adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Intensity-weighted velocity dispersion (moment 2) map of (a) HCN J = 4–3, (b) HCO+ J = 4–3, (c) HCN J = 3–2, and (d) HCO+ J = 3-2, created with 1.5 mas pixel−1. The displayed velocity range is 0–240 km s−1 for J = 4–3 and 0–130 km s−1 for J = 3–2. Note that the peak velocity dispersion value is significantly higher for the J = 4–3 lines than for the J = 3–2 lines, possibly because of the smaller synthesized beam size for J = 4–3, which can probe velocity structures at a finer spatial resolution. The horizontal thick bar, open circle, and plus and open diamond marks are the same as in Figure 5.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Comparison of position–velocity diagrams between observational data and the model by B. Vollmer et al. (2022). (a): HCN J = 4–3. (b): HCO+ J = 4–3. In these plots, the major axis is PA = 110°, consistent with those shown in B. Vollmer et al. (2022). For the observations (left), the images are rotated by 20°to make the elongated structure horizontal (E–W). For the model (right), the data are projected such that the disk plane is horizontal (E–W). In each panel, the curved dotted line indicates the expected Keplerian rotation for the radial distribution of the total enclosed mass, M(R) = MSMBH + M0R5/4, where MSMBH is the central SMBH mass (MSMBH = 1 × 107M⊙) and M0 is the stellar mass distribution (M0 = 0.8 × 106M⊙ (pc−5/4)), in the same way as presented in B. Vollmer et al. (2022).
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Gaussian fit (dashed line) of the detected HCN J = 4–3 (top), HCO+ J = 4–3 (second top), HCN J = 3–2 (second bottom), and HCO+ J = 3–2 (bottom) emission lines at the W-torus (1.7 pc diameter) (left), E-torus (1.7 pc diameter) (second left), torus (3.4 pc diameter centered at the continuum emission peak) (second right), and the torus with an even wider area (6.8 pc diameter) (right). The abscissa is the optical LSR velocity (in km s−1) and the ordinate is the flux density (in mJy). The horizontal dotted straight line indicates the zero-flux level. Lower-frequency (redshifted) emission tails, relative to the molecular line emission at the systemic velocity (Vsys = 1130 km s−1), are discernible in some of the spectra in Figure 4. We apply two Gaussian fits to the HCN J = 4–3, HCO+ J = 4–3, and HCN J = 3–2 emission lines at the W-torus and at the torus with a 3.4 pc diameter aperture. For the HCN J = 3–2 emission line, a second redshifted emission component is also added at the E-torus (j). For the remaining data, a single Gaussian fit is applied.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Map of flux ratios calculated in units of Jy beam−1 km s−1 for (a) HCN J = 4–3 to HCN J = 3–2, (b) HCO+ J = 4–3 to HCO+ J = 3–2, (c) HCN J = 4–3 to HCO+ J = 4–3, and (d) HCN J = 3–2 to HCO+ J = 3–2. Flux ratios are calculated after modifying the synthesized beam to a 0﹩\mathop{.}\limits{^{\prime\prime} }﹩021 circular one for (a), (b), and (d), and a 0﹩\mathop{.}\limits{^{\prime\prime} }﹩015 circular one for (c). The plus and open diamond marks are the same as in Figure 5.
Paper: ALMA Subparsec Resolution Dense Molecular Line Observations of the NGC 1068 Nucleus
Authors: Masatoshi Imanishi, Bernd Vollmer, Yoshiaki Hagiwara, Kouichiro Nakanishi, Takuma Izumi, Nozomu Kawakatu
Figure caption: Comparison between observational (left) and model (right) spectra by B. Vollmer et al. (2022), at multiple torus positions. (a): HCN J = 4–3. (b): HCO+ J = 4–3. In these plots, NW and SE are along PA = 110°, to be consistent with those shown in B. Vollmer et al. (2022). Spectra are extracted along the NW and SE directions, at distances of 0 pc, ±1.4 pc, ±2.8 pc, and ±4.2 pc, with 1.4 pc diameter circular apertures.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Example accretion history number 35, adopted from V. G. Elbakyan et al. (2019).
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Propagation diagrams for 1.0 M⊙ classical and accreting models. Buoyancy profiles appear hashed for the classical model and gray for the accreting model. The Lamb profiles of dipole modes are respectively drawn in dashed and full red. The characteristic frequency, νmax, for the accreting model is also indicated, along with the pp-burning profile.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Top panel: a power-law fit between Δν and νmax values derived from our models (top) and the corresponding residuals (bottom). A 1:1 line is drawn in black, and the data points are additionally colored by temperatures increasing from red to blue colors. Bottom panel: residuals with the zero-line drawn in dashed black.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Evolution of frequencies for classical (gray) and accreting (black) 0.9 M⊙ models. Radial modes are drawn as full lines, dipole modes as dashed lines, and νmax as thicker dashed lines. The accretion history is drawn in red, and a blue arrow highlights the individual frequencies (black lines) responding to mass accretion. For visualization, the frequencies are scaled with the third root of the ratio of the radius to the ZAMS radius ﹩{(r/{r}_{0})}^{3/2}﹩.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: C–D diagram displaying the small separation against the large separation. Classical models are plotted in gray, and accreting models are colored according to ZAMS mass, increasing from blue to yellow. The moment accretion ends is marked by a dashed red line, the ZAMS by a full red line, and the beginning of the Henyey track as a pink dotted–dashed line.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Violin diagram illustrating frequency differences at the ZAMS between classical and accreting models of 1 solar mass. Radial modes are shown in green, and dipole modes are shown in pink. Dashed lines indicate the means of the distributions, and dotted lines indicate the 25th and 75th quartiles.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Kippenhahn diagrams for 1.1 M⊙ classical (top) and accreting models (bottom). Radiative zones are colored gray, and zones of different mixing types are hashed. Burning strength is increasing from yellow to red.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Δν values obtained from GYRE (﹩{\rm{\Delta }}{\nu }_{{\mathtt{GY\; RE}}}﹩) drawn against Δν values derived from MESA (ΔνMESA). Each data point is colored by Teff increasing from red to blue colors, and an ideal one-to-one line is also drawn in black.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Temperature versus density diagram for a 1 solar mass model. The profiles are colored by age and span a phase, in which the model is at 90% of its ZAMS mass up until the ZAMS. A temperature inversion is seen for the early stages of the model.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Young stars from SPYGLASS IV (R. Kerr et al. 2023) for which PAge < 50 Myr > 0.99 and that fall within LOPS2 (red symbols). The stars are concentrated in the upper part of the field of view, which is where PLATO intersects the galactic plane. Stars marked as black symbols do not fall within LOPS2.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Thermal efficiency parameter β (full line; Equation (7)) and heat injection depth Mouter (dashed line; Equation (9)) against mass accretion rate ﹩\dot{M}﹩.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Comparison of 1.0 M⊙, accretion history 35, models calculated with the two different MESA setups, A (top) and B (middle), as described in the text. The diagrams display fundamental stellar parameters along the protostellar and the pre-MS phases. The bottom panel compares evolutionary tracks.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Young stars from the SPYGLASS survey by R. Kerr et al. (2023) with ages less than 50 million years. Gray symbols represent the whole sample, while colored symbols represent stars in LOPS2 for which masses are available. Luminosities, effective temperatures, and masses are taken from O. L. Creevey et al. (2023). Evolutionary tracks are also plotted, increasing in mass from black to orange colors.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Simulated light curve (top) for a young pre-MS star exhibiting spot modulation and solar-like oscillations. The corresponding power spectrum (bottom) is drawn in gray, with a filtered spectrum in black. The pure oscillation signal is drawn in green.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Frequency differences between resolutions of 0.8 and 0.4 for 1.2 M⊙ models. Radial modes are shown in green, and dipole modes are shown in pink. The top panel corresponds to the coarser resolution, while the bottom panel corresponds to the finer resolution.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: HR diagram displaying the locations of the models used, for which we compare propagation diagrams in Figure 5.
Paper: Solar-like Oscillations in Accreting Pre-main-sequence Stars: Insights and Prospects
Authors: Johannes Jørgensen, Konstanze Zwintz, Ebraheem Farag, Eduard I. Vorobyov, Thomas Steindl
Figure caption: Convergence map for the calculated model grid. Squares indicate converged models and are colored by runtime in hours increasing from blue to red.
Paper: Determining the State of Jupiter’s Magnetosphere Using In Situ and Remote Sensing Observations
Authors: J. W. Sun, L. Xie, Z. H. Yao, S. Y. Fu, B. Zhang, Y. Xu, F. Leppard, Y. N. Chen, D. Grodent, L. C. Ray, B. Bonfond, W. R. Dunn
Figure caption: Comparisons of magnetospheric phenomena between compressed and quiet states. Two representative UV auroral images for the (a) X-family aurora and (b) Q-family aurora identified by D. Grodent et al. (2018). Each image is labeled with the observation date, total power, and auroral morphology. The magnetic field in the lobelike region, ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩, across different radial distances in (c) the compressed (blue) and (d) the quiet (gray) magnetosphere (from Y. Xu et al. 2023). Each circle’s color and size in (c), (d) represent the duration of the spacecraft crossing the current sheet, a proxy for the current sheet thickness. Total magnetic field strengths and magnetic field fluctuations using a fourth-order Butterworth filter to produce 10–60 minutes bandpass-filtered results of (e) the compressed magnetosphere, which shows significant fluctuations, and (f) the quiet magnetosphere, where almost no magnetic field fluctuations appear (modified from J. W. Sun et al. 2024). Measurements of radio emissions in (g) the compressed magnetosphere, showing prominent broadband kilometric (bKOM) emission features and (h) quiet magnetosphere where almost no bKOM radio emissions are detected (modified from Y. Chen et al. 2024). These phenomena present concurrent responses to changes in the magnetospheric states.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison of flux-weighted mean optical depths for subsets of disks in different star-forming regions—i.e., L1641/L1647 (1.5 Myr), Taurus (1–2 Myr), Serpens (1–3 Myr), Lupus (1–3 Myr), Cha I (2–3 Myr), and Upper Sco (5–10 Myr)—plotted versus (a) disk dust mass, (b) disk size, and (c) disk dust mass ratio (i.e., Mdust,DIAD/Mdust,lit). Optical depths are obtained from flux-weighted averages of the 1.3 mm optical depth at each radius in the disk, calculated using the DIAD models. Optical depth values for the Lupus, Taurus, Cha I, and Upper Sco regions are adopted from A. M. Rilinger et al. (2023). The denoted disk masses correspond to the median value of the distribution obtained for each object. The color bar in panel (c) indicates the dust mass of the disk. In all three panels, marker size increases proportionally with the size of Rdisk (in au), and the black dashed line represents τω = 1.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison of CDFs that correspond to dust masses of Serpens (red line) and L1641/L1647 (blue line) gathered from this work and Serpens’s (light red line) and L1641/L1647’s (light blue line) dust masses recalculated using literature millimeter fluxes (A. R. Anderson et al. 2022; S. E. van Terwisga et al. 2022) in Equation (1), and mass content available in confirmed exoplanets that are above the detectability threshold (i.e., >0.3 MJup), using data gathered from the NASA Exoplanet Archive (black line). The CDFs were developed using the Kaplan–Meier fitting method.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Median dust masses for 12 star-forming regions compared to the respective age of each region. Following A. M. Rilinger et al. (2023), the black dashed line denotes the dust depletion function Mdust ∝ t−1 (L. Testi et al. 2022) and scales it by the weighted mean mass at 1.5 Myr. Median values for Mdust are calculated for each region. Serpens data correspond to this work, while data for the remaining star-forming regions are gathered from A. M. Rilinger et al. (2023).
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Probability density functions of Mdust for 12 star-forming regions. Blue dotted lines denote the median for each region, and red dashed lines denote the median for all regions (∼9.28 M⊕). Serpens and L1641/L1647 data correspond to this work, while data for the remaining star-forming regions are gathered from A. M. Rilinger et al. (2023).
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison of flux-weighted mean optical depth for a subset of disks in Serpens (top) and L1641/L1647 (bottom) plotted versus disk dust mass. Optical depths are gathered from flux-weighted averages of the 1.3 mm (left) and 7 mm (right) optical depth at each radius in the disk, calculated using the DIAD models. Denoted disk masses correspond to the median value of the distribution obtained for each object. We note that for Serpens, we show the whole sample of 18 objects, while for L1641/L1647, we show 10% of the sample. The color bar denotes the disk’s outer radius (in au). The black dashed line represents τω = 1.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison between the existing literature prior values and the posterior value estimations derived from the ANN analysis of the L1641 and L1647 disks. The dotted black line denotes a perfect correlation (one-to-one fit) between the values.
Paper: Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
Authors: Luisa F. Zamudio-Ruvalcaba, Catherine C. Espaillat, Álvaro Ribas, Enrique Macías
Figure caption: Comparison between the existing literature prior values and the posterior value estimations derived from the ANN analysis of the Serpens disks. The dotted black line denotes a perfect correlation (one-to-one fit) between the values.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The momentum density ρur, multiplied by ﹩2\pi r\sin \theta ﹩, is expressed in units of ﹩[{L}_{{\rm{Edd}}}{c}^{-2}{r}_{{\rm{g}}}^{-1}]﹩. Negative values indicate inflow, while positive values correspond to outflow. The red dashed line represents the zero Bernoulli surface Be = 0, and the green solid line is the photosphere τr = 1. The arrows depict the radiation flux direction, and the magnetic field strength is labeled above each frame.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The efficiency of outgoing kinetic luminosity ﹩{L}_{{\rm{KE}}}/(\dot{M}{c}^{2})﹩ computed in the outflow region with Be > 0, ur > 0 (top panel) and the efficiency of radiation luminosity ﹩{L}_{{\rm{r}}}/(\dot{M}{c}^{2})﹩ computed in the optically thin region with τr < 1 (bottom panel). The accretion in each simulation is shown in a different color, and the magnetic dipole strength is shown in line style.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The efficiency of outgoing kinetic luminosity ﹩{L}_{{\rm{KE}}}/(\dot{M}{c}^{2})﹩ computed in the outflow region with Be > 0, ur > 0 (top panel) and the efficiency of radiation luminosity ﹩{L}_{{\rm{r}}}/(\dot{M}{c}^{2})﹩ computed in the optically thin region with τr < 1 (bottom panel). The strength of the dipole in each simulation is shown in a different color and line style.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The momentum density ρur, multiplied by ﹩2\pi r\sin \theta ﹩, is expressed in units of ﹩[{L}_{{\rm{Edd}}}{c}^{-2}{r}_{{\rm{g}}}^{-1}]﹩. Negative values indicate inflow, while positive values correspond to outflow. The red dashed line represents the zero Bernoulli surface Be = 0, and the green solid line is the photosphere τr = 1. The top and bottom rows correspond to the magnetic dipole strengths of 3 × 1010 G and 1010 G. Streamlines depict the radiation flux direction, and the accretion rate is labeled above each frame.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The isotropic luminosity, expressed in units of LEdd, is displayed in polar coordinates. The right side labels indicate the corresponding viewing angles. Straight gray solid lines denote specific viewing angles. For each magnetic field and accretion rate, the faded portion of the curve represents the optically thick region, where the radiation flux drops to zero.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: Isotropic luminosity in the unit of LEdd in polar coordinates. The straight gray solid lines correspond to particular viewing angles. The right side labels show viewing angles. The faded colored straight line in each magnetic field curve represents the optically thick region at which the radiation flux diminishes to zero.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: Magnetospheric radius Rm versus accretion rate in simulations with two different magnetic dipole strengths. Each color corresponds to the simulations with a given magnetic dipole strength. The dashed gray lines represent fitted functions, while the solid black line denotes the analytical solution of R. F. Elsner & F. K. Lamb (1977), multiplied by a suitable constant.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The accretion ﹩\dot{M}﹩, inflow ﹩{\dot{M}}_{{\rm{in}}}﹩, and outflow ﹩{\dot{M}}_{{\rm{out}}}﹩ rates in the unit of LEdd/c2 are shown in the top, middle, and bottom panels, respectively. The line styles represent different magnetic dipole strengths, and the colors represent different accretion rates.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The efficiency ﹩L/(\dot{M}{c}^{2})﹩ of total luminosity Ltot and its components for two simulations with accretion rate of ﹩{\dot{M}}_{100}﹩ (top) and ﹩{\dot{M}}_{1000}﹩ (bottom). Each efficiency is denoted by a different color and line style.