adsabs/AstroCLIMB huggingface dataset:
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The second-order, two-point stencil structure functions for the patchy (left) and filamentary (right) foreground RM. The green points indicate the SF for the initial sampled data (with extragalactic contribution), the red points represent the SF from the Gaussian extragalactic contribution that was added, and the blue points represent the SF after the 3σ cut was made on the data. The dashed lines represent the ﹩2{\sigma }_{\mathrm{RM}}^{2}﹩ asymptotes for each of the RMs considered. In the patchy foreground, the sampled RM has best-fit values of ﹩A={348.15}_{-2.60}^{+1.51}﹩ rad2 m−4, ﹩{\rm{\Delta }}{\theta }_{\mathrm{break}}={5.00}_{-0.07}^{+0.07}﹩ deg, ﹩{\alpha }_{1}={0.42}_{-0.00}^{+0.00},\,\mathrm{and}\,{\alpha }_{2}=-{0.07}_{-0.01}^{+0.01}﹩, while the best-fit values for the 3σ cut RM are ﹩A={295.07}_{-4.63}^{+1.02}﹩ rad2 m−4, ﹩{\rm{\Delta }}{\theta }_{\mathrm{break}}={4.00}_{-0.04}^{+0.05}﹩ deg, ﹩{\alpha }_{1}={0.49}_{-0.01}^{+0.00},\,\mathrm{and}\,{\alpha }_{2}={0.05}_{-0.01}^{+0.01}﹩ . With the filamentary foreground, the sampled RM has best-fit values of ﹩A={1549.08}_{-5.68}^{+1.50}﹩ rad2 m−4, ﹩{\rm{\Delta }}{\theta }_{\mathrm{break}}={6.00}_{-0.00}^{+0.05}﹩ deg, ﹩{\alpha }_{1}={0.33}_{-0.01}^{+0.00},\,\mathrm{and}\,{\alpha }_{2}=-{0.43}_{-0.00}^{+0.01}﹩, while those for the 3σ cut RM are ﹩A={1589.34}_{-2.59}^{+1.92}﹩ rad2 m−4, ﹩{\rm{\Delta }}{\theta }_{\mathrm{break}}={6.00}_{-0.02}^{+0.00}﹩ deg, ﹩{0.37}_{-0.00}^{+0.00},\,\mathrm{and}\,{\alpha }_{2}=-{0.56}_{-0.01}^{+0.01}﹩.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Reconstructed RM maps for each of the interpolation techniques for the patchy structures, saturated from −50 to +50 rad m−2. The color map represents RM, with red being positive and blue being negative. At the top center, we present the simulated foreground RM. From top left to bottom right, the reconstructions are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The plot on the left shows the data points (in blue). The Delaunay triangulation is shown in dotted blue lines, with a few selected circumcircles portrayed in red. The black lines show the edges of the Voronoi polygons. The plot on the right shows the recalculated Voronoi diagram when an interpolation point (in orange) is inserted into the figure. The orange lines show the edges of the Voronoi polygon of the interpolation point.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Simulated foreground RM maps for patchy (left) and filamentary (right) RM structures. The color bars represent RM in units of rad m−2 and are saturated from −50 to +50 rad m−2.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Reconstructed RM maps for each of the interpolation techniques for a foreground sky with filamentary structures, saturated from −50 to +50 rad m−2. The color map represents RM, with red being positive and blue being negative. At the top center, we present the simulated foreground RM. From top left to bottom right, the reconstructions are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Residual RM maps for each of the interpolation techniques in the case of a patchy RM sky. In every map, the residual RM for each pixel was calculated by finding the difference in the RM value between the reconstructed pixel and the pixel from the simulated foreground RM. From top left to bottom right, the reconstruction are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The sampling of the RM data points from the patchy (left) and filamentary (right) foreground RM, saturated from −100 to +100 rad m−2 after the 3σ cut has been made.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Reconstructed RM maps for each of the interpolation techniques for the patchy structures (with the data points having no extragalactic contributions), saturated from −50 to +50 rad m−2. The color map represents RM, with red being positive and blue being negative. At the top center, we present the simulated foreground RM. From top left to bottom right, the reconstructions are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Residual RM maps for each of the techniques in the case of a filamentary RM sky. In every map, the residual RM for each pixel was calculated by finding the difference in the RM value between the reconstructed pixel and the pixel from the simulated foreground RM. From top left to bottom right, the reconstruction are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The top figures display the power spectra of the reconstructed RM maps and the simulated foreground for the patchy sky (left) and the filamentary sky (right), and the bottom two figures display the power spectra of the residuals of the reconstructed RM maps for the patchy sky (left) and the filamentary sky (right), with both data sets having no extragalactic contributions.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: A histogram of the magnitude of the residual RM for all the techniques applied for the patchy RM sky (left) and a histogram of the magnitude of the residual RM for all reconstructions applied to the filamentary RM sky (right).
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: A plot of the Voronoi diagram for an interpolation point (in black) at the edges of the grid. The edges of the Voronoi polygons of the data points (in blue) are shown with black lines, and the Voronoi polygon for the interpolation point is shown in red. A dashed line represents an edge that extends to infinity.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: A histogram of the magnitude of the residual RM for all the techniques applied for the patchy RM sky (left), and a histogram of the magnitude of the residual RM for all reconstruction applied to the filamentary RM sky (right), with the data sets having no extragalactic RM contributions.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The top figures display the power spectra of the reconstructed RM maps and the simulated foreground for the patchy sky (left) and the filamentary sky (right), and the bottom two figures display the power spectra of the residuals of the reconstructed RM maps for the patchy sky (left) and the filamentary sky (right).
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: A plot of the convex hull (in red) of a random set of points. Voronoi edges that are unbounded are illustrated with dotted lines.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Zooming into a corner of the NNI RM reconstruction, highlighting the NaN values present at the edges of the interpolation region. The NaN values in this case are the gray pixels along the top right corner.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: PDF of the orbital energy of each star (in units of E tide = E tide1, given by Equation (14)) after binary breakup. The initial binary has e  b  = 0. The blue and orange solid lines represent the results for two different values of β  b : gentle encounters (β  b  = 0.7) and deep encounters (β  b  = 5). These PDFs are obtained by sampling all encounters with different phase angles and inclinations. Note that the PDF is not normalized to unity, because for a given β  b , only a fraction of the encounters lead to binary breakups; each PDF includes all encounters, not just those leading to binary breakups.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Reconstructed RM maps for each of the interpolation techniques for a simulated foreground with filamentary structures (with the data points having no extragalactic contributions), saturated from −50 to +50 rad m−2. The color map represents RM, with red being positive and blue being negative. At the top center, we present the simulated foreground RM. From top left to bottom right, the reconstructions are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Plots of the accuracy (measured in I res) of the interpolation techniques against the source density for the patchy (left) and filamentary (right) foreground RM structures with extragalactic RM contributions.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Residual RM maps for each of the interpolation techniques in the case of a patchy RM sky (with the data points having no extragalactic contributions). In every map, the residual RM for each pixel was calculated by finding the difference in the RM value between the reconstructed pixel and the pixel from the simulated foreground RM. From top left to bottom right, the reconstruction are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The fraction of binary breakups as a function of the dimensionless parameter ﹩{\beta }_{b}\equiv {r}_{\mathrm{tide}}^{b}/{r}_{p}﹩ for several different values of the initial binary eccentricity.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Plots of the accuracy (measured in I res) of the interpolation techniques against the standard deviation in the noise for the patchy (left) and filamentary (right) foreground RM structures with extragalactic RM contributions.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: Residual RM maps for each of the techniques in the case of a filamentary foreground (with the data points having no extragalactic contributions). In every map, the residual RM for each pixel was calculated by finding the difference in the RM value between the reconstructed pixel and the pixel from the simulated foreground RM. From top left to bottom right, the reconstructions are as follows: IDW1, IDW2, NNI, IM RBF, TPS RBF, and BRMS.
Paper: Interpolation Techniques for Reconstructing Galactic Faraday Rotation
Authors: Affan Khadir, Ayush Pandhi, Sebastian Hutschenreuter, B. M. Gaensler, Shannon Vanderwoude, Jennifer L. West, Shane P. O'Sullivan
Figure caption: The accuracy in terms of the goodness-of-fit parameter I res against the computational time in seconds. The plots show the results for data sets that have extragalactic contributions for the patchy (left) and filamentary (right) foregrounds.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The fraction of stellar collisions induced by binary–SMBH encounters as a function of the dimensionless parameter α ≡ a  b /R col, for several different values of ﹩{\beta }_{b}\equiv {r}_{\mathrm{tide}}^{b}/{r}_{p}=0.5,0.6,0.7﹩, and 0.8 (all are gentle encounters).
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: Distribution of the relative velocities between the two stars at collision for β  b  = 0.6 (upper panel) and β  b  = 5 (lower panel). The horizontal axis represents the radial velocity v col,r  and the vertical axis represents the tangential velocity v col,t . The red dashed line indicates the escape velocity ﹩{v}_{\mathrm{esc}}=\sqrt{2{{Gm}}_{12}/{R}_{\mathrm{col}}}﹩. Each blue dot in the figure represents the result of one simulation.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The same as Figure 5, except for deep encounters with β  b  ≳ 1. The solid lines correspond to β  b  = 1, 3, 5, and 10. The red dashed line represents the “billiard ball” model in which the collision fraction is 1/(π α).
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The same as Figure 2, except showing only the positive part of the energy (the negative part is perfectly symmetric with respect to the positive part) and for different initial binary eccentricities. The left panel represents gentle encounters (β  b  = 0.7), while the right panel represents deep encounters (β  b  = 5).
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The maximum (point) and average (star) values of the dimensionless energy ϵ rem (see Equation (23)) of merger remnants as a function of α for different β  b . Each point represents the result of a suite of simulations (about 104 runs). The jaggedness in the figure comes from numerical precision.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: PDF of the time difference Δt DD between double stellar disruptions for α = 8, β  b  = 20. The blue, orange, and green solid lines represent the results for M/m = 104, 105, and 106 (assuming m 1 = m 2 = m), respectively, while the vertical dashed lines represent ﹩{\left({\rm{\Delta }}{t}_{\mathrm{DD}}\right)}_{\max }﹩ given by Equation (15).
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The maximum eccentricity the binary can achieve during gentle binary–SMBH encounters as a function of β  b , calculated using the single-averaged secular Equations (18)–(19). Each blue dot represents the result of one calculation (with a specific set of initial conditions). Note that the gaps in the middle range of β  b s result from the finite samplings of the initial angles and phases.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: PDF of the remnant orbital energy for the gentle encounters (β  b  = 0.6, upper panel) and deep encounters (β  b  = 5, lower panel), each with two values of α. The vertical red dashed line is the dividing line that distinguishes whether a remnant is captured by the SMBH or not.
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The same as Figures 5 and 7, except for different initial binary eccentricities with two selected β  b .
Paper: Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision
Authors: Fangyuan Yu, Dong Lai
Figure caption: The same as Figures 5 and 7, except that the figure shows the fraction of the stellar merger remnants (among the stellar collisions) that are captured by the SMBH. Note that for β  b  = 5 and 10, we only consider α > 2−2/3 β  b  (see Equation (13)), to avoid stellar tidal disruption.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Profiles of primary-star stellar structure in a triple system relevant to CE interaction. Top panel: the radial evolution of the 10M ⊙ progenitor star of PSR J0337+1715 is shown as a function of time. The outer binary, assumed here to be composed of two 1M ⊙ Sun-like stars, is expected to be embedded within the envelope of the primary star, provided that it resides at separations below 400R ⊙. The vertical axis shows the radial extent of the primary in R ☉ units (left) and astronomical units (right). Bottom panel: the internal structure of the primary as calculated by MESA. The radial extent of the primary is shown in black. As the binary spirals, it is expected to be tidally disrupted at a radius given by the orange curve, while the yellow curve represents the tidal disruption radius of a single 1 M ⊙ Sun-like star. The shaded blue region represents the range of radii in which CE ejection is possible due to a single Sun-like star, since the binary will have already been tidally disrupted at the radius represented in orange. The pink curve represents the outer edge of the primary’s He core.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Diagram illustrating the proposed post-CE formation scenario for PSR J0337+1715 (T. M. Tauris & E. P. J. van den Heuvel 2014; E. Sabach & N. Soker 2015). The initial setup consists of three main-sequence stars: a primary (pink) with M ≈ 10M ⊙, a secondary (blue), and a tertiary (orange) with m 1 ≈ m 2 ≈ 1M ⊙, where M > m 1 + m 2. As the primary evolves, it will expand and the system will undergo a CE. The center of mass of the binary will sink toward the core of the primary until it reaches its tidal radius. The tertiary is ejected from the CE but remains bound to the system, while the secondary sinks and unbinds the envelope. This results in a hierarchical triple system in which the inner binary is composed of the primary’s core and the secondary.
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Diagnostics of CE flow properties. Top panels: flow morphology for a binary with a b,0 = 0.42 and q = 0.15 embedded in a CE flow with varying stellar density gradients. Density slices through the z = 0 plane surrounding the binary are displayed. From left to right, ε  ρ  = 0.5, 1.0, and 2.0. Bottom left panel: the net drag force on the center of mass of the binary projected onto the velocity of the center-of-mass vector, including contributions from dynamical friction,  F   d f , and accretion of linear momentum, ﹩{{\boldsymbol{F}}}_{\dot{p}}﹩. The drag forces are integrated over a spherical domain up to a radius 3.0 R  a  from the center of mass of the binary. Bottom right panel: the change in the binary separation, Δa b(t) = a b(t) − a b,0, as function of simulation time in units of R  a . For the case of a steep ε  ρ , the binary separation increases over time, while for a shallower ε  ρ , the separation decreases, as also found in the case of ε  ρ  = 0 (A. Antoni et al. 2019).
Paper: The Evolution of Binaries Embedded Within Common Envelopes
Authors: Alejandra Rosselli-Calderon, Ricardo Yarza, Ariadna Murguia-Berthier, Valeriia Rohoza, Rosa Wallace Everson, Andrea Antoni, Morgan MacLeod, Enrico Ramirez-Ruiz
Figure caption: Net drag force (with contributions from dynamical friction and accretion of linear momentum) projected along the direction of the center-of-mass velocity vector and mass accretion rate as a function of simulation time for a binary embedded in a CE flow. The simulation parameters are a b,0 = 0.42R  a , ε  ρ  = 0.3, and ﹩{ \mathcal M }\approx 1.0﹩. The period of the binary is ∼1.2R  a /v ∞. The effect on the binary is compared with that on a single point mass (a b,0 = 0). Top left panel: flow morphology for a single point mass. Top rightmost three panels: flow morphology for the binary case at three different times increasing from left to right. Density slices are taken for z = 0 plane surrounding the sinks. Bottom left panel: net drag force on the center of mass of the binary. The solid line shows the net force on the binary, while the dotted line shows the net force on the single mass particle. The different colors denote the distance from the center of mass to the integration radius. Bottom right panel: mass accretion rate for the single point mass and total accretion rate for the two sinks in the case of the binary. Lighter lines show the rate at each time step, and darker lines show the median values. The variations in the mass accretion rates are mainly driven by the periodic motion of the binary, which in turn modifies the density structure of the flow.