adsabs/AstroCLIMB huggingface dataset:
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: Left: distribution of spectral indices for our sample of 24 transient sources. Right: comparison of the distribution of spectral indices for the combined sample of archetypal GPS and CSS sources from M. A. Keim et al. (2019) and the combined sample of radio transients from this work and from A. Wołowska et al. (2021).
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption:                         The GMRT image and selected VLA images showing source 064001+28 (marked as A) and additional components/sources marked as B1–B3 and C. The bottom right panel shows measurements of their flux densities, with measurements of component A added for comparison. Note, however, that a more detailed spectrum of component A with a fitted model is shown in Figure 10.
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: Radio color–color diagram for our sample. The blue square corresponds to the spectral index range from −0.5 to 0.5 (“blazar box”). Galaxies are marked with yellow circles, and the only quasar in the sample is shown in gray. The two galaxies, 180940+24 and 203909−30, with fixed values for their spectral indices are indicated by brown circles. Details on the calculation of αthin and αthick are provided in Section 3.6 and Table 2.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: A ﹩P\mbox{--}\dot{P}﹩ diagram for over 3474 pulsars. Period (P) is in seconds and period derivative (﹩\dot{P}﹩) is in seconds per second. Light-gray circles represent known pulsars, magenta stars indicate FAST null pulsars, and circles with blue highlight our candidates for PSR J1900–0134, red for PSR J2323+1214, and green for PSR J1945+1211. PSR J0901–4046, an ultra-long-period pulsar (M. Caleb et al. 2022), is marked with a black star. The inset plot provides a zoomed-in view of the region containing our candidates, while the red circle in the main plot highlights their location. Diagonal lines represent constant magnetic fields (magenta), spin-down luminosities (cyan), and characteristic ages (gray). The lower-right corner displays “death valley” with various death lines: traditional (black), K. Chen & M. Ruderman (1993; red), curvature radiation from vacuum gap (green), and from the space-charge-limited flow model (blue). Data are obtained from the ATNF pulsar catalog (R. N. Manchester et al. 2005).
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Log–log plot showing the relationship between pulse period and pulse width, along with a power-law fit. Data are obtained from the Australia Telescope National Facility (ATNF) pulsar catalog, http://www.atnf.csiro.au/research/pulsar/psrcat/ (R. N. Manchester et al. 2005). Our candidate pulsars are marked with colored circles: blue for (PSR J1900–0134), orange for (PSR J2323+1214), and green for (PSR J1945+1211).
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Histogram of null fractions observed in various pulsars. The distribution indicates a higher frequency of pulsars with low null fractions and decreases as the null fraction increases. The vertical dotted lines represent the null fractions for PSR J1900–0134 (cyan), PSR J2323+1214 (yellow), and PSR J1945+1211 (red), highlighting the positions of these pulsars within the distribution.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Examples of quasiperiodic pulses. The left column shows the pulse profiles, and the right column shows their corresponding ACFs at 49.25 μs resolution for pulse numbers 536 (top) and 548 (bottom). The blue dotted vertical line indicates the microstructure width (tμ), and the red dotted vertical line indicates the quasiperiodicity (Pμ).
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: A single bright pulse (solid red) detected in the trailing component of PSR J2323+1214. The black solid line represents the integrated pulse profile from the entire observation of the pulsar.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Example pulses from PSR J1900–0134 at 1.25 GHz showcasing the microstructures.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: Main panel: a scatter plot of peak flux density and tμ values for 124 microstructure pulses. Top panel: the PDFs of the tμ values. Right panel: the PDFs of peak flux density, fitted with a log-normal distribution.
Paper: Unveiling the Emission Properties of Three Long-period Pulsars Using FAST
Authors: H. M. Tedila, D. Li, P. Wang, R. Yuen, J. P. Yuan, N. Wang, Z. G. Wen, S. J. Dang, A. G. Tegegne, R. Rejep, C. C. Miao
Figure caption: The distribution of the detection rate of bright pulses (Nbright/h) for different pulsars. Data for PSR J1900–0134 (blue star), J2323+1214 (green star), and J1945+1211 (red star) are from this work. The magenta curve represents a power-law fit.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: The top panel shows the evolution of baryon fraction in the IGM, fb,IGM, at redshifts z = 0.0, 0.1, 0.2, 0.3, 0.4, 0.5, 0.7, 1.0, 1.5, 2.0, and 3.0, which are calculated from the TNG100 simulation. The second panel shows DMIGM as a function of redshift, in which the blue line is calculated by Equation (14) with fb,IGM = 0.83, and the orange line is derived from the value in the top panel. The third panel presents the absolute residual of calculating DMIGM by using the value of fb,IGM in the TNG100 simulation, with respect to use fb,IGM = 0.83. The fourth panel is the corresponding relative residual.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: The top and bottom panels show the number of intervening extragalactic foreground halos and the differential number per unit redshift, as function of the redshift, respectively. The blue, orange, green, red, purple, and brown lines indicate the results of halo mass with 1010–1011, 1011–1012, 1012–1013,​​​​​​ 1013–1014, 1014–1015, and 1010–1015 M⊙, respectively.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: The blue, orange, red and purple lines are the evolution of ﹩{\sigma }_{{{\rm{DM}}}_{{\rm{IGM}}}}﹩ according to the results in W. Zhu & L.-L. Feng (2021), the best-fitting results of the EAGLE simulation given by Equations (12) and Equation (11) of A. J. Batten et al. (2021), and the simplified model used in J. M. Cordes et al. (2022), respectively. The green line is the formula of ﹩{\sigma }_{{{\rm{DM}}}_{{\rm{IGM}}}}﹩ we used in this work.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: The probability density distribution (top row) and cumulative probability distribution (bottom row) of the scattering measure caused by the host galaxies and their halos, SMhost, for PSFR (left column) and PStar (right column) model at different redshift values based on TNG100 simulation. The blue, orange, green, red, purple, and brown lines are the distribution at z = 0.0, 0.5, 1.0, 1.5, 2.0, and 3.0, respectively. The black dashed line in the bottom row represents the 50% cumulative probability.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: The intrinsic probability density distribution of FRBs between redshift 0.0 and 3.0 for the PStar (blue), PSFR (red), and PMix (green) source population models. The blue, green, and red lines indicate the fraction of FRBs associated with young progenitors (i.e., tracing the cosmic star formation rate, SFR, density), with fPSFR = 0.0, 0.5, and 1.0, respectively.
Paper: The Dispersion Measure and Scattering of Fast Radio Bursts: Contributions from Multicomponents, and Clues for the Intrinsic Properties
Authors: Jian-feng Mo, Weishan Zhu, Long-Long Feng
Figure caption: Similar to Figure 2, but for τHost at 600 MHz.
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: Left: distribution of variability ratio at 3 GHz for our sample. Right: the 3 GHz light curves for selected sources. The gray dashed line indicates the recalculated value of νLν,GHz = 1039 erg s−1 below which most known thermal TDEs occur (Y. Cendes et al. 2024).
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: The intrinsic turnover frequency vs. linear size diagram. The transient sources from this work are marked with yellow (galaxies) and gray (quasar) circles. The open red circles (galaxies) and open black circles (quasars) indicate CSS and GPS sources taken from C. P. O’Dea (1998), I. A. G. Snellen et al. (1998a), W. H. de Vries et al. (1997), C. Stanghellini et al. (1998), and R. Fanti et al. (1990), collected by M. A. Keim et al. (2019) in one sample. The filled red circles (galaxies) and filled black circles (quasars) indicate radio transients discovered in the CNSS by A. Wołowska et al. (2021). The sizes of the circles correspond to their radio luminosity at rest frame 5 GHz. The blue solid line indicates the linear relationship log ﹩{\nu }_{p}=-0.21-0.59\times \mathrm{log}\,\mathrm{LLS}﹩, found by M. Orienti & D. Dallacasa (2014). The gray diamond indicates the range of values for PS sources from J. R. Callingham et al. (2017).
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: The radio SEDs between 144 MHz and 15 GHz. The solid line shows the best-fit to the data with the modified power-law model (Equation (1)).
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: The radio power vs. linear size (P−D) diagram adapted from M. Kunert-Bajraszewska et al. (2010), including various types of radio-selected AGNs. The plots of GPS, CSS, LLC, FR I, and FR II sources are taken from M. Kunert-Bajraszewska et al. (2010). The sample of giant radio galaxies is adapted from A. Kuźmicz et al. (2018). The RIQs and RQQs are taken from M. J. Kukula et al. (1998) and M. E. Jarvis et al. (2019). LINERs and Seyfert galaxies are from J. F. Gallimore et al. (2006), R. D. Baldi et al. (2018), and V. Singh et al. (2013). The transient sources are taken from A. Wołowska et al. (2021) and from this work and are indicated with black plus signs and red triangles, respectively. The black dashed line shows a possible evolutionary track for high-power objects as described in T. An & W. A. Baan (2012).
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: Left: Palomar (red) and archival 6dF (black) optical spectra of 101841−13 with strong emission lines indicated. The left axis shows the flux obtained from the (nonphotometric) Palomar observations, and the right axis shows the uncalibrated flux in counts from the 6dF observations. Small panels below zoom in on key absorption-line and emission-line regions: Ca K and H lines (left); Hβ and [O III] lines (middle); and [N II], Hα, and [S II] lines (right). Scaling of the 6dF spectrum was chosen as to fit the profiles of absorption and Balmer lines in Palomar spectrum. Right: radio 3 GHz light curve (red points), WISE W1 (yellow) and W2 (green) light curves, and NVSS 1.4 GHz emission (blue point). The vertical red dashed line indicates the date of the Palomar spectroscopic observation.
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: The LOFAR 144 MHz images (yellow contours) overlaid on the SDSS i-band images for four objects. The presented contours have the following values: 1.5, 2.0, 2.5, 3.5, and 4.5 × 10−4Jy beam−1 (source 095141+37); 1.5, 2.0, 3.5, 5.5, and 7.5 × 10−4Jy beam−1 (source 112940+39); 2.4, 4.0, 6.5, 10.0, and 14.0 × 10−4Jy beam−1 (source 150415+28); and 2.5, 3.5, 5.5, and 7.5 × 10−4Jy beam−1 (source 164607+42) .
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: The VLA S-band image (magenta contours) overlaid on the SDSS i-band image of 064001+28. The presented contours have the following values: 1.7, 5, and 20 × 10−4 Jy beam−1.
Paper: VLASS-based Survey of Transition State Galaxies and Their Relationship to Compact Peaked-spectrum Radio Sources
Authors: Magdalena Kunert-Bajraszewska, Aleksandra Krauze, Amy E. Kimball, Łukasz Stawarz, Preeti Kharb, Daniel Stern, Kunal Mooley, Kristina Nyland, Dorota Kozieł-Wierzbowska
Figure caption: BPT and WHAN diagrams (J. A. Baldwin et al. 1981; L. J. Kewley et al. 2006; R. Cid Fernandes et al. 2011) for 101841−13. The red circle indicates values calculated based on measurements from the Palomar spectrum, and the black circle indicates upper limits estimated based on the 6dF spectrum.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Azimuthal/poloidal slice of initial conditions along with the grid geometry. The color scale denotes the logarithm of the rest-mass density, and as an example, we plot the magnetic fields structure (in black) for a SANE disk. The grid zone boundaries are represented by the white mesh. The grid zones are concentrated toward the equatorial plane and at smaller radii, where we expect most of the relevant physics to occur.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Time series of the horizon-penetrating fluxes for six models: a* = { −15/16, 0, +15/16}, MAD and SANE. Left column: MAD simulations. Right column: SANE simulations. Top row: rest-mass accretion rate. Second row: dimensionless magnetic flux. Third row: normalized, absolute angular momentum flux. Bottom row: normalized absolute energy flux with the contribution from rest mass subtracted. a* = −15/16 simulations are plotted in indigo, a* = 0 simulations in crimson, and a* = +15/16 in gold.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Time- and azimuth-averaged poloidal slices of rest-mass density with averaged conserved currents overlaid for the MAD a* = +0.94 model. In the top row, we plot (left to right) the mass ﹩{{\mathfrak{J}}}_{M}\equiv \sqrt{-g}\rho {u}^{\mu }﹩, angular momentum ﹩{{\mathfrak{J}}}_{L}\equiv \sqrt{-g}{T}_{\phi }^{\mu }﹩, and energy ﹩{{\mathfrak{J}}}_{E}\equiv -\sqrt{-g}{T}_{t}^{\mu }﹩ currents. The middle row shows from left to right the total angular momentum current, the electromagnetic contribution, and the fluid contribution, respectively. The bottom row is similar to the middle row except that we plot the energy current. The arrows in the flow lines indicate the direction of the conserved currents, and the color scale indicates the magnitude plotted on a log scale since it can vary by several decades on a poloidal slice. The general morphology of the currents is similar, namely, strong inflow in the disk that transitions to an outflow at higher latitudes.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Radial profiles of rest-mass density ρ (in arbitrary code units), dimensionless fluid temperature Θ ≡ pg/(ρc2), fluid entropy s, radial velocity vr, specific angular momentum uϕ, specific energy ut, magnetic field strength squared b2, inverse plasma-beta ﹩{\beta }_{p}^{-1}\equiv ({b}^{2}/2)/{p}_{g}﹩, and the density scale height h/r. The solid (dashed) lines represent MAD (SANE) simulations. Different colors correspond to different spins. Note that the units of rest-mass density in our simulations are arbitrary—a consequence of the scale-free nature of ideal GRMHD simulations—and therefore the absolute values of 〈ρ〉 have limited physical significance. One should instead focus on the structure of the radial profile.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: The 3 hr modulation index M3 for the accretion rate ﹩\dot{M}﹩ (defined as MΔt ≡ σΔt/μΔt; here Δt = 3 hr). To estimate the average M3 (indicated by a marker for each simulation in this plot) for Sgr A* (which has a characteristic timescale tg ∼ 20 s), we extract as many independent 3 hr time segments from the ﹩\dot{M}﹩ time series from t = 15,000 tg to t = 30,000 tg (∼27) and compute the average sample mean. The error bars plot the standard error of the sample means (﹩\sim {\sigma }_{{{\rm{M}}}_{3}}/\sqrt{27}﹩) and quantify the uncertainty in our measurement of M3.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Similar to Figure 3 but now plotting the contribution of various components of the fluxes (see Equations (15), (16), (17), (18), (19), and (20)). We see that magnetic fields have little-to-no contribution toward ﹩\dot{L}﹩ and ﹩\dot{E}﹩ in the SANE models. In the MAD models, the trend in total flux closely matches the trend observed in the electromagnetic components.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Time-averaged radial fluxes as a function of black hole spin. The data points in red (blue) denote MAD (SANE) simulations. The dashed line plots the value expected for a thin disk at the ISCO. Left panel: specific angular momentum flux. Middle panel: specific energy flux. Right panel: ratio of outflow power (﹩\dot{E}-\dot{M}﹩) to rest-mass accretion rate.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Top to bottom: time- and azimuth-averaged poloidal plots of ρ, σ ≡ b2/ρ, and Θ ≡ pg/(ρc2), respectively. Each column represents a different black hole spin. In each subplot, the left panel shows the MAD simulation, while the right panel shows the corresponding SANE simulation. Contours in each plot indicate σ = 1. Note that for quantities defined as ratios, such as magnetization σ and fluid temperature Θ, the averages are taken separately, e.g., 〈σ〉 = 〈b2〉/〈ρ〉.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Angular velocity profiles 〈Ω〉 ≡ 〈uϕ〉/〈ut〉 in Kerr–Schild coordinates in units of deg/GM/c3. The solid line plots the time-average value, and the shaded region plots one standard deviation. The dotted black line is the Keplerian fit ﹩{{\rm{\Omega }}}_{K}={({r}^{3/2}+a)}^{-1}﹩ for a* = +0.94. The MAD rotational profiles are sub-Keplerian and have a significantly greater spread as compared to the SANE models. The SANE angular velocity agrees with the Keplerian expectation.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Time-averaged, density-weighted radial profiles of tin for the v3 library. The dashed lines are power laws that approximately trace tin.
Paper: A Survey of General Relativistic Magnetohydrodynamic Models for Black Hole Accretion Systems
Authors: Vedant Dhruv, Ben Prather, George N. Wong, Charles F. Gammie
Figure caption: Time- and azimuth-averaged “jet profiles” (σ = 1 contours). The solid (dashed) lines represent MAD (SANE) models. The filled gray circle at the lower-left corner denotes a zero spin black hole (reh = 2 rg).