adsabs/AstroCLIMB huggingface dataset:
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Unfolded spectra of the XMM-Newton observation in 2011 (red) and XMM-Newton + NuSTAR observations in 2021 (gray). Both the 2011 and 2021 spectra are modeled using the phenomenological model. The 2011 observation is modeled assuming a photon index of 1.45.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Distributions of the 2–10 keV flux, column density, and 2–10 keV intrinsic luminosity measured in the 10,000 simulations. The black dotted line shows the 2021 best-fit source properties. The red dashed line and the red shaded area show the 2011 measured source properties and their 1σ uncertainty, respectively.
Paper: A Search for Collisions and Planet–Disk Interactions in the Beta Pictoris Disk with 26 Years of High-precision HST/STIS Imaging
Authors: Arin M. Avsar, Kevin Wagner, Dániel Apai, Christopher C. Stark, Mark C. Wyatt
Figure caption: Uncertainty maps for each epoch of data in our sample. The higher levels of noise seen in the inner disk are due to the noise introduced by PSF subtraction residuals and higher levels of photon noise.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Schematic rendering illustrating how to compute the column density in the SALT formalism along an arbitrary line of sight. Top left: a spherical outflow (salmon) surrounding a star-forming region (light green). We aim to compute the column density along the path shown in light blue. Top right: 2D projection of the outflow. Bottom left: to avoid integrating inside the source, we begin our calculation of the column density starting from the surface of the star-forming region, or a distance L from the l ξ-plane. We compute the column density along this path until it terminates at the edge of the outflow a distance U from the l ξ-plane. Bottom right: we can account for a biconical outflow geometry by setting the density field to zero everywhere along the light blue path that falls outside the boundary of the bicone. We can determine whether a location along the path falls outside the bicone by checking if the angle subtended by the axis of the cone, ﹩{\hat{r}}_{\mathrm{BC}}﹩, and the location of the point, ﹩{{\boldsymbol{r}}}_{\mathrm{LOS}}﹩, denoted by ﹩{\alpha }^{{\prime} }﹩, is greater than the opening angle of the cone, α.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: An Illustration of how the observed synchrotron intensity structures are regulated by the Alfvén Mach number M A and inclination angle γ. Within all three panels, these intensity structures elongate along the POS magnetic field where l ∥ > l ⊥. Structures 1 and 2, depicted in panels (a) and (b) are projected onto the POS with identical inclination angles γ 1 = γ 2, yet exhibit different magnetization with ﹩{M}_{{\rm{A}},1}^{-1}\gt {M}_{{\rm{A}},2}^{-1}﹩. Notably, the anisotropy observed, represented as l ∥/l ⊥, in the weakly magnetized Structure 2 is less pronounced than in Structure 1. Structure 2 is less straightened because the weak magnetic field has more fluctuations. Comparatively, Structures 1 and 3—showcased in panels (a) and (c)—possess equivalent magnetization ﹩{M}_{{\rm{A}},1}^{-1}={M}_{{\rm{A}},3}^{-1}﹩, but divergent inclination angles with γ 1 > γ 3. The observed anisotropy decreases with smaller γ, though it is crucial to note that the straightness of Structure 3 remains unaffected by this projection. Modified from Y. Hu et al. (2024a).
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Architecture of the CNN model. The input image is a 22 × 22 cell map cropped from the synchrotron intensity map. The network outputs the prediction of the magnetic field’s POS orientation angle ϕ, inclination angle γ, or the Alfvén Mach number M A. Modified from Y. Hu et al. (2024a).
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Spectral parameters obtained from time-resolved spectroscopy of X-ray bursts from 4U 1820–30 using a variable persistent emission model. The evolution of the six most representative bursts is shown. The black circle and gray square in the fifth panel indicate the total and the blackbody bolometric fluxes in the 0.1–100 keV range, respectively.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Relation between various burst and persistent spectral parameters. Unabsorbed persistent flux in 0.5–10 keV in a unit of 10−9 erg s cm−2. Factor﹩{}_{\max }﹩: maximum value of scaling factor (f  a ) observed from a burst. Burst fluence: the total sum of blackbody flux integrated over each time interval from time-resolved spectroscopy in a unit of erg cm−2. Peak flux: maximum value of total (black circle) and blackbody (gray square) fluxes observed from each burst in erg s cm−2, respectively. The preburst blackbody temperature and radius (in km) are denoted with kT inner and Radiusinner, respectively. ﹩{{R}}_{{\rm{PRE}}}﹩ corresponds to the maximum radius attained during these PRE bursts.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Flux–temperature diagram from time-resolved spectroscopy of all 15 X-ray bursts of 4U 1820–30. The left (a), middle (b), and right (c) panels are from time-resolved spectroscopy of bursts using three different spectral approaches, such as the variable persistent emission model, variable preburst component method, and reflection model, respectively. Bolometric blackbody flux is shown with black solid dots, where the red plus symbol represents total model flux. The constant radius contours are also marked by dashed diagonal lines, assuming a distance of 8.4 kpc. The radius contours are not color corrected (see, e.g., F. Garcia et al. 2013; V. F. Suleimanov et al. 2017). The horizontal dotted line corresponds to the PRE flux level.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Spectral parameters obtained from time-resolved spectroscopy of three representative bursts from 4U 1820–30 using a combination of blackbody and reflection model at a fixed preburst emission. The black circle, gray square, and blue triangle in the sixth panel indicate the total model flux, blackbody flux, and reflection flux in the 0.1–100 keV range, respectively.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Spectral parameters obtained from time-resolved spectroscopy of three representative bursts from 4U 1820–30 using the second modeling approach. The black circle, gray square, and black triangle in the sixth panel indicate the total model flux, burst blackbody flux, and the second blackbody flux from the disk in the 0.1–100 keV range, respectively.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: NUV-B15 image of NGC 4151, the yellow circles correspond to a radius of 20 pixels (8.″3; 1 pixel ∼0.″416). The background is taken from within the galaxy with a relatively clean region.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: The SXT image of NGC 4151 (obs4), the yellow circle (radius ﹩=15^{\prime} ﹩) shows the source extraction area.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: The 3–10 keV X-ray burst light curve of Burst #11 at a bin size of 0.125 s (black). The contours of dynamical power spectra showing the burst oscillations at 716 Hz are included. Contours refer to Z 2 > 10 (blue) and >15 (red) up to the maximum with steps of 2.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Summary of the temporal evolution of the relative correlation function ﹩\tilde{\omega }(\theta )﹩ at θ = 36° (same angular scale of the orbital pole dispersion of the seven more clustered satellites in the VPOS). As in Figure 6, the correlation function was computed in 106 randomly chosen DM particles in the outer halo (50–150 kpc). Positive (negative) values of ﹩\tilde{\omega }(\theta )﹩ indicate an enhancement (decrease) of clustering within θ = 36°. The five LATTE halos with massive satellites are shown with color lines, while the two halos without massive satellites are shown in black. The arrows represent the first pericentric passage of a massive satellite in each halo. In most of the halos, changes in ﹩\tilde{\omega }(\theta )﹩ occur after the pericentric passages. The strongest clustering at this angular scale is seen in m12b (blue line), which is the best LMC analog. However, there is also a noticeable enhancement in clustering in m12r (orange line), which has three massive satellites. In systems that do not have a massive satellite during this time window, like m12i and m12m, these changes in ﹩\tilde{\omega }(\theta )﹩ are within 0.5, which is the lowest across all the halos.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Mean values of the orbital poles of all the subhalos (upper panel) and satellite galaxies (bottom panel) with masses ≥107  M ⊙ and within 50–150 kpc in m12b (left panel) and m12i (right panel). Variations in the mean orbital poles are seen at the pericentric passages (vertical dashed lines) of the massive satellite galaxies. In both m12b and m12i the changes are primarily in the longitudinal orbital poles l op, after the pericenter of the satellites (blue dashed lines). In m12i, there is an increase of the mean close to the passage of the satellite at ≈8 Gyr. In the satellite galaxies (bottom panels) the mean values are more noisy given the lower number of satellites compared to subhalos. Shaded regions show the distribution of the mean orbital poles of DM subhalos after downsampling to the same number of satellite galaxies. In m12b, the mean values of l op increase after pericenter the opposite trend as seen in the subhalos.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: All-sky orbital poles density distribution for DM particles (gray color map) between 50 and 150 kpc. Orbital poles of subhalos and satellite galaxies are shown with open and solid yellow circles, respectively. Each row corresponds to a different time in the evolution of the halos and each column represents a different halo m12c, m12f, m12m (no massive satellite). The orbital poles of the particles were computed after rotating the disk into the x–y plane and removing the particles from the most massive subhalos. The density of orbital poles was computed using HEALPIX with HEALPY (K. M. Górski et al. 2005).
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Dispersion of the orbital poles computed using subhalos with masses ≥107  M ⊙ and within 150 kpc in m12b (left panel) and m12i (middle panel). The gray-shaded regions show the dispersion in the orbital poles of the DM subhalos after downsampling to the same number of satellite galaxies. The dispersion in the orbital poles of the MW–LMC analog (m12b) decreases for both subhalos and satellites between the pericentric passages of the satellites (blues dotted lines). Note that the decrease in the dispersion of the satellites is larger than in the subhalos. In m12i, on the other hand, the subhalos dispersion is unaltered, while in the satellites, there is an increase after the pericenter of the low-mass satellite.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Temporal evolution of the spherical standard distance Δsph of the k closest orbital poles of the top 11 massive satellites in the MW–LMC analog m12b (left panel) and m12i (right panel). Smaller values of Δsph correspond to more clustered orbital poles. During the first pericentric passage of the massive satellite in m12b, Δsph changes rapidly and reaches its minimum. Dashed lines show Δsph close to the pericenter passage, while the dotted lines show the times closer to the satellite’s infall. In contrast with the evolution of Δsph in m12i, the spread in the values of Δsph reaches ≈30°, almost twice as in m12i.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Temporal evolution of the correlation function for five LATTE halos, m12c (first panel), m12f (second panel), m12m (third panel), m12r (fourth panel), and m12r (fifth panel). The correlation function is computed with 106 DM particles randomly selected within 50–150 kpc. Red colors show an increase in the probability of finding pairs at a given angular distance (θ). The probabilities are roughly constant time, however, when a massive satellite is at pericenter the probability distribution increases at a smaller angular distance.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Same as Figure 13, but for m12r (left panels), and m12w (right panels). Major changes in the distribution of orbital poles in m12r change through the evolution of the halo. Note that his halo has three major mergers after 10 Gyr, which is where most of the changes in the pole distribution happen. For m12w, the changes happen early on in the distribution of poles.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Galactocentric distances (upper panels) and velocities (lower panels) of the massive satellites in m12c, m12f, m12m, m12r, and m12w. Blue vertical lines illustrate the first pericenter passage of the massive satellites. In m12r, m12w there are multiple satellites. The transparency of the lines is proportional to the mass of the satellites.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Velocity of the COM of the host halos as a function of cosmic time. The velocity is measured with respect to the halo’s velocity at t = 6.2 (z = 1). Drastic velocity changes happen when massive satellites approach pericenters (indicated by the vertical blue dashed line). Changes up to 80 km s−1 can occur (for example in m12r) in short periods of time.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Superposition of visual outburst light curves of EX Dra, constructed from observations made by the AAVSO and the VSNET. The x-axis is time relative to the onset of the outburst. Crosses indicate measurements of the outbursts at the epoch of the observations of R. Baptista & M. S. Catalán (2001), while small dots are measurements of outbursts at other epochs. The blue points with error bars are the result of applying a median filter to this data set. R-band out-of-eclipse magnitudes from observations of R. Baptista et al. (2000) are shown as filled circles along with their uncertainties.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of the accretion disk of U Gem obtained from our simulations for an event of enhanced mass of 106 s. Top panel: The luminosity of the disk as a function of time (in units of days). Middle panel: The radius of the disk in units of orbital separation a. Bottom panel: The mass-transfer rate (solid line) and the mass-accretion rate over the primary (dotted line).
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Best-fit simulation in the case of local blackbody emission. The input parameters for this simulation are shown in the body of the figure together with the χ 2 value of the fit. Upper panel: The points with error bars are the same as in Figure 9. The solid lines are the magnitudes in the V (green) and R (black) passbands of the simulated accretion disk. Bottom panels: The residuals of each fit.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of the accretion disk for a variable deposit. Analogous to Figure 2, but the dashed lines in the two upper panels represent the results obtained in Section 2. In the middle panel, the green and red curves correspond to R  c  and R  p , respectively.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of optical depth (at 5038 Å, top panel) and effective temperature (bottom panel) for the simulations of Figure 7. The horizontal dotted line in the top panel marks the τ = 1 limit, below which the disk gas becomes optically thin. Temperatures in the bottom panel are computed using the blackbody (dashed lines) and gray atmosphere (solid lines) models for the disk emission. The notation is similar to that of Figure 3.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of surface density (top panel) and effective temperature (bottom panel) obtained from our simulations. The time corresponding to each curve is indicated in the figure legend. The dotted vertical line indicates the position of the circularization radius.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of the accretion disk with α = 5. Analogous to Figure 2, but the dashed lines in the two upper panels are the results obtained in Section 2.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of the accretion disk for a quadri-Gaussian event. Analogous to Figure 2, but the dashed lines in the two upper panels are the results obtained in Section 2.
Paper: Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Wagner Schlindwein, Raymundo Baptista
Figure caption: Time evolution of the V magnitude of the accretion disk. The local emission from the disk is modeled using a blackbody (blue) or gray atmosphere (red).