adsabs/AstroCLIMB huggingface dataset:
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Evolution of best-fit X-ray spectral parameters, including logT in and log﹩{R}_{\mathrm{in}}^{* }﹩ in the diskbb component (top two panels), Γ and f sc in the simpl component (third and fourth panels). Note that the uncertainty of log(﹩{R}_{\mathrm{in}}^{* }/{R}_{{\rm{g}}}﹩) is greater than the uncertainty of ﹩{R}_{\mathrm{in}}^{* }﹩ by 0.44 dex (i.e., the uncertainty of M BH; Section 3.1), which is not included in the figure. Data are from model (1a) in Table 4, model (2a) in Table 5, Table 6, and Table 7. For parameters in model (2a), we assume an uncertainty of 10%. Fixed values are shown as semitransparent symbols. Background colors follow the scheme shown in Figure 16.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Galactic extinction-corrected 0.3–10 keV X-ray luminosity (L X, 0) as a function of hardness ratio for Swift/XRT detections only.
Paper: A Mid-infrared Flare in the Seyfert Galaxy NGC 3786: A Changing-look Event Triggered by an Obscured Tidal Disruption Event?
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Dohyeong Kim, Taehyun Kim
Figure caption: Light curves of NGC 3786 in the (a) g band from the ZTF, (b) WISE W1 band, (c) WISE W2 band, and (d) W1-W2 color. In panels (b) and (c), the gray circles denote photometric data from individual visits of WISE, and the blue circles represent the median values in each epoch. The error bars represent the 1σ uncertainty. The epoch of the mid-infrared (MIR) flare is highlighted by the red shaded area.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Rest-frame g-band light curve of AT2021ehb compared with that of the 30 TDEs presented by Hammerstein et al. (2022). The solid lines show the best-fit models (see the text for details). Data points and labeled names are only shown for TDEs with no discernible optical broad lines.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: A snapshot SED of AT2021ehb at δ t≈147 days. The data has been corrected for extinction (in UV/optical) and Galactic absorption (in the X-ray). The solid lines are the blackbody fits to UV/optical data (Section 4.1) and the XRT “s3” spectrum best-fit model (Section 4.4.5). The shaded region shows that the L bol is calculated in three energy ranges (see the text).
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Typical SEDs of AT2021ehb in five phases. The data has been corrected for extinction (in UV/optical) and column density absorption (in the X-ray). The solid lines are the blackbody fits to UV/optical data.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Spherically averaged profiles at approximately 80 dynamical times after periapse passage (left panels). We see that wave breaking has disturbed the outer layer of the object’s profile adding kinetic energy (which has both rotational and turbulent components) and heat, as traced by the specific entropy. The right panel shows the mass of the late-time atmosphere compared to the nonlinear mass by several measures. We find that the linear theory prediction and simulated periapse mass with ∣k  r  ξ  r ∣ > 1 correlate with the late-time mass with ﹩{ \mathcal M }\gt 1﹩. The total late-time shock-heated mass correlates with the periapse mass with ∣k  r (R 1)ξ  r ∣ > 1, which implies ∣δ v  r ∣ > c  s (R 1).
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Power in the l = 2 mode as a function of time and its damping. After periapse passage, we see that the mode decays exponentially, with a characteristic timescale that is shortest in the strongest encounters. This effect is so extreme that after ∼40 dynamical times, the closest periapse passage has weaker ongoing oscillations than the furthest periapse passage. These strong encounters generate shorter dissipation timescales due to the larger masses of shocked atmosphere material generated by the initial wave breaking. The second panel shows the dissipation rate associated with the exponential fits (the r  p  = 1.9 R 1 case is shown with a lower limit because of background material in our hydrodynamic models). The overall behavior is similar to that of our estimate of the dissipation efficiency, with ϵ th ∼ 1 and m atm equal to the wave-breaking mass at periapse (∣k  r  ξ  r ∣ > 1).
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Simulation results for the orbital energy exchanged with tides in eccentric passages of varying periapse distance (top panel) and the wave breaking mass as a function of oscillation energy (lower panel). The dotted lines in the upper panel show the predictions of linear theory for each of the Γs = γ = 1.35 and Γs = γ = 5/3 isentropic polytropes. The lower shows that despite differing levels of central concentration, the wave-breaking mass as a function of mode energy is similar, and follows a linear relationship implying approximately constant specific energy, as traced by contours in units of ﹩{v}_{1}^{2}={{GM}}_{1}/\,{R}_{1}﹩.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: Image of the molecular outflows in I16076. The background gray scale image is the ALMA 0.9 mm continuum image from Figure 1, and the black contours are set at three and six times the rms noise level, respectively. The red and blue circles correspond to redshifted and blueshifted CO(3–2) gas condensation, identified in the velocity cubes as parts of the outflows in the region (see Section 3.2). The driving sources of the ensemble of filaments (west) and the blueshifted monopolar outflow lobe (east) are marked with yellow stars.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: PV diagram of the CO(2–1) emission from the ensemble of filaments associated with I16076. The blueshifted and redshifted dots are extracted to analyze the CO condensations of the filamentary outflows emerging from the MM8 dense core. The black straight lines are plotted to link the yellow star, placed at the location of MM8 at 0 km s−1 (radial velocities are given with respect to the cloud velocity), and the tips of each of the 24 filaments of the ensemble. Better angular resolution is needed for better analysis of the filament kinematics.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: The redshifted (left panel) and blueshifted (right panel) CO(3–2) gas condensations detected in I16076. We identified 12 redshifted filaments and 12 blueshifted filaments, labeled RF and BF, respectively. The possible origin of the all filaments is marked with the yellow.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: The CO(3–2) spectrum integrated over the whole ensemble of filaments associated with MM8. The radial velocity is expressed relative to the system cloud velocity of −87.7 km s−1. The spectrum shows deep absorption by the parental cloud, but also two less prominent absorptions, at 23.4 and 44.5 km s−1, which are probably due to foreground clouds along the line of sight. There are also other spectral lines (HCCCN, 34SO2, CH3CHO, and CH3OH) that are much weaker than the main CO line.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: 3D representation of the dispersal outflowing event in I16076. The radial blueshifted and redshifted velocities are show with colors from blue to red. The LSR radial velocity scale bar (in km s−1 ) is shown to the right. The (0″, 0″, 0 km s−1) position is the origin of the plot and is marked by a black star, representing the origin of the dispersal outflow.
Paper: Possible Explosive Dispersal Outflow in IRAS 16076-5134 Revealed with ALMA
Authors: Estrella Guzmán Ccolque, Manuel Fernández-López, Luis A. Zapata, Tapas Baug
Figure caption: 0.9 mm continuum emission toward I16076 in color scale with gray contours (at 3, 5, 10, 15, 30, 40, and 45 times the rms noise level of 4 mJy beam−1). The synthesized beam, shown in the bottom right corner, is 0.″8 × 0.″7, with PA = 74.°6. The submillimeter continuum sources identified here are marked by the black dots.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Joint posterior distributions for the LRS retrieval of HD 4747 B. We omit the P–T profile parameters, which are better visualized by the P–T plot in Figure 6. The distributions for a few parameters are bimodal.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Joint posterior distributions for the HRS retrieval of HD 4747 B. We omit the P–T profile parameters, which are better visualized by the P–T plot in Figure 6.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The FeLoBAL outflows in our sample show a wide range of physical properties including ionization parameter (log U) and density (log n). The gray shaded bars represent the range of values among the tophat model bins for each BAL. For Gaussian opacity profile models or when the tophat bins for a given BAL had a single ionization and/or density parameter, the 2σ (95.45%) uncertainties from the MCMC posterior distributions are plotted as error bars. Some of the special BALs are marked as follows: red circles for overlapping-trough BALs (Section 6.4), blue diamonds for loitering BALs (Section 6.5), and green crosses for inflows. Left panel: the dashed line shows the location of the hydrogen ionization front as a function of ionization parameter. Right panel: the locations of the BAL gas from the central SMBH (log R) are marked as shaded areas for reference. They were calculated assuming the typical ranges of photoionizing photon flux used in our sample of FeLoBALQs (﹩\mathrm{log}Q\sim 55.5\mbox{--}56.5﹩ [photons s−1]).
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption:  Left panel: we found no strong correlations between the offset velocities and the physical properties of the BAL gas (log U and ﹩\mathrm{log}{N}_{H}-\mathrm{log}U﹩) for the whole FeLoBAL sample. Instead, there is a “v” shape with high-log U BALs present at the lowest and highest velocities (red and blue shades). Right panel: the widths of the BALs scale with the velocity offsets. The distribution roughly follows a one-to-one ratio (brown dotted–dashed line), which indicates that most of the FeLoBAL outflows are not detached from the emission line at rest. A linear scale was used in the region ∣v off∣ < 100 km s−1, and log scale was used elsewhere in the x-axis. Markers and error bars as in Figure 4.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The BALs have a wide range of distances from the central engine, ranging from a torus scale (∼pc) to a host-galaxy scale (∼kpc). The cyan squares mark the powerful outflows that have well-constrained physical parameters (log U and log n) and kinetic luminosity (L KE) greater than 0.5% of the bolometric luminosity of the quasar (L Bol). The powerful outflows are located in a various distances from the central black hole, and they have a variety of physical properties. The histogram on the y-axis shows the distribution of log R in our sample. There is a lack of FeLoBALs near ﹩\mathrm{log}R\sim 2﹩ [pc] (Section 7.1). A range of BAL cloud volume filling factors (or normalized radial widths, ﹩\mathrm{log}{\rm{\Delta }}R/R﹩) and two log n values are marked as shaded areas for reference. Markers and error bars as in Figure 4.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: Anatomy of the near-UV spectrum of an FeLoBAL quasar. SimBAL models for SDSS J1214+2803 showing some of the principal line transitions observed in FeLoBAL troughs are plotted. Top: the best-fit model has been divided by the ionic species that are the major contributors of the opacity in the near-UV bandpass for FeLoBALs. Bottom: the Fe II model has been further broken up into 4 different models depending on the lower-level excitation energy.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The best-fitting SimBAL models are plotted in red, along with the 2σ (95.45%) confidence models and unabsorbed continuum models in pink and orange, respectively. The binned data and the associated uncertainties are plotted in black and gray, respectively.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The kinetic luminosities (L KE) of the FeLoBAL outflows scale with the outflow velocities with the slope of ∼3. This relationship is expected from the definition of L KE. The scatter in the L KE direction can be mainly ascribed to the range of mass outflow rate (﹩\dot{M}﹩) of the outflows as well as gas physical conditions such as covering-fraction-corrected hydrogen column densities. The colors of the markers represent the locations of the outflows (log R), and for an FeLoBAL outflow at a given outflow velocity, larger log R will yield larger ﹩\dot{M}﹩ and greater L KE. We did not find any particular trend with log R and the properties plotted in the figure; however, the outflows with the highest velocities in our sample were all found to be within the vicinity of torus ﹩\mathrm{log}R\lesssim 1﹩ [pc]. The 5 BALs with inflows are not plotted.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The BALs with high log U have larger covering-fraction-corrected hydrogen column densities. The strong correlation between the two parameters is expected for FeLoBALs that require the gas column densities to be high enough to reach the hydrogen ionization front (﹩\mathrm{log}{N}_{H}-\mathrm{log}U\sim 23\,[{\mathrm{cm}}^{-2}]﹩). Markers and error bars as in Figure 4.
Paper: The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL 
Authors: Hyunseop Choi, 현섭 최, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, Gordon T. Richards
Figure caption: The best-fitting SimBAL models for six objects modeled using the modified partial-covering scheme. The best-fitting models and the unabsorbed continuum emission models are shown in red solid lines and blue dashed lines, respectively. Top: the FeLoBAL gas does not absorb the emission lines (green shaded region). Bottom: the FeLoBAL gas does not absorb both emission lines and a fraction of the continuum emission (green and orange shaded regions). The power-law partial-covering (log a) used in SimBAL alone could not model the heavy nonblack saturation seen in these spectra.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Dependence of r ring (left panel) and Σd ,ring/Σg (right panel) on η v K. In both panels, solid lines with marks show the resulting r ring and Σd ,ring/Σg. In the left panel, we plot the radial location of dust cells that are initially located in 49 au ≤ r ≤ 50 au with the shaded regions. We find that larger η v K makes the ring radius smaller. This is because dust grains with a certain τ s move faster for larger η v K.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Cumulative dust mass profile from the q2T20a1 run (left panel) and the q2T20a5 run (right panel). The ring locations r ring correspond to “cliffs” in the cumulative mass profiles. The gray dashed line and the black dashed line show M(<49 au) and M(<50 au) at t = 0 yr, respectively. One can see that the resulting dust rings in both runs consist of dust cells initially located around 50 au.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Time evolution of dust surface density (left panel) and dimensionless stopping time (right panel) obtained from the q2T20a5 run. As in the q2T20a1 run, we observe a local increase in dust-to-gas ratio by an order of magnitude. The dimensionless stopping time locally becomes larger than unity at t = 8.7 × 104 yr.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. I. First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
Authors: Ryosuke T. Tominaga, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Radial profiles of τ s in the q1T20a1 run (left panel) and the q3T20a1 run (right panel). In each run, τ s reaches unity in the most collapsed ring at t = 9.6 × 104 yr and 6.1 × 104 yr, respectively. The background τ s increases as r decreases in the q1T20a1 run and becomes larger than the background τ s in the q3T20a1 run. This means that dust grains drift inward more efficiently in the former run, which explains the trend that r ring is smaller for smaller q.