adsabs/AstroCLIMB huggingface dataset:
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Similar to Figure 8 but for different grid resolutions (NΠH) at Z = 0.012 and Π = 0.05. Runs shown here have Lx = 4ΠH and Lz = 8ΠH. Different colors denote different NΠH values. The gray shaded regions indicate the saturated state, spanning from t/T = 10 to 25. The dispersions are well converged with grid resolution during the saturated state.
Paper: Bridging Unstratified and Stratified Simulations of the Streaming Instability for τs = 0.1 Grains
Authors: Jeonghoon Lim, 정훈 임, Stanley A. Baronett, Jacob B. Simon, Chao-Chin Yang, 朝欽 楊, Debanjan Sengupta, Orkan M. Umurhan, Wladimir Lyra
Figure caption: Similar to Figure 10 but for different grid resolutions (NΠH) at Z = 0.012 and Π = 0.05. In these models, Lx = 4ΠH and Lz = 8ΠH. The distributions are time-averaged between t/T = 10 and 25 (see Figure A5). When NΠH ≳ 128, the distributions show satisfactory convergence with grid resolution.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: Comparison of ﹩{\rm{\Delta }}{\chi }^{2}(\equiv {\chi }^{2}-{\chi }_{{\rm{\min }}}^{2})﹩ as a function of MBH and M/L for dynamical models with different galactic geometries. The dashed contour lines along with the blue density profiles indicate the 1σ, 2σ, 3σ, … confidence levels of 2D Δχ2 at 2.3, 6.2, 11.8, …, etc. The orange lines show the Δχ2 value as a function of MBH marginalized over M/L. The intrinsic flattening of the bulge (qb) varies down the columns and is fixed across the rows, whereas the intrinsic flattening of the stellar halo (qs) varies across the rows and is constant down the columns. The intrinsic flattening of the disk (qd) is held fixed at 0.2 for all of the panels. The models with the lowest χ2 are found in the third and fourth rows with qb = [0.6–0.7] and qs = [0.7–1.0], and in the second row with qb = 0.5 and qs = [0.9–1.0].
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: Kinematic maps derived from pPXF for the inner 3″ × 3″ (370 pc × 370 pc) of MCG–06-30-15 based on data we collected with SINFONI. The panels show the velocity (v), velocity dispersion (σ), and higher-order (h3–h6) moments of the GH polynomials for the data. The maps are rotated so that the kinematic major axis is parallel to the X-axis. The redshifts and blueshifts from the rotation of the nuclear stars are clearly visible in the velocity map. As shown in the color bars, red and blue correspond to higher and lower values, respectively. The higher-order GH moments (h4 − h6) use the same color scaling as h3. The three white bins close to the center were severely affected by the AGN emission, and were masked out during the modeling.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: 1D and 2D profiles of Δχ2 in the MBH and M/L parameter space, marginalized over qb and qs (the other two parameters shown in Figure 4), as explained in the text. Blue contours have the same meaning as in the previous figure, while red and green curves show the marginalized 1D profiles for MBH and M/L, respectively. Dark and light dashed lines show the 1σ and 3σ confidence intervals on each of these two parameters.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: The spectral fit from pPXF for a selected bin at about 1″ from the center. Data are shown in black, overplotted with the best-fit template in red, and the residuals (data minus model) are shown in green. Plotted on the X-axis are the pixel values corresponding to observed wavelengths from 2.19 to 2.42 μm, while on the Y-axis the corresponding fluxes normalized by the median value are shown. A noise spike appears at the wavelength associated with the blue line in several bins, and those pixels have been masked out during the fitting of all the spectra. The CO (2–0) absorption bands are the primary features we fitted to constrain the stellar LOSVDs.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: HST/WFC3 F547M (medium-band V) image of MCG–06-30-15 (M. C. Bentz et al. 2016). The scale for 10″ is shown. The dust lane in the galaxy disk was masked before fitting the surface-brightness profile.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: Comparison of Δχ2 for different parameter choices in the dynamical models. All the panels have the same flattening for the bulge and the stellar halo (qb = 0.6 and qs = 0.8). The top and bottom rows have the same disk flattening (qd = 0.2) too. In the top row, we show how the adoption of different distances to the galaxy affects the MBH constraints. The distances shown are, from left to right, D = 18 Mpc, 25.5 Mpc (fiducial model), and 38 Mpc. These distances are from the Extragalactic Distance Database and correspond to the two distances measured for galaxies in the same group as MCG–06-30-15 and their average. MBH and distance are linearly correlated, yielding a lower MBH for smaller distance and a higher MBH for larger distance. The middle row shows the effect of different disk flattening values, which correspond to different inclinations. The plotted disk flattening values are 0.1, 0.2, and 0.3, corresponding to, from left to right, i = 66°, 69° (fiducial model), and 73°. The bottom row shows the contribution of the DM halo to our results. The left panel shows the model results when a DM halo is included, with a velocity of ﹩100\sqrt{{\rm{\Upsilon }}}\,{{\rm{km}}\,{\rm{s}}}^{-1}﹩, where ϒ is the stellar mass-to-light ratio, and a scale radius rDM = 180″, while the right panel shows the same models without a DM halo. The shape of the χ2 contours and the minimum χ2 value change slightly for models with/without DM.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: Comparison of kinematic maps derived from pPXF for the inner 3″ × 3″ of MCG–06-30-15. The top two rows show the velocity (v), velocity dispersion (σ), and higher-order (h3–h6) moments of the GH polynomials for the data (same as Figure 2) and the fiducial model (qd = 0.2, qb = 0.6, and qs = 0.8), respectively. The bottom row shows the residuals (= ﹩\frac{\mathrm{model}-\mathrm{obs}}{{\epsilon }_{\mathrm{obs}}}﹩) for each moment. All the bins from the full FOV are shown for completeness, though our models only included half of the kinematics because the other half are point-symmetric. The orientation and the color scaling are the same as for Figure 2. The three white bins close to the center were severely affected by the AGN emission, and were masked out during the modeling. The highly negative h4 values in the data may arise from the counterrotating disk in the galaxy.
Paper: Simulation of Solar Surface Flux Transport Constrained by Magnetic Power Spectra. I. Flux Transport Parameter
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Examples of magnetic power spectra of CR 1916 (left) and CR 1993 (right), respectively. Panels (a)–(b): the SFT models run with the same λR but different diffusion coefficients η and peak meridional flow speeds v0. Panels (c)–(d): the simulated power spectra, using the three different meridional flow profiles shown in Figure 1.
Paper: Simulation of Solar Surface Flux Transport Constrained by Magnetic Power Spectra. I. Flux Transport Parameter
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Comparison of synoptic maps and magnetic power spectra. CR 1916 (left) and CR 1993 (right) are taken as examples. Panels (a)–(b): synoptic maps, with magnetic fields saturated at 100 G. Panels (c)–(d): same as panels (a) and (b) but for the simulated magnetograms. The rings around the ARs are the ringing artifact explained in Section 2.3. Panels (e)–(f): magnetic power spectra of synoptic maps (black, from panels (a)–(b)) and simulated magnetograms (red, from panels (c)–(d)), ﹩{l}_{{\rm{\max }}}=60﹩. Panels (g)–(h): magnetic power spectra with ﹩{l}_{{\rm{\max }}}=﹩60, 100, and 140 using two spatial resolutions of the initial magnetogram 180 × 360 and 360 × 720. The vertical gray lines mark the spatial scale at l = 60.
Paper: Simulation of Solar Surface Flux Transport Constrained by Magnetic Power Spectra. I. Flux Transport Parameter
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Comparison between observations and simulations. Panel (a): temporal evolution of the axial dipole strength of the observation (black) and simulation (red). Panel (b): same as panel (a) but for the total unsigned flux. Panel (c): time–latitude plot of the longitudinally averaged surface field, i.e., magnetic butterfly diagram, based on MDI synoptic maps. Panel (d): same as panel (c) but derived based on simulated magnetograms.
Paper: Simulation of Solar Surface Flux Transport Constrained by Magnetic Power Spectra. I. Flux Transport Parameter
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Illustration of magnetic flux source assimilation for the SFT simulation. The assimilation of the CR 1993 synoptic map is taken as an example. Upper panel: magnetic field distribution from the SFT simulation on the last day of CR 1993, representing the final time step before flux assimilation. Middle panel: ARs identified from the CR 1993 synoptic magnetic map using the ARISE database. Lower panel: updated magnetic field, in which the field from the upper panel is replaced by the detected ARs shown in the middle panel. The rings around ARs are the ringing artifact explained in Section 2.3.
Paper: Simulation of Solar Surface Flux Transport Constrained by Magnetic Power Spectra. I. Flux Transport Parameter
Authors: Yukun Luo, Jie Jiang, Ruihui Wang
Figure caption: Latitudinal dependence of the three meridional flow profiles considered in this study. Their amplitudes vary between cases and are specified in the main text.
Paper: A Stellar Dynamical Mass for the Central Black Hole in MCG–06-30-15
Authors: Nabanita Das, Misty C. Bentz, Eugene Vasiliev, Monica Valluri, Christopher A. Onken, Sandra. I. Raimundo, Marianne Vestergaard
Figure caption: Posterior probability distributions for several parameters of the velocity-resolved reverberation models: MBH, mean time delay τmean, and BLR inclination to our line of sight θi.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: Example of our spaxel construction in IllustrisTNG. Example face-on map from the TNG simulation of a galaxy at 1 kpc spaxel resolution. The system shown here (TNG subhalo id 167393) is a massive star-forming galaxy with ﹩\mathrm{log}({M}_{\star }\,[{M}_{\odot }])=11.66﹩, ﹩\mathrm{log}({M}_{{\rm{gas}}}\,[{M}_{\odot }])=11.62﹩, and SFR = 10.31M⊙ yr−1. We present maps of the stellar mass surface density (Σ⋆; upper left), gas mass surface density (Σgas; upper right), SFR surface density (ΣSFR; lower left), and mass-weighted gas-phase metallicity (lower right). The field of view for the large maps is 100 kpc, and each spaxel has a size of 1 kpc × 1 kpc. The central panel shows a zoom-in of the central region of the galaxy in SFR surface density projection. The contours in each panel (loosely) reflect our selection criteria of pixels with ΣSFR > 10−4M⊙ kpc−2 yr−1 and Σ⋆ > 107M⊙ kpc−2 (see Section 2.3 and Appendix B). We note that these images are downsampled from the native TNG resolution to be closer to the resolution of current IFS surveys.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: The resolved star formation main sequence (rSFMS) in IllustrisTNG. The rSFMS in TNG at z = 0 with 1 kpc spaxel resolution. The solid orange line shows the median value of ΣSFR in each Σ⋆ bin, while the two dashed orange lines indicate the 16th–84th percentiles. The background 2D distribution displays our selected spaxels, color-coded by the number in each bin. For comparison, we show the rSFMS from the EAGLE simulation (J. W. Trayford & J. Schaye 2019) in the gray dashed line (and shaded region about it), observational results from the MaNGA survey (B. C. Hsieh et al. 2017) in the red dotted line, from the CALIFA survey (M. Cano-Díaz et al. 2016) in the orange dashed line, and PHANGS survey in the solid purple line (I. Pessa et al. 2021), and ALMaQUEST (S. L. Ellison et al. 2021) in the red dotted–dashed line. We note that for the rSFMS, as well as all other median/percentile binning in this work, we space Σ⋆ bins in width of 0.25 dex and require 200 spaxels in each bin.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: Best-fitting parameters for the rSFMS of individual galaxies. Left: the probability distribution function (PDF) of normalizations of the rSFMS for individual galaxies’ ΣSFR (taken at Σ⋆ =  108.0M⊙). In all three panels, the colored distributions are the individual galaxies’ PDFs broken up by the global mass bin, and the solid black line is the distribution for all galaxies combined. Middle: the PDF of power-law indices (i.e., α from Equation (4)). Right: the scatter distribution around their best-fit linear rSFMS model, as measured by the standard deviation of the residual.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: The rMZR in a resolved leaky box model. The rMZR formed with different choices of ηin and ηout. The grayscale background shows the distribution of actual IllustrisTNG spaxels included in this study, the same as Figure 5. The colored solid lines are the relations formed by spaxels at t = 5 Gyr under different model assumptions, as labeled.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: (a) TEM image (mass thickness contrast) of a FIB-prepared cross section showing a deposited porous magnesium silicate layer on a silicon wafer. The layer has a variable thickness and a very high porosity. The thickness of the prepared TEM sample in beam direction is about 100 nm. The metal coating is protecting the surface during the FIB sample preparation. (b) and (c) Magnified view of the porous and foam-like structure of the film. Brighter areas represent less solid material in the beam direction. Areas with pore diameters over 100 nm are scarce, and most pores measure less than 20 nm.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: IR spectra for the case of 50 nm deposition of MgSiO3: upper—after CO2 deposition, middle—after MgSiO3 deposition, lower—after NH3 deposition. The spectra are shifted vertically for clarity. The species responsible for the main vibrational bands are assigned in the figure. The small band on the left side of the 13CO2 band is 12CO2 contamination in the amount of less than 1% with respect to 13CO2.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: The gas mass main sequence in a resolved leaky box model. The fgas–Σ⋆ formed with different choices of ηin and ηout. The grayscale background shows the distribution of actual IllustrisTNG spaxels included in this study. The colored solid lines are the relations formed by spaxels at t = 5 Gyr under different model assumptions, as labeled.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: Dependence on definition of “resolved” pixel.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: The rMZR in a resolved closed box model. The grayscale background shows the distribution of simulated TNG spaxels. The dashed lines track the evolution of representative individual spaxels. The solid lines represent the rMZR predictions in our closed box model.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: IR spectra before and after 4 hr of the isothermal kinetic experiment at 80 K for the sample containing a 50 nm MgSiO3 layer. Two bands related to NH4+NH2COO− (13C) are shown by arrows.
Paper: Star Formation Rates, Metallicities, and Stellar Masses on Kiloparsec Scales in TNG50
Authors: Jia Qi, Alex M. Garcia, Davis Robinson, Paul Torrey, Jorge Moreno, Kara N. Green, Aaron S. Evans, Z. S. Hemler, Lars Hernquist, Sara L. Ellison
Figure caption: Modified smoothing kernel.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: Carbamic acid and carbamate anion formation reaction schemes using the “curly arrow” notation common in mechanistic chemistry to identify the movement of electron pairs and the making and breaking of chemical bonds. In (a), nucleophilic donation of the N atom lone pair on the NH3 to the central C in CO2 opens one of the C–O double bonds by transferring an electron pair from the bond to the terminal O atom. The enhanced electron density on the terminal O atom can then pull a proton from the incoming NH3 forming carbamic acid. In (b) and (c), the presence of a base (NH3 and H2O, respectively), the lone pairs on the corresponding N and O atoms in the base see their nucleophilicity provide a pathway to the carbamate anion via proton transfer from the incoming NH3 to the base as the incoming NH3 donates its lone pair to the electrophilic carbon in the CO2 forming the N–C bond as an electron pair transfers from a C–O double bond to a terminal O atom.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: Time dependences of the NH4+NH2COO− column density calculated from the 1522 cm−1 band for all samples except CO2-ice/H2O-ice/NH3-ice and their fits. The nanometer (nm) values are the dust layer thicknesses. Errors are reflected by the variation of the signal for 0 nm around the 0-line.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: Sketches (left) of three experiments—CO2 + NH3 ice mixtures (top), CO2-ice/NH3-ice layers (middle), and CO2-ice/MgSiO3-grains/NH3-ice layers (bottom)—and the IR spectral indication of the ammonium carbamate formation (right) in the CO2 + NH3 ice mixtures and CO2-ice/MgSiO3-grains/NH3-ice layers.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: Evolution of the ammonium carbamate bands with the reaction time at 80 K for the sample containing a 100 nm MgSiO3 layer. The spectra are shifted vertically for clarity.
Paper: Cosmic Dust as a Prerequisite for the Formation of Complex Organic Molecules in Space?
Authors: Alexey Potapov, Kilian Pollok, Falko Langenhorst, Martin McCoustra, Robin T. Garrod
Figure caption: Evolution of the ammonium carbamate bands with the dust layer thickness after 4 hr of the isothermal kinetic experiment at 80 K. The spectra are shifted vertically for clarity.
Paper: Constraining the Neutron-star Equation of State via Short Gamma-Ray Burst X-Ray Afterglows
Authors: R. Moradi, Y. Wang, F. Rastegarnia, E. S. Yorgancioglu, Shu-Xu Yi, B. Eslam Panah, S. N. Zhang
Figure caption: The GM1 EOS, representing an intermediate stiffness, provides the best fit to observational data by minimizing the absolute difference ﹩{\rm{\Delta }}P=\left|\,{P}_{{\rm{NS}}}({t}_{{\rm{co}}})-{P}_{{\rm{BH}}}({t}_{{\rm{co}}})\right|,﹩ where PNS(tco) is the spin period of the NS at collapse (from multipolar spin-down) and PBH(tco) is the BH spin period inferred from postplateau energy (see Section 2). GM1 yields the smallest average ΔP, with only a marginal difference from TM1 (﹩{M}_{{\rm{\max }}}=2.2\,{M}_{\odot }﹩), as indicated by Δ〈ΔP〉 ∼ 10%. This corresponds to Mcrit ≈ 2.3 ± 0.1 M⊙. The uncertainty on Mcrit shrinks with broader temporal coverage, and when only the highest-quality light curves are used, the best-fit value shifts to Mcrit ≈ 2.4 M⊙ with noticeably smaller error bars.
Paper: Constraining the Neutron-star Equation of State via Short Gamma-Ray Burst X-Ray Afterglows
Authors: R. Moradi, Y. Wang, F. Rastegarnia, E. S. Yorgancioglu, Shu-Xu Yi, B. Eslam Panah, S. N. Zhang
Figure caption: NS spin-down energy as the primary energy source of the GRB afterglow. Initial spin period (P0) and magnetic field components are detailed in Table 2. The plot is presented on a logarithmic scale, and the residuals are expressed relative to the model-predicted luminosity: ﹩\,{\rm{Residual}}\,\,=\,\frac{\rm{Observed Luminosity}\,-{\rm{Model-Predicted Luminosity}}}{\,{\rm{Model-Predicted Luminosity}}}﹩.
Paper: Oscillatory Behaviors in General Relativistic Magnetohydrodynamical Simulations of Interacting Toroids
Authors: Dilshodbek Bardiev, Jan Schee, Zdeněk Stuchlík
Figure caption: Evolution of the normalized mass accretion rate as a function of time for three model groups: Single models, Corot models, and Contra models. Each subplot shows the mass accretion histories for different simulations within the group, using consistent colors and line styles for comparison.