10.75 GM/c2 (corresponding to different vertical slices in the left panels). Each panel shows both coherent inward advection and broadening of the distribution function, indicating mixing over time.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Initial positions of matter accreting through the event horizon for high-spin a* = 0.9 MAD (top row) and SANE (bottom row) simulations. Each panel shows an azimuthal slice in Kerr–Schild coordinates, colored by a kernel density estimate (KDE) of all tracer particles that accrete within 1000 GM/c3 of the listed time. Light gray contours mark KDE levels at 0.1, 0.2, …, 0.9 of the maximum value. Black contours show the initial mass distribution, drawn at even logarithmic intervals from 1% to 100% of the maximum initial density. All values are integrated dϕ. Early accretion is dominated by particles within a narrow midplane wedge; over time, a larger fraction of the disk contributes. The MAD simulation shows broader, more radially extended source regions than the SANE simulation (the asymmetric behavior in the t = 50,000 GM/c3 panel is a random transient; see the next figure). The matter source in the SANE simulation also begins to spread vertically around t ≈ 20,000 GM/c3, coinciding with accretion from the initial mass maximum. Finally, notice that in the SANE flow material is drawn from throughout the draining region, while in the MAD flow the inner disk drains quickly and the dominant source region moves outward.
Paper: Mass Transport, Turbulent Mixing, and Inflow in Black Hole Accretion
Authors: George N. Wong, Lia Medeiros, James M. Stone
Figure caption: Radial velocity vr = ur/ut of the accreting plasma in the equatorial plane for GRMHD simulations with black hole spins a* = −0.9 to 0.9. Each panel shows time-averaged, axisymmetrized velocities over the interval 15,000–40,000 GM/c3 from the 8/8 resolution simulations. White dashed contours indicate vr = −0.05, −0.1, −0.15, … in uniform spacing. The event horizon is denoted by the gray-filled region, and the ISCO is plotted as the blue line. Both MAD and SANE flows exhibit trends with spin, with more rapid infall as spin decreases toward a* = −0.9. MAD accretion flows exhibit stronger radial inflow at large radii, while SANE disks show a more rapid increase in ∣vr∣ with decreasing radius. Retrograde SANE flows in particular exhibit steep radial velocity gradients and enhanced infall near the black hole compared to MAD flows. We use the 8/8 resolution simulations to provide a more dense sample in spin and use fluid velocities rather than tracer-based measurements since the 8/8 simulation output cadence is too long to robustly follow particle trajectories close to the event horizon. The velocities inferred from the tracers and the fluid data agree away from the horizon and are consistent across resolution.