adsabs/AstroCLIMB huggingface dataset:
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Summary of our selection procedure to reveal Specter in Gaia DR3 data. Top: reflex-corrected proper motions in our transformed great circle coordinates, after applying an isochrone filter to select stars at ≈12.5 kpc. Our proper motion selection is shown with a red ellipse, and is centered on the mean proper motion of the H3 members. Middle: CMD of stars that lie in the proper motion ellipse shown in the top panel, without any CMD filtering applied. We overlay a fiducial 13 Gyr MIST isochrone with [Fe/H] = −1.8 and [α/Fe] = +0.3. Bottom: spatial density of stars that pass both the PM and CMD filters, smoothed with a 1.°5 Gaussian kernel. We overlay the spectroscopic members and their predicted orbit.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Comparing the luminosity, size, and metallicity of Specter to known streams and intact structures. Left: stream widths (Gaussian σ) and luminosities for several dwarf and GC streams from Shipp et al. (2018). We overlay intact (gravitationally bound) dwarfs and GCs, using the half-light radius as a proxy for characteristic size (McConnachie 2012; Baumgardt et al. 2020; Vasiliev & Baumgardt 2021). Middle: luminosity–metallicity relation for Specter, alongside an updated sample of intact dwarfs from McConnachie (2012) and dwarf streams from Shipp et al. (2018). Right: mean metallicity and intrinsic metallicity spreads for streams from Ji et al. (2020). We overlay intact dwarfs and GCs compiled by Willman & Strader (2012), omitting error bars for clarity.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Top: H3 spectra for seven members in Specter, with the best-fitting MINESweeper model overlaid in red. The topmost star is the BHB, for which a reliable metallicity cannot be estimated. A masked telluric region is shown in gray, and we indicate strong Fe I lines in blue. Bottom: comparison between H3 spectra for the most metal-poor member in Specter, and a reference star at higher metallicity selected from the H3 catalog to have similar temperature, surface gravity, and spectral signal-to-noise ratio. Both spectra are smoothed with a 5 pixel boxcar. Note in particular the Fe line at ≈5170 Å that is much weaker in the Specter member than the reference star. We emphasize that the full-spectrum-fitting MINESweeper routine picks up on aggregate spectral details that are difficult to discern by eye. Regardless, this comparison reassures us about this member’s metallicity.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Mixture modeling the spatial structure of Specter. Top panel: Observed spatial density of stars that pass our proper motion and isochrone selection. We overlay the fitted mean ϕ 2 of the Gaussian component in each ϕ 1 bin, along with the predicted orbit of the H3 member stars. Second panel: the density of stars in the Gaussian stream component of each bin. Third panel: the standard deviation of the Gaussian component, transformed to physical units using the distance predicted by the orbit model. Fourth and bottom panels: median and standard deviation of the proper motions of stars in the Gaussian component.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Top: 1σ–3σ confidence contours derived by fitting a grid of MIST isochrones to the six non-BHB spectroscopic members in Specter. The mean H3 spectroscopic metallicity is overlaid. Bottom: Pan-STARRS CMD of PM-selected members in the inner region of the stream, with the spectroscopic members highlighted as red stars. The overdensity of turnoff stars is best matched by a ∼13 Gyr isochrone and is inconsistent with an isochrone younger than ∼12 Gyr at this metallicity.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Tinsley–Wallerstein diagram of Specter members using measurements from H3, excluding the BHB star. We overlay abundance measurements for ultrafaint dwarf galaxies with similar luminosities (Frebel et al. 2014; Ji et al. 2016). We also show stars in the Sextans dwarf galaxy observed by H3, which should be on an identical metallicity scale to the Specter stars.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Demonstrating Specter’s significant RV signal in the H3 data set. Top: equatorial PMs of CMD-selected giants in H3 within 25° of Specter, with nine selection regions overlaid near Specter’s mean PM. Bottom: galactocentric RV distributions in each PM selection region. Specter stands out as a sharp spike in the RV distribution, and there are no similar spurious spikes in other PM-selected regions.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Specter in various integrals of motion. In gray we show the sample of giants from the H3 Survey. We highlight two known retrograde structures following the selections in Naidu et al. (2020), Arjuna/Sequoia/I’itoi in green, and Thamnos in magenta.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Comparing the observed orbital track, distance, and proper motions of Specter to some nearby known streams in the galstreams library.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Radial profiles of dust surface density Σd (first row), dimensionless stopping time τ s (second row), the collision velocity Δv pp (third row), the effective turbulence strength α eff (fourth row), and the dust-to-gas ratio in the sublayer ε s (fifth row). We also plot ε mid with a dashed line in the bottom panels. We show the results with and without the effects of the backreaction in the right and left panels, respectively. Different lines on each panel show profiles at different times (see the legend on the first row). Dust grains are not so large yet at t = 2.0 × 103 yr (τ s ≪ 1, light blue line), and thus the profile of Σd at this time step is a line of 0.01Σg (see the first row). We note that τ s is less than 10−2 at t = 2 × 103 yr, and thus the light blue line does not appear on the panels in the second row.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The resulting structures in the a1vf10BR run. (Top panel) The radial profiles of dust surface density (dark blue line) and dust size a (red line) are shown. We find that the sufficiently evolved ring shows a plateau structure in the dust surface density profile. This is in contrast to the result of the a1vf10 run (the left panels of Figure 3) and of Paper I. The dust sizes increases locally up to the size of τ s = 1, which is consistent with the result in Paper I. (Bottom panel) The radial profiles of the mean drift velocity ﹩\left\langle {v}_{r}\right\rangle ﹩ (black line), the total velocity v  r  (blue dashed line), and the diffusion velocity (gray line) are shown.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The dust collision velocity Δv pp on the r − t plane obtained from the a1vf10 run. Each colored line shows the trajectory of each dust-cell boundary. The color of the lines represents the magnitude of Δv pp. We arrange the line color so that a line is highlighted in light gray if Δv pp is larger than 10 m s−1. Since our method is based on the Lagrangian cells, the dust surface density is larger at radii where more lines concentrate. We note that we used a reduced number of dust cells to plot this figure.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The radial profiles of the collision velocities due to the turbulent motion (red lines), the radial drift (orange lines), and the azimuthal drift (purple lines) at the final time step. The black line is the total collision velocity. The solid lines show the collision velocities in the presence of the backreaction while the dashed lines show those in the absence of the backreaction. The dust grains are faced with the fragmentation if the colored or black lines cross the gray line. We can see that the backreaction reduces the collision velocities in the ring (r ≃ 31 au), and the total collision velocity becomes less than v frag.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The ratios α eff/α 0 and ε mid/ε mid,0 as a function ε mid (see also Equations (7) and (12)). In most of the present simulations in Section 3, the turbulence strength α eff becomes smaller than α 0 by a factor of ≃2–5 (see Figure 3). From this figure, we see that ε mid is in the range of ≃1–4, and the difference between ε mid and ε mid,0 is a few in such a case.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Time evolution of τ s (black solid line), Δv pp/v frag (red solid line), ε s (purple dashed line), and α eff/α eff(t = 0) (dark purple dashed line) of the dust cell whose τ s reaches unity at the final time step. The thin lines correspond to the evolution of dust cells of i ring − 15 ≤ i ≤ i ring + 15, where i is the cell number, and i ring is the cell number of the dust cell whose τ s reaches unity at the final time step.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The collision velocity Δv pp as a function of τ s for Σd/Σg = 10−3 (black line), 10−2 (purple line), and 10−1.5 (orange line). We assume α 0 = 1 × 10−4 for each case.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Histogram of the ring mass from the a1vf10BR run. We conduct another five runs for the same parameter but with different phases of initial perturbations and compile the results. The ring mass is defined as dust masses within the FWHM of the dust surface density.
Paper: A Ghost in Boötes: The Least-Luminous Disrupted Dwarf Galaxy
Authors: Vedant Chandra, Charlie Conroy, Nelson Caldwell, Ana Bonaca, Rohan P. Naidu, Dennis Zaritsky, Phillip A. Cargile, Jiwon Jesse Han, Benjamin D. Johnson, Joshua S. Speagle, 佳士 沈, Yuan-Sen Ting, 源森 丁, Turner Woody
Figure caption: Identification of spectroscopic members from H3 Survey data. The black points denote all H3 objects in the 10° × 10° field of view shown in the top left panel, orange crosses denote PM-selected stars that were specifically followed up for this work, and the red points are our final Specter members. We show the ϕ 2 = 0 line that defines our great circle coordinate frame. In the top right CMD, we overlay an [Fe/H] = −1.8, 13 Gyr MIST isochrone, as well as the BHB ridgeline from Deason et al. (2011). Our members lie on the same isochrone, have near-identical proper motions and radial velocities, and are systematically metal-poor with spectroscopic [Fe/H] < −1.5. We also show the tentative LAMOST member described in Section 2.3.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Percentage error of nuclear energy generation e nuc with respect to percentage error of updated mass fractions ﹩{X}_{k}^{\mathrm{out}}﹩ at different initial conditions.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Profiles of mass fractions and nuclear energy generation rate along the x-center line for the V-shaped flame problem at final time t = 12 μs using a parallel DNN in the predictor step of second-order Strang splitting algorithm.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: (a) Profile of species mass fractions and nuclear energy generation rate at final time t = 12 μs, and (b) validation results using symmetric mass fraction loss function for full DNN.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Final profiles of mass fractions and nuclear energy generation rate at t = 12 μs (left), and parallel validation results (right) using symmetric mass fraction loss function for DNN1.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: Total loss of training and validation data for 500 epochs during the validation phase.
Paper: Neural Networks for Nuclear Reactions in MAESTROeX
Authors: Duoming Fan, Donald E. Willcox, Christopher DeGrendele, Michael Zingale, Andrew Nonaka
Figure caption: (Left) Relative timing plots of subroutines in MAESTROeX. (right) Comparison of runtimes of the computational reaction kernel using VODE and DNN models.
Paper: Variability from Thermoresistive Instability in the Atmospheres of Hot Jupiters
Authors: Raphaël Hardy, Andrew Cumming, Paul Charbonneau
Figure caption: Frequency f in day−1 of the instability domain for the atmospheres of HJ with magnetic field strength of B = 10 G and B = 40 G and an acceleration of ﹩\dot{v}=1\,\mathrm{cm}\,{{\rm{s}}}^{-2}﹩ in green and red, respectively. The blue region represents the results for B = 3 G and ﹩\dot{v}=1.4\,\mathrm{cm}\,{{\rm{s}}}^{-2}﹩. The parameters used to solve Equations (8)–(10) were obtained the same way as in Figure 3. For ﹩\dot{V}﹩, we applied the exponential decay, ﹩\exp (-P/\mathrm{bar})﹩ and used the scaling presented in Equation (21) to transform ﹩\dot{v}﹩ to its dimensionless counterpart, ﹩\dot{V}﹩. Frequencies are recast in dimensional units using the Alfvén time, as given by Equation (22). The black lines represent the edges of the unstable regions.
Paper: Variability from Thermoresistive Instability in the Atmospheres of Hot Jupiters
Authors: Raphaël Hardy, Andrew Cumming, Paul Charbonneau
Figure caption: Values of Rm, E  η , Ec, and τ shown as a function of temperatures and pressures relevant for HJ atmospheres. The magnetic Reynolds number is taken from Equation (19). The temperature sensitivity of the magnetic diffusivity is defined as ﹩{E}_{\eta }\equiv -{T}_{3}d\mathrm{ln}\eta /d\mathrm{ln}T﹩. The Eckert number is taken from Equation (18). The radiative cooling time is taken from Table 2 of Showman et al. (2008) with a linear interpolation at higher temperatures and was turned into dimensionless form with the ohmic time t Ohm from Equation (20). We assume a surface gravity equal to that of Jupiter and a magnetic field of B = 10 G (note that Rm ∝ B, Ec ∝ B 2,E  η , and τ are independent of B). The black lines represent the isocontours of the presented parameters in each panel.
Paper: Variability from Thermoresistive Instability in the Atmospheres of Hot Jupiters
Authors: Raphaël Hardy, Andrew Cumming, Paul Charbonneau
Figure caption: Time evolution of velocity v, toroidal field b, temperature T, and effective magnetic Reynolds number ﹩{\mathrm{Rm}}_{\mathrm{eff}}=\mathrm{Rm}| v| /\tilde{\eta }﹩, showing the three different outcomes: (a) the system reaches steady state (Rm = 0.1, τ = 1, Ec = 1, E  η  = 0, ﹩\dot{V}﹩ = 0.1), (b) oscillations (Rm = 0.1, τ = 1, Ec = 1, E  η  = 10, ﹩\dot{V}﹩ = 0.1), and (c) bursts (Rm = 0.01, τ = 10, Ec = 1, E  η  = 10, ﹩\dot{V}﹩ = 0.01).
Paper: Variability from Thermoresistive Instability in the Atmospheres of Hot Jupiters
Authors: Raphaël Hardy, Andrew Cumming, Paul Charbonneau
Figure caption: Thermoresistive instability domain using Equation (17) with ﹩\tilde{\eta }{T}^{2}=1﹩, combined with Equation (7) of Menou (2012a). The default magnetic drag law (n  s  = n  e  = 1) was used, as well as the exponential decay at higher pressures: ﹩\exp (-P/\mathrm{bar})﹩. The green and red regions correspond to input zonal velocities of V  ϕ  = 7 km s−1 with magnetic fields of B = 10 and 40 G, respectively. The blue region represents the instability region for V  ϕ  = 10 km s−1 and B = 3 G. These parameters were chosen to replicate Figure 1 of Menou (2012a) with Equation (17). The black lines represent the edges of the unstable regions.
Paper: Variability from Thermoresistive Instability in the Atmospheres of Hot Jupiters
Authors: Raphaël Hardy, Andrew Cumming, Paul Charbonneau
Figure caption: Angular frequency ω/ω  A  of the oscillation cycle as a function of ﹩\dot{V}﹩ and τ for (a) Rm = 0.1, Ec = 1.0 and (b) Rm = 0.01, Ec = 1.0 and as a function of Ec and τ for (c) Rm = 0.01, ﹩\dot{V}=0.1﹩ and (d) Rm = 0.01, ﹩\dot{V}=0.01﹩. The magnetic diffusivity sensitivity is kept constant for all panels at E  η  = 10.0. The black lines represent the isocontours of the angular frequency ω/ω  A . The solid red lines represent the instability criterion of Equation (15); the system should be oscillating above it. The dashed red lines represent the analytic estimate of Equation (14) for the boundary between bursts and Alfvénic oscillations.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The dust-to-gas surface density ratio ε (left panel) and the dust-to-gas ratio at the midplane (right panel) around the dust cell (i ringth cell) whose τ s reaches unity at the final time step. The marks show the averaged values for i ring − 15 ≤ i ≤ i ring + 15 where i is the cell number. The error bars correspond to the standard deviation. The surface density ratio slightly increases as α 0 while the ε mid is roughly constant. The black dotted line in the left panel shows the dust-to-gas surface density ratio that we semianalytically derive using ε mid = 1 and τ s = 1. The black dotted line roughly reproduces the α 0-dependence of ε.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Summary of the parameter study. The open circles mean that coagulation instability (CI) develops, radially concentrates dust grains, and leads to τ s → 1 in the resulting ring. The cross marks mean that the instability is inefficient and does not increase τ s up to unity because of too small v frag or because of too large α 0 that reduces the growth rate of the instability as found in Paper I.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The results of the a3vf10BR run. The left and right panels show the time evolution of Σd and τ s. The densest dust ring forms at inner radii compared to the a1vf10BR run (see also Appendix C). This is due to large diffusion that reduces the growth rate of coagulation instability. The dust size increases up to the size of τ s = 1 in the resulting ring. We note that τ s is less than 10−2 at t = 2 × 103 yr, and thus the light blue line does not appear in the right panel.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The results of the a1vf10BR run with the sublayer thickness of ∣z∣ ≤ 3H d. The left and right panels show the time evolution of Σd and τ s. We note that τ s is less than 10−2 at t = 2 × 103 yr, and thus the light blue line does not appear in the right panel. The dust-to-gas ratio in the ring is larger than the run with the sublayer thickness of ∣z∣ ≤ H d (Figure 3). This is because the drift deceleration due to the backreaction is weaker and coagulation instability grows more efficiently.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The radial profiles of the collision velocities at the final time step obtained in the a3vf10BR run. The colored solid (dashed) lines represent each collision velocity component in the presence (absence) of the backreaction as in Figure 7. The dominant velocity component is the turbulence-induced velocity in the a3vf10BR run (see the red lines). We can see that the backreaction reduces the collision velocities in the ring, and the total collision velocity becomes less than v frag.