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: PS1 RGB false-color g/i/z image centered on AT2021ehb. North is up and east to the left. A 10″ scale bar is included.
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 profile of Σd and dust size a (top panel), and radial velocities ﹩\left\langle {v}_{r}\right\rangle ﹩, ﹩-{{\rm{\Sigma }}}_{{\rm{d}}}^{-1}D\partial {{\rm{\Sigma }}}_{{\rm{d}}}/\partial r﹩, and ﹩{v}_{r}=\left\langle {v}_{r}\right\rangle -{{\rm{\Sigma }}}_{{\rm{d}}}^{-1}D\partial {{\rm{\Sigma }}}_{{\rm{d}}}/\partial r﹩ (bottom panel) around the most collapsed ring at the final time step. Red filled circles show the position of the cell boundaries. One can see that the ring structure is well resolved even though the radial width is less than 0.1 au. We find the radial gradient in v  r  around the left-side tail of the Σd profile (32.3 au ≲ r ≲ 32.35 au), while v  r  is almost uniform within the ring. Thus, the ring will sweep inner dust grains up, and the surface density increases through further evolution.
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: Results of the local simulation with λ = 1 au, Σd ,0/Σg ,0 = 10−3, and α = 10−4. The green solid line shows the amplitude of the dust surface density perturbation as a function of tΩ. The gray dotted line shows the time evolution of the background stopping time τ s,0. The initial dust surface density perturbation is damped by the diffusion at a rate of Dk 2 (black dotted line). The perturbation exponentially grows after the initial damping. The green dashed lines show the growth rates derived in the previous linear analyses (Equation (18)). We use physical values at times marked by the orange filled circles to derive the growth rate. The linear analyses are in good agreement with the simulation at each point.
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 (top panels) and dimensionless stopping time (bottom panels) obtained from the q2T20a1 run. The left two panels and the right two panels show evolution with and without initial perturbations, respectively. Coagulation instability locally increases dust-to-gas ratio up to ∼10−1. We stop the simulation at t = 9.0 × 104 yr since the dimensionless stopping time τ s becomes larger than unity around the most collapsed dust ring.
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: Schematic summary of the initial setups of local simulations. We input sinusoidal perturbations only on dust surface density (black line), and thus δ τ s = 0 at t = 0 (gray line). Since our method utilizes the Lagrangian scheme, we set up δΣd displacing the cell (δ ξ) as depicted on the bottom of this figure: open and filled circles represent cell locations before and after the displacement, respectively. Note that the number of cells used in the local simulations is larger than the number of filled circles in this figure.
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: (a) The stack plot of B  z  along the magnetopause (denoted by the dashed line in Figure 1(b)) in the northern hemisphere at different times, and the coalescence of FTEs is denoted by the black dotted lines. (b) The evolution of B  z  at x = −1.55R  M  (green dashed line in (a)). The results are obtained in Case 2.
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: Growth and propagation of δΣd/Σd ,0 (left panel) and δτ s,0/τ s,0 (right panel) obtained from the local simulation with λ = 1 au and α = 10−4. Note that the horizontal axis is the radial position X in the background-dust-rest frame (Equation (22)). The phase shift between δΣd and δτ s and the radial propagation of the perturbations are consistent with the previous linear analyses (Tominaga et al. 2021).
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: Results of the local simulation with α = 10−4 for λ = 0.25,  1, and 4 au. The blue, green, and yellow solid lines show the evolution of δΣd/Σd ,0 for each wavelength. The gray dotted line shows the time evolution of the background stopping time τ s,0. The blue, green, and yellow dashed lines show the growth rates derived in the previous linear analyses (Equation (18)). We use physical values at times marked by the orange filled circles to derive the growth rate. The linear analyses have a good agreement with each simulation.
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: The structure of FTE obtained from the simulation at t = 122.7 s. The red lines are the magnetic field lines associated with the FTE. The ion number density N  i  in the noon–midnight meridian and equatorial planes is also plotted. The simulation parameters are the same as those in Cases 1 and 2, except that the IMF is ﹩{{\bf{B}}}_{{\bf{0}}}=\left(0,14.1,-14.1\right)\ {\rm{nT}}﹩.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Schematic diagram of the trace magnetic PSD and frequency break at 0.82 au. In the inertial range, the trace PSD is dominated by the perpendicular turbulence, which scales as f −5/3. The black solid circle is where f b is at r = 0.82 au. The black dashed line shows the scaling of f b as r. For reference, we also draw the PSD of the parallel turbulence, which scales as f −2. The gray dotted line is the extension of the 1/f power law to higher frequencies to contrast the change in the inertial range.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Geometry of the CME (blue lines) and the shock (red lines) at 15:18 UT on 2020 November 29. The blue and red arrows indicate the propagation directions of the CME and shock, respectively. The directions of the Earth, STEREO A, PSP, and Solar Orbiter are marked by the black arrows. The center of the shock ellipsoid (O) and its distances from the center of the Sun (d), from the nose of the shock (c) and from the flank perpendicular to the propagation direction (b) are also indicated.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Magnetic field configuration and EUV observations of the source region. (a) PFSS modeled coronal magnetic fields surrounding the source region mapped onto the EUVI 195 Å image at 13:14 UT on 2020 November 29. The blue lines represent the closed field lines, and the green lines are the open magnetic field lines. The white arrow marks the source region. (b)–(c) Running-difference images of STEREO A/EUVI at 195 Å showing the low coronal signatures associated with the CME. (d) Hot channel at 131 Å from SDO/AIA. The white line indicates a slice along the radial direction to create a distance–time diagram for the hot channel. (e)–(f) Running-difference images of SDO/AIA at 193 Å showing the plasma loop and the EUV wave from the viewpoint of the Earth. The red arrow marks the eruption caused by the EUV wave.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Kinematics of the CME and shock derived from different methods. Top: the distances of the CME derived from EUV observations, the GCS model, and the HM approximation, and the height of the shock nose derived from the ellipsoid model. Middle: speeds of the CME and shock nose derived from the numerical differentiation of the distances in the top panel. GOES 1–8 Å X-ray flux is overlapped in the panel scaled in arbitrary units. The horizontal dashed line represents the shock speed of ∼700 km s−1 at STEREO A. Bottom: expansion speeds of the shock along the radial and lateral directions and translation speed of the shock center. The distances and speeds of the CME front are binned to reduce the uncertainties, so the CME parameters are average values and standard deviations within the bins. Following Kwon et al. (2014), the uncertainty of the ellipsoid model parameters is estimated to be 8%.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Positions of the spacecraft and planets in the ecliptic plane on 2020 November 29. The “A”, “B,” and “SO” represent the satellites of STEREO A, STEREO B, and Solar Orbiter respectively. The black circle and red ellipse mark the orbits of the Earth and PSP respectively. The dotted curves show Parker spiral magnetic fields created with a solar wind speed of 450 km s−1. The red arrow indicates the direction of the source region in the ecliptic plane.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Left: distance–time map of the hot channel by stacking SDO/AIA 131 Å running-difference images along the white line in the panel (d) of Figure 2. The red curve indicates the track of the hot channel. Right: time-elongation map constructed from running-difference images of C2 and C3 from SOHO/LASCO along the ecliptic plane. The red curve marks the track of the CME leading edge, along which the elongation angles are extracted.
Paper: Multispacecraft Remote Sensing and In Situ Observations of the 2020 November 29 Coronal Mass Ejection and Associated Shock: From Solar Source to Heliospheric Impacts
Authors: Chong Chen, Ying D. Liu, Bei Zhu
Figure caption: Running-difference images from GOES 16, STEREO A, and SOHO with corresponding modeling of the CME and shock. Panels (a)–(c) show the same shock modeling result for 13:15 UT. Panels (d)–(i) display the running-difference coronagraph images and corresponding GCS modeling (green) and ellipsoid shock modeling (red).
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The C II]λ2326/C II λ1335 line intensity ratio vs. T  U  for N  e  = 1000 cm−3. The curves indicate the theoretical predictions for various κ values, among which the solid line represents the κ = ∞ case (i.e., the Maxwell–Boltzmann distribution). The circles with error bars are the observed values in PNs, where the open and filled circles represent T  M (BJ) and the derived T  U  (see text), respectively. The filled triangles denote the observed values in quasars extracted from Vernet et al. (2001), where we have assumed T  U  ≡ 1.5 × 104 K.
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The relations between r(C II) and T  M (BJ) predicted by the two-EED model, which is composed of a regular MB-EED nebular component and a κ-EED component with a κ index of 3, 5, 10, and 20, and various filling factors (ω). The squares with error bars represent the observed values.
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The κ index vs. T  M (N II) − T  M (BJ) (upper panel) and ADF(O2+) (lower panel). The solid lines represent linear fittings. The correlation coefficients are shown in the upper right corners.
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The theoretical C II line ratio as a function of T  U  and N  e  for different κ values.
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: Configuration of the energy levels and transitions of the C II ion.
Paper: The Ultraviolet C II Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae
Authors: Zheng-Wei Yao, Yong Zhang
Figure caption: The IUE spectra of the PNs, which show the C II]λ2326 (left panel) and C II λ1335 (right panel) features. The smooth curves represent the Gaussian fits.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Temperature distributions as a function of time for runs rhdg2_c3 (left), rhdg3_c3 (middle), and rhdg4_c3 (right). The boundaries of the damping zones are indicated with dotted lines in the t = 0 snapshots. Videos made with snapshots of these runs can be found in https://youtu.be/RT8IFe8W13g.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Same as Figure 10, but this time showing a time-dependent comparison of the current temperature T with the initial temperature T 0.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Temperature distributions after 35 iterations for f dg = 10−2, t iter = 1 yr, and ﹩\hat{c}={10}^{-2}﹩ (top), ﹩\hat{c}={10}^{-3}﹩ (middle), and ﹩\hat{c}={10}^{-4}﹩ (bottom). The horizontal white dashed lines indicate the θ values where the temperature profiles in Figure 8 were taken.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Same as Figure 10, but showing the expected linear growth rate of the fastest-growing VSI mode for instant thermal relaxation normalized by the local Ω.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Midplane temperature as a function of radius measured at different times for f dg = 10−2 (top) and 10−3 (bottom), taking ﹩\hat{c}/c\,=\,{10}^{-3}﹩ (left) and 10−4 (right). The power law r −0.45 used at the first iteration for the construction of initial conditions is shown for comparison (dashed lines).
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Same snapshots as in Figure 11, but showing the time evolution of ﹩{\mathrm{log}}_{10}{\epsilon }_{k}﹩, where ﹩{\epsilon }_{k}=\tfrac{1}{2}\rho ({v}_{r}^{2}+{v}_{\theta }^{2})﹩.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Radial temperature profiles at θ − π/2 = 0 and 0.07 in run dg2t1_c2 after 35 iterations.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Same as Figure 10, but showing the evolution of ﹩{\mathrm{log}}_{10}f﹩ (color scale) and the direction of  F   r  (arrows).
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Temperature distributions at different times for runs rhdg2_c3 (left) and rhdg2_c4 (right).
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: The distributions of parallax (panel (a)), proper motions (panel (b)), as well as the G − RP vs. G CMD (panel (c)) for the known members (blue circles and blue histogram), the new candidates (orange diamonds and orange histogram), the new members (red squares and red filled histogram), and the Gaia sample described in Section 2.1 (gray pluses and gray histogram). The vertical dashed lines in panel (a) mark the 3σ interval. The red ellipse in panel (b) is the 3σ confidence ellipse (see the text for detail). The blue vertical and horizontal dashed lines indicate the weighted means of the proper motions along R.A. and decl., respectively. The red solid line in panel (c) is the 10 Myr isochrone from the PARSEC stellar model (Bressan et al. 2012), with solar metallicity and scaled to a distance of 300 pc. The red dashed line corresponds to the color (G − RP = 1.45 mag) of the lowest mass star in the PARSEC stellar model. The black arrow is the extinction vector of A  V  = 3 mag (the typical extinction value of the Perseus sources, see Figure 7) corresponding to the extinction law from Wang & Chen (2019).
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Spatial distribution of previously known members (blue circles), new members (red squares), and candidates (orange diamonds) in the Perseus molecular cloud overlaid on the FCRAO 12CO J = 1 → 0 integrated intensity map. The two rectangles mark the sky coverage of the two clusters as defined in Rebull et al. (2007), note that the cluster regions adopted here are slightly different from that in Luhman et al. (2016). The scale bar on the left bottom shows a size of 2 pc at a distance of 300 pc. The large solid circle and the dashed ellipse mark the stellar aggregates discussed in Section 5.2.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Example spectra of a representative sample of the newly confirmed members. The prominent emission lines and the Li I λ 6707 Å absorption lines are marked in each panel, if present. The Gaia EDR3 source designations and the corresponding spectral types are labeled as well.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Comparison between spectral types from this work and that from previous works for known members that have LAMOST observations. The solid line indicates the line of equality, and the dashed lines mark differences between three subtypes.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Distributions of spectral types for previously known (blue bars) and newly confirmed (red bars) members.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Phase diagrams showing the distribution of gas mass (top) and its initial radius (bottom) on the plane of radial velocity vs. radius from the 3DCONV0.5 (left) and 3DMESA0.5 (right) runs. The diagrams are taken at t = t dyn and 3 t dyn. The mass-weighted radial velocity (orange lines) and local escape velocity (black dashed lines) are shown for reference. The nonuniform shock propagation in the convective envelope of 3DCONV0.5 causes a much wider spread of velocity and allows gas from the deep interior to be accelerated above the escape velocity (dark blue band in the bottom left panel), leading to ≈3× more ejected mass.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Density profiles of the stellar envelopes and the ejecta from the 3DCONV0.5 and 3DMESA0.5 models (solid lines). The profiles are taken at the end of their mass loss episodes when the mass loss rates fall to zero, at 2.8 and 2.3 yr after energy deposition, respectively (see Figure 10). Dashed lines denote the steady wind solution assuming a constant wind velocity of v w = 65 km s−1. The black vertical line marks the outer boundary of the FLASH simulations. The colored vertical lines denote the half-mass radii of the escaped mass measured from the outer boundary. Density profiles immediately before energy deposition are plotted as dotted–dashed lines for reference.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Evolution of mass loss rate of models with different initial structures and amounts of injected energy. The fiducial model’s mass loss rate is a factor of a few higher than that of 3DMESA0.5 throughout their entire mass loss episodes.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Density profiles at two characteristic times t = t dyn and 10 t dyn from the 3DCONV0.5, 3DMESA0.5, and 1DMESA0.5 runs. Density inversion following energy deposition only manifests in the initially static models without convection (1D/3DMESA0.5). It persists in 1D (green dotted–dashed line) but is later smoothed out by RTIs in 3D (orange dotted–dashed line). Note the logarithmic scale in radius.
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Mollweide projection of the escaped mass from 3DCONV0.5 (left) and 3DMESA0.5 (right), expressed in M ⊙ per unit solid angle. These projections are taken at the end of the mass loss episode in each model, at the same moments as in Figure 13. Nonuniform shock propagation in the convective model leads to 10× variations in the column density along different lines of sight. In the initially static 3DMESA0.5 model, the variations in column density are within ≲1%.