adsabs/AstroCLIMB huggingface dataset:
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: WISE W2-band Tully–Fisher relation of the FGLR galaxies using FGLR distance moduli for the calculation of absolute magnitude. The green line corresponds to the zero-point obtained with these galaxies. The galaxy in gray is NGC 3109. It is not used for the zero-point fit.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: WISE W1-band Tully–Fisher relation of the FGLR galaxies using FGLR distance moduli for the calculation of absolute magnitude. The green line corresponds to the zero-point obtained with these galaxies. The galaxy in gray is NGC 3109. It is not used for the zero-point fit.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: Curved I-band Tully–Fisher relation of the FGLR galaxies.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: Curved WISE Tully–Fisher relations of the FGLR galaxies. Top: W1; bottom: W2.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Left: distributions of 0.5–2.0 MeV nucleon−1 3He/4He (red solid line) and 386 keV nucleon−1 Fe/O (blue dashed line). The two vertical dotted lines indicate the SSW 3He/4He ratio (G. Gloeckler & J. Geiss 1998) and Fe/O ratio (R. von Steiger et al. 2000). Right: scatter plot of 3He/4He versus Fe/O. The three numbers indicate the Spearman correlation coefficient, the p-value, and the sample size. Note that outlier event #4 (3He/4He ∼ 4 × 10−1) and event #12 (3He/4He ∼ 2 × 10−1) are not considered. Blue squares mark events associated with jets at the source; red circles denote events without observed jets. White crosses represent events with Fe and O time profiles that differ from the remaining events (see text). The blue shaded histogram (left panel) excludes these events. Dotted horizontal and vertical lines indicate SSW values.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Ratios of 3He/4He and Fe/O as a function of the total 0.3–0.5 MeV nucleon−1 3He count integrated over the 24 hr preceding the onset of the 3He intensity increase. Blue squares indicate events associated with jets at the source; red circles denote events where no jets were observed.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Element abundance ratios relative to oxygen (O) plotted against Fe/C for the final set of 15 events listed in Table 2. Events associated with jets are shown as filled triangles; those without jets are shown as open triangles. The two numbers below each element label represent the Spearman correlation coefficient and the corresponding p-value. For clarity, some abundance ratios have been scaled by the multiplicative factor indicated. Open black circles mark the corresponding average GSEP abundances from M. I. Desai et al. (2006).
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: 3He/4He and Fe/O versus the absolute value of the longitudinal separation between the ACE magnetic footpoint at 2.5 R⊙ from the Sun center and the flare location. Blue squares indicate events associated with halo CMEs, and red circles indicate events associated with partial halo CMEs. Points marked with white crosses (right panel), as well as the the three numerical values shown, have the same meaning as in Figure 5.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: LASCO C2 running-difference images. Left: the two adjacent CMEs, shown 30 minutes before the X-ray flare associated with event #23. Right: tracing of the CME front associated with event #23. Each red cross corresponds to the average from several points manually selected along the outermost bright front at a given time.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: 3He/4He and Fe/O ratios versus CME speed. Blue squares indicate events associated with jets at the source, while red circles denote events where no jets were observed. Points marked with white crosses (right panel), as well as the the three numerical values shown, have the same meaning as in Figure 5.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Mean heliocentric distance (r) of the CME front versus time (t) since the first front. The red line presents the linear fit; the slope is directly proportional to the CME speed.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Sensitivity of escape suppression to mantle anisotropy. The suppression index Ξ is shown as a function of the anisotropy factor ζ (ratio of shear moduli along distinct crystallographic directions). For ζ = 1 (isotropic mantle), we adopt ϵV ≃ 6 × 10−3, which yields Ξiso ≃ 1 + ϵV/6 ≈ 1.001. Increasing ζ reduces the effective volumetric strain via ϵV,eff = ϵVf(ζ) with 0 < f(ζ) ≤ 1, thereby diminishing the enhancement of escape velocity. In the small-strain limit, Ξ(ζ) ≈ 1 + ϵVf(ζ)/6. Astrophysical implications: Increasing mantle anisotropy (ζ > 1) lowers the effective volumetric strain [ϵV,eff = ϵVf(ζ)], drives Ξ → 1, and thus maps to smaller (≲ppm–tens of parts per million) depressions in near-IR transit depths; isotropic or weakly anisotropic interiors (ζ ≈ 1) maximize the observable ∼10–50 ppm suppression, within JWST multiepoch and ARIEL sensitivity.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Comparison of classical atmospheric escape prescriptions as a function of the planetary mass. The EL regime (﹩{\dot{M}}_{{\rm{EL}}}\propto {v}_{{\rm{esc}}}^{-2}﹩) decreases gradually with increasing M, the Jeans escape (﹩{\dot{M}}_{{\rm{J}}}\propto \exp [-{v}_{{\rm{esc}}}^{2}/{c}_{s}^{2}]﹩) falls off exponentially due to its strong sensitivity to vesc, and hydrodynamic blow-off shows an intermediate ﹩{v}_{{\rm{esc}}}^{-1}﹩ scaling, dominating at low masses and high irradiation. The thermoelastic suppression index Ξ derived in this work modifies all regimes by replacing vesc with ﹩{v}_{{\rm{esc}}}^{* }={\rm{\Xi }}\,{v}_{{\rm{esc}}}﹩, systematically reducing the effective escape rates compared to the classical case.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Time-dependent evolution of the suppression index Ξ(t) over a 5 Gyr cooling history, constrained to the small-strain amplitude discussed in Section 2.8. We adopt ΔT0 − ΔTeq = 66.7 K with ΔTeq = 3000 K, τth = 1.5 Gyr, K = 220 GPa, αT = 3 × 10−5 K−1, and Pavg = 3 × 1010 Pa, yielding ϵV(0) = 0.008 and ϵV(∞) = 0.010. As ΔT(t) decays, ϵV increases and Ξ – 1 rises from ∼1.34 × 103 to ∼1.66 × 103 ppm, remaining within the small-strain limit.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Percent increase in escape velocity, Δvesc/vesc, as a function of the volumetric strain ϵV for a representative super-Earth (M = 5 M⊕, R = 1.8 R⊕). Even small thermoelastic strains produce measurable changes in vesc, though the effect remains subpercent in the EL regime. Interpretation: Subpercent increases in vesc from thermoelastic strains (ϵV ∼ 10−3–10−2) are negligible in the EL regime but amplify exponentially in the Jeans regime, leading to ∼10%–20% reductions in ﹩\dot{M}﹩ for representative parameters.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Mass–radius map colored by the suppression index offset Ξ – 1, expressed in parts per million as 106(Ξ – 1). Each point corresponds to an entry in Table 1, spanning the extended parameter survey (M = 0.5–15 M⊕, R = 1–4 R⊕, K = 80–320 GPa, αT = (1–5) × 10−5 K−1, ΔT = 800–5000 K). Larger values of Ξ – 1 indicate stronger atmospheric escape suppression via a deeper effective escape surface and a higher ﹩{v}_{{\rm{esc}}}^{* }﹩, which reduces the atmospheric scale height.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Thermoelastic control across thermal contrast ΔT and bulk modulus K, colored by volumetric strain ϵV. Points correspond to the extended grid in Table 1, with ΔT = 800–5000 K and K = 80–320 GPa. Higher ΔT and lower K yield larger ϵV, thereby increasing Ξ and suppressing escape via a downward shift of the effective escape surface.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Escape-velocity enhancement versus thermoelastic volumetric strain ϵV. The normalized ratio ﹩{v}_{{\rm{esc}}}^{* }/{v}_{{\rm{esc}}}﹩ follows the analytic scaling ﹩{(1-{\epsilon }_{V}/3)}^{-1/2}﹩. Reference values: ϵV = 0.005 and 0.010 correspond to 0.083% and 0.167% increases in vesc, respectively.
Paper: Thermoelastic Contraction as a Suppressor of Atmospheric Escape in Close-in Exoplanets
Authors: L. Yıldız, D. Kaykı, E. Güdekli
Figure caption: Suppression index Ξ across mantle thermal contrast and bulk modulus. Contours at Ξ – 1 = {5 × 10−4, 10−3, 2 × 10−3} illustrate near-linear scaling with αTΔT and inverse scaling with K. For realistic ϵV ≲ 10−2, departures from unity remain at a per-mille level.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: 2D Cartesian model representing the original LH91 model. Each grid point is associated with a field Bi,j, and with four neighbors in vertical and horizontal directions as shown.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: Diagram of the system where panel (a) is the original lattice before the rewiring processes. In panel (b) a random node is selected, and its neighbors are identified; the selected node is red, yellow nodes are neighbors that cannot be selected because they are at the boundary, and green nodes are neighbors that can be selected. In panel (c), one of the green nodes has been selected to move its connection to another, randomly selected node; the magenta node is the node that has just lost a connection, and the cyan node is the node that has gained that connection. In panel (d), the rewiring has been carried out, conserving the number of neighbors and highlighting the modified nodes, and panel (e) shows the final, rewired state.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: The pdf colored by probability for driving–rewiring values from 10 to 90. Each subplot shows the distribution for a specific driver-rewiring. Using 107 avalanches, N = 64. The color bar represents the percentage of events considered in each bin that was produced by driving: 0% implies events produced entirely by rewiring, while 100% implies events produced entirely by driving.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Two-dimensional surface density distribution in polar coordinates after 1000 orbits of evolution for models without wind. The planet is located at (R, ϕ) = (1.0, 0.0). The rows present different planet masses, from left to right: 0.1MJup, 0.3MJup, 1.0MJup, and 3.0MJup. The columns present different fluids, from top to bottom: gas, gas tracer (St = 1 × 10−6), 1, 10, 100 μm, and 1 mm. The dust surface density is scaled up from the true density according to ϵi.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: Spatial distribution of one avalanche: the top row shows the original model without rewiring, and the bottom row corresponds to an 80–20 rewiring configuration. Panels (a) and (e) depict the beginning of the avalanche; panels (b) and (f) show the system at time t3; panels (c) and (g) show the state at the peak of the avalanche; and panels (d) and (h) show the full extent of the avalanche-affected area, with impact frequency visualized on a color scale: white (0 times affected), black (1 time), and a rainbow gradient for larger values.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: (a) Relative error for the best fit of the decay exponent for a power-law model (red) or exponential model (blue), for the dissipated energy distribution, as a function of the probability of driving p(d) rather than rewiring. (b) Decay exponents obtained for each model: power-law (αE, red) and exponential (βE, blue) model, as a function of p(d).
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: (a) LH total energy at time t. (b) Total energy for the whole system at time t, where the colors represent the different relations in percentage between driving–rewiring as a mechanism for the avalanche, i.e., light green: 99.9–0.1, purple: 99–1, black: 90–10, red: 80–20, orange: 70–30, yellow: 60–40, blue: 50–50, cyan: 40–60, magenta: 30–70, green: 20–80, brown: 10–90. The system uses 107 iterations with N = 64, Zc = 1.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Example of the restart condition where dust is inserted in the outer disk only. These images show the two-dimensional surface density distribution in polar coordinates, (r, ϕ). Both gas and dust surface density are normalized by the initial gas surface density, Σg,0, for visualization purpose. The dust surface density is constructed such that all of the dust material is in the outer disk (r ≥ 1.5rp), and in the inner disk it is effectively equal to zero. The dust surface density is scaled up from the true density according to ϵi, so that the dust surface density in the outer disk is exactly equal to the gas surface density.
Paper: Lu and Hamilton Model for Solar Flares over a Rewiring Complex Network
Authors: Alejandro Zamorano, Laura Morales, Denisse Pastén, Víctor Muñoz
Figure caption: Dissipated energy from an 80 to 20 system. The red region in the lower panel shows a particular avalanche with total energy dissipated E, peak energy P, and duration T.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Two-dimensional surface density distribution in polar coordinates after 1000 orbits of evolution for a mp = 1MJup model with varying wind strength, from left to right: no wind, ﹩{\dot{M}}_{w}=1{0}^{-9}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩, ﹩{\dot{M}}_{w}=1{0}^{-8}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩, and ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩. The planet is located at (R, ϕ) = (1.0, 0.0). The columns present different fluids in the disk, increasing from top to bottom: gas, gas tracer (St = 1 × 10−6), 1, 10, 100 μm, and 1 mm. The dust surface density is scaled up from the true density according to ϵi. An animated version of this figure is available here: https://zenodo.org/records/17228085.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Azimuthally averaged surface density profiles after 1000 orbits of evolution for models without wind, adopting various planet masses of 0.1MJup (top left), 0.3MJup (top right), 1.0MJup (bottom left), and 3.0MJup (bottom right). The planet is located at R = 1.0. Each gas and dust fluid is plotted corresponding to the colors in the figure legend. The dotted line in each panel is the initial gas surface density according to Equation (16). The gas tracer and small dust grains were able to flow inward more efficiently than the larger dust grains, while the large dust grains became trapped in the pressure bump in the outer disk. The dust surface density is scaled up from the true density based on their abundance (Σd,i/ϵi) for visualization purposes.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Azimuthally averaged surface density profiles after 1000 orbits of evolution for models with wind, adopting various mass-loss rates: no wind (top left), ﹩{\dot{M}}_{w}=1{0}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (top right), ﹩{\dot{M}}_{w}=1{0}^{-8}\,{M}_{\odot \,}{\mathrm{yr}}^{-1}﹩ (bottom left), and ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (bottom right). The planet is located at R = 1.0. Each gas and dust fluid is plotted corresponding to the colors in the figure legend. The dust surface density is scaled up from the true density based on their abundance (Σd,i/ϵi) for visualization purposes. The dotted line in each panel is the initial gas surface density according to Equation (16).
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Left panels: visualization of the two-dimensional velocity (vr, vϕ) distribution for the case of a Jupiter-mass planet. The top panel is the gas tracer in the case of no wind, the middle panel is the gas tracer in the case of wind with a mass-loss rate ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩, and the bottom panel is the 100 μm dust in the case of wind with a mass-loss rate ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩. The white streamlines indicate the direction (but not magnitude) of the velocity vector. The background color contour shows the corresponding surface density. Right panels: mass flux at each grid cell evaluated at R = 0.9 (dashed green line on the left side). Gas and dust flows in the corotating region near the planet become asymmetric when wind is turned on.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Left panel: mass within one-third of the planet’s Hill radius for each of the models, calculated after 1000 orbits. The ×'s are gas mass, and the solid points are dust mass. Right panel: luminosity of the CPD region (corresponding to ﹩1/3{R}_{\mathrm{Hill}}﹩) evaluated at λ = 1.3 mm and assuming T = 20 K, κ = 2.4 cm2 g−1, and d = 150 pc. For reference, PDS 70c (rescaled to 150 pc) is shown as the dotted green line (A. Isella et al. 2019) and the DSHARP 5σ detection limit (S. M. Andrews et al. 2018) is shown as the shaded green region.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Absolute value of the total mass flux at R = 0.9rp over time for the case of Mp = MJup. The different colors show different wind strengths corresponding to the figure legend. From top to bottom, the panels show the results for gas, 1 μm dust, and 1 mm dust.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Analytical prediction for the mass-loss parameter bcrit that would cause a dust fluid to flow inward, assuming Mp = 1Mjup. For reference, we plot the bcrit for dust fluids with a = 1 mm (blue), 100 μm (light blue), 10 μm (red), and 1 μm (pink). The dotted horizontal black lines indicate the three ﹩{\dot{M}}_{w}﹩ used in this study.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Evolution of the dust-to-gas ratio throughout the disk for the case of Mp = MJup. The dust-to-gas ratio is ϵ = Σd/Σg, where Σd is the total dust surface density and Σg is the gas surface density. The four panels represent models with different wind mass-loss rates: no wind (top left), ﹩{\dot{M}}_{w}=1{0}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (top right), ﹩{\dot{M}}_{w}=1{0}^{-8}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (bottom left), and ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ (bottom right). The final dust-to-gas ratio from the no-wind case is plotted in red in each panel for visual comparison.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Depletion factor ζ(a) for every model in this study evaluated after 1000 orbits of evolution. Each panel shows the result for the different planet masses used in this study. When there is wind, large dust grains are less depleted compared to the reference model than when there is no wind.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Evolution of the azimuthally averaged dust-to-gas ratio throughout the disk for all the planet masses in this study. The dust-to-gas ratio is ϵ = Σd/Σg, where Σd is the total dust surface density and Σg is the gas surface density. From top to bottom, the panels show the results for Mp = 0.1MJup, 0.3MJup, 1.0MJup, and 3.0MJup, respectively. From right to left, the panels show the results for different wind mass-loss rates: no wind, ﹩{\dot{M}}_{w}=1{0}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, ﹩{\dot{M}}_{w}=1{0}^{-8}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, and ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. The final dust-to-gas ratio from the no-wind case is plotted in red in each panel for visual comparison.
Paper: Enhanced Pebble Drift across Planet-opened Gaps in Windy Protoplanetary Disks
Authors: Lorraine Nicholson, Jaehan Bae
Figure caption: Surface density radial profile after 1000 orbits of evolution for every model in this study. From top to bottom, the panels show the results for Mp = 0.1MJup, 0.3MJup, 1.0MJup, and 3.0MJup, respectively. From right to left, the panels show the results for different wind mass-loss rates: no wind, ﹩{\dot{M}}_{w}=1{0}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, ﹩{\dot{M}}_{w}=1{0}^{-8}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, and ﹩{\dot{M}}_{w}=1{0}^{-7}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. The dust surface density is scaled up from the true density according to ϵi.