adsabs/AstroCLIMB huggingface dataset:
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the VSO coordinate system as observed during the Venusian bow shock crossing on 2011 July 26. The transition is highlighted by the gray shaded area.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the VSO coordinate system as observed during the Venusian bow shock crossing on 2011 December 15.
Paper: Enthalpy of the N+ + H2 → NH+ + H Reaction—Experimental Study of the Reverse Process
Authors: Štěpán Roučka, Serhiy Rednyk, Thuy Dung Tran, Artem Kovalenko, Dmytro Mulin, Sunil S. Kumar, Petr Dohnal, Radek Plašil, Juraj Glosík
Figure caption: Upper panel: the measured rate coefficients of the reverse reaction as a function of translational, collisional, and NH+ internal temperatures. The inner error bars indicate the statistical errors, whereas the outer error bars also include the systematic uncertainty due to n H calibration. Middle panel: the rate coefficient of the forward reaction extracted from the data of Zymak et al. (2013). The systematic error of the data is indicated by the filled band. Lower panel: values of ΔE 0 obtained from the detailed balance principle Equation (5). The overall (systematic + statistical) uncertainties obtained using interval arithmetic from the overall uncertainties of the input data are indicated by the error bars.
Paper: Enthalpy of the N+ + H2 → NH+ + H Reaction—Experimental Study of the Reverse Process
Authors: Štěpán Roučka, Serhiy Rednyk, Thuy Dung Tran, Artem Kovalenko, Dmytro Mulin, Sunil S. Kumar, Petr Dohnal, Radek Plašil, Juraj Glosík
Figure caption: Measured numbers of trapped ions, N  i , as a function of trapping time t, showing the loss of the 14NH+/15N+ ions (squares) and formation of the N+ ions (circles) in the trap. The curves represent least-squares fits of the data with a kinetic model. The data were measured with the H beam on (closed symbols and solid lines) and H beam off (open symbols and dashed lines). The fitted numbers of 14NH+ and 15N+ in the measurement with the H beam on are indicated by the dotted lines. The measurement was performed at ion and atom temperatures of ﹩{T}_{{\mathrm{NH}}^{+}}=26\ {\rm{K}}﹩, T H = 75 K, with an H number density of n H = 3.2 × 107 cm−3.
Paper: Enthalpy of the N+ + H2 → NH+ + H Reaction—Experimental Study of the Reverse Process
Authors: Štěpán Roučka, Serhiy Rednyk, Thuy Dung Tran, Artem Kovalenko, Dmytro Mulin, Sunil S. Kumar, Petr Dohnal, Radek Plašil, Juraj Glosík
Figure caption: Comparison of the reaction enthalpy determined in the present study with the upper estimates obtained in previous studies of the forward reaction: Pla22 (Plašil et al. 2022), Ger93 (Gerlich 1993), Mar88 (Marquette et al. 1988), Erv87 (Ervin & Armentrout 1987), Mar85 (Marquette et al. 1985), and Ada85 (Adams & Smith 1985). The circles indicate activation energies and the diamonds indicate evaluated reaction enthalpies with the assumption of no barrier. The values labeled as “global fit” were evaluated by combining the experimental data for multiple isotopic variants of the forward reaction.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Morlet wavelet spectrum of the frequency shifts for all modes (top) and the global power spectra (bottom). The two vertical brown lines in the top panel delineate the boundaries between cycles 23 and 24 then cycles 24 and 25, while the dashed lines in both panels represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Morlet wavelet spectrum of the frequency shifts (left) and the global power spectrum (right) for modes with lower-turning points in the convection zone (top), radiative zone (middle), and the core (bottom). The two vertical brown lines in the left panels delineate the boundaries between cycles 23 and 24 then cycles 24 and 25, while the dashed lines in all panels represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: The same as Figure 5, but for modes with upper-turning points in the high-ν (top), mid-ν (middle), and low-ν (bottom) bands. The dashed lines represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Morlet wavelet spectra (left) and the global power spectra (right) for all modes with a lower-turning point in the upper 10% layer below the surface. The two vertical brown lines in the left panels delineate the boundaries between cycles 23 and 24 then cycles 24 and 25, while the dashed lines in both panels represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Temporal evolution of: (a) the mean frequency shifts (green symbols connected with the solid line) and the dominant 11 yr signal of the solar cycle as calculated by applying a boxcar filter of a width of 2 yr (solid red line); and (b) the residual shifts after removing the 11 yr signal. The errors in frequency shifts are of the order of 10−6 μHz.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Morlet wavelet spectra (left) and the global power spectra (right) for all modes with a lower-turning point in the upper 10% layer below the surface in cycle 23 (top) and cycle 24 (bottom). The dashed lines represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Morlet wavelet spectra (left) and the global power spectra (right) to study QBO periodicities for all modes in cycle 23 (top) and cycle 24 (bottom). The dashed lines represent the 95% confidence level.
Paper: Helioseismic Investigation of Quasi-biennial Oscillation Source Regions
Authors: Kiran Jain, Partha Chowdhury, Sushanta C. Tripathy
Figure caption: Duty cycles of 36 day p-mode frequency data sets.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: Evolutionary tracks of seven HeWD+MS merger models that pass through the parameter space where BLAPs are found. The tracks are distinguished by color and identified by mass in the key. Top panel: evolution in the ﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩–﹩\mathrm{log}L﹩ (H-R) diagram. Bottom panel: evolution in the ﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩–﹩\mathrm{log}g﹩ diagram. Filled dots with errors represent observed BLAPs 1, 9, 11, 14, and 15–23 from Table 1. The triangle and circle show the stars with previously determined luminosity, OGLE-BLAP-009 (Meng et al. 2020) and TMTS-BLAP-1 (Lin et al. 2022), respectively.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: A part of the post-merger evolution of a 0.250 + 0.650 M ⊙ HeWD+MS system during three helium shell flashes. Left panel: the dashed line shows evolution in the ﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩–﹩\mathrm{log}g﹩ diagram. The solid line indicates a selected loop of evolution. Numbers indicate stages identified in the text. Right panel: the evolution of radius (red) and helium shell luminosity (black) for the same model.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: Profile of opacity, the mass fraction of Fe and Ni, and work function dW/dx of stellar interior temperature. The logarithm of the opacity is shown by the solid black line, the logarithm of the mass fraction of Fe and Ni is indicated by the dotted line, while the value of dW/dx is indicated by the solid pink line. The blue zone indicates the approximate temperatures of the partial ionization opacity peaks of iron group elements.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: The rate of period change ﹩r\equiv \dot{P}/P﹩ vs. pulsation period P for the seven possible BLAP models. Tracks are identified by color as in Figure 3. The solid line shows the same loop through a helium shell flash for the 0.250 + 0.650 M ⊙ post-merger model shown in Figure 2. Filled dots represent BLAPs 1–14 and 23 in Table 1.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: The pulsation stability of the seven HeWD+MS merger models on the ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩–﹩\mathrm{log}g﹩ plane. The tracks are indicated by gray dotted lines, while the unstable modes are shown by colored circles and identified in the key. The BLAPs shown in Figure 3 are also indicated.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: Evolution of surface helium abundance ﹩\mathrm{log}\,N(\mathrm{He})/N({\rm{H}})﹩ during helium shell flashes in seven possible BLAP models as a function of ﹩\mathrm{log}g﹩. Tracks are identified by color and key as in Figure 3. Filled dots with errors represent observed BLAPs 1, 9, 11, 14, and 15–23 in Table 1.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: Evolution of seven possible BLAP models in the period–luminosity (top), period–temperature (middle), and period–gravity (bottom) planes. Tracks are identified by color as in Figure 3. Filled dots with errors represent observed BLAPs from Table 1.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The global mean temperature (a) is plotted against pressure for the P19 PI (orange), P19 noTL (dark red), P19 10% PAL (brown), P19 1% PAL (yellow), and P19 0.1% PAL (red) simulations, and the W21 PI (light blue), W21 noTL (black), W21 10% PAL (blue), W21 1% PAL (lilac), and W21 0.1% PAL (gray) simulations. The globally averaged mixing ratios for O (b), O2 (c), O3 (d), H2O (e), CH4 (f), N2O (g), and CO2 (h), are also shown.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The O3 column in DU across the simulation’s latitudinal and longitudinal grid is plotted for all the simulations used in this work (the P19 scenarios are in the left column and the W21 scenarios are in the right column). 1 DU is equal to 2.6867 × 1020 molecules m−2. In all simulations, O3 column maxima occur at high latitudes. The substellar point for the tidally locked cases is at 180° longitude and 0° latitude on Earth’s coordinate grid (in the center of each Robinson projection). Note that the color bars are extended for some simulations in order to show the O3 column structure in each scenario. Each panel has a different color bar range.
Paper: Dwarf Galaxies Show Little ISM Evolution from z ∼ 1 to z ∼ 0: A Spectroscopic Study of Metallicity, Star Formation, and Electron Density
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Teja Teppala, Fuyan Bian, Timothy Carleton, Sandra Faber, Puragra Guhathakurta, David C. Koo
Figure caption: The [O II]λ λ 3727,3729 doublet for three different HALO7D dwarf galaxies showcasing a range of line ratios and electron densities. The continuum-subtracted spectrum normalized to the peak line flux is given in blue, with the in-atmosphere rest wavelengths of [O II]λ λ 3727,3729 given by the dashed vertical lines. The inset text gives the HALO7D ID, emission-line-derived redshift, stellar mass, [O II]λ λ 3727,3729 doublet ratio R, and electron density n  e  in cm−3 for each galaxy. The density for GDS_17954 is reported as an upper limit since R becomes insensitive to the electron density for n  e  ≲ 100 cm−3.
Paper: Dwarf Galaxies Show Little ISM Evolution from z ∼ 1 to z ∼ 0: A Spectroscopic Study of Metallicity, Star Formation, and Electron Density
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Teja Teppala, Fuyan Bian, Timothy Carleton, Sandra Faber, Puragra Guhathakurta, David C. Koo
Figure caption: The electron density as a function of redshift for HALO7D dwarf galaxies. Each point shows median n  e  in a redshift bin of 162 galaxies, with error bars giving the interquartile range of ﹩\mathrm{log}({n}_{e})﹩ for the bin. The shading of the points denotes the median sSFR for each bin. The solid horizontal line indicates the low-density limit from Sanders et al. (2016) for measuring n  e  from the [O II]λ λ 3727,3729 doublet ratio, and the dashed horizontal line gives the value at which the density becomes insensitive to the flux ratio. This shows that the dwarf galaxies at z < 1 have low electron densities consistent with those typical of z ∼ 0 galaxies, while at z > 1, the dwarf galaxy sample has higher densities as well as elevated sSFR, though the scatter in density is high throughout.
Paper: Dwarf Galaxies Show Little ISM Evolution from z ∼ 1 to z ∼ 0: A Spectroscopic Study of Metallicity, Star Formation, and Electron Density
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Teja Teppala, Fuyan Bian, Timothy Carleton, Sandra Faber, Puragra Guhathakurta, David C. Koo
Figure caption: The RO2–n  e  distribution for HALO7D [O II]λ λ 3727,3729 emitters. Red lines give the median R = 1.37 and n  e  = 55 cm−3 values for the sample. However, the histograms of the R and n  e  distributions show that this is far from a uniform distribution: nearly half the sample is clustered at very low n  e . This is largely due to the insensitivity of the R–n  e  calibration for densities below ∼50 cm−3, where the changes in R are much smaller than the measurement error.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The P19 (left column) and W21 (right column) irradiation scenarios are compared to each other for the PI (top row) and 0.1% PAL (bottom row) cases. The zonal mean (averaged over longitude) of the production of O from O2 photolysis is displayed, with latitude in degrees on the horizontal axis and pressure in hectopascals on the vertical axis. O2 photolysis takes place at wavelengths less than 242 nm. The white regions show where the production has dropped below 108 molecules m−3 s−1.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The P19 (left column) and W21 (right column) irradiation scenarios are compared to each other for the PI (top row) and 0.1% PAL (bottom row) cases. The zonal mean (average over longitude) of the O3 number density is shown, with latitude in degrees on the horizontal axis and pressure in hectopascals on the vertical axis. The white regions show where the number density has dropped below 1016 molecules m−3.
Paper: Degenerate Interpretations of O3 Spectral Features in Exoplanet Atmosphere Observations Due to Stellar UV Uncertainties: A 3D Case Study with TRAPPIST-1 e
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, A. Youngblood
Figure caption: The top of atmosphere irradiance per unit wavelength as a function of wavelength for the TRAPPIST-1 semiempirical stellar spectra from P19 (orange) and W21 (light blue), each of which are scaled to the total integrated irradiance received by TRAPPIST-1 e (900 W m−2). These spectra were rebinned in order to match the wavelength grid used in the WACCM6 simulations. The gray shaded region indicates UV wavelengths (100–400 nm).
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Dust size distributions at 50 au (solid lines) and 100 au (dashed lines) of our DustPy models (left panel). In the right panel, we show the respective vertical cooling time profiles, assuming vertical settling–mixing equilibrium for the given α and the critical VSI cooling time. Models with larger particles also exhibit longer cooling times owing to collisional decoupling between dust and gas. We also show the height-dependent cooling time for local VSI modes as purple lines (see Equation (3)).
Paper: All We Are Is Dust in the WIM: Constraints on Dust Properties in the Milky Way’s Warm Ionized Medium
Authors: J. L. West, B. M. Gaensler, M.-A. Miville-Deschênes, N. Mahajan, J. Dechant, F. Boulanger, P. G. Martin, I. A. Zelko
Figure caption: Corner plots showing the posterior distribution results of the MCMC plane fitting of the ϵ  a (ν), ϵ  a (ν), and ϵ  c (ν) parameters at 353 GHz (top left), 545 GHz (top right), 857 GHz (bottom left), and 3000 GHz (bottom right) for the case where ﹩{\chi }_{{\rm{H}}}^{{\mathrm{WNM}}_{{\rm{H}}\,{\rm\small{I}}}}=0.0﹩ and ﹩{\chi }_{{\rm{H}}}^{\mathrm{WIM}}=1.0﹩. These plots are the results of fitting the 14 lines of sight together, where each line of sight is given equal weight. The values in Tables 2 and 3 are derived from a distribution of such fits performed using bootstrapping, where in each bootstrap iteration the weights given to each line of sight are randomly varied.
Paper: All We Are Is Dust in the WIM: Constraints on Dust Properties in the Milky Way’s Warm Ionized Medium
Authors: J. L. West, B. M. Gaensler, M.-A. Miville-Deschênes, N. Mahajan, J. Dechant, F. Boulanger, P. G. Martin, I. A. Zelko
Figure caption: Results of the MCMC blackbody fitting. Here, we fix ﹩T\,(\mathrm{WIM})=T\,({\mathrm{WNM}}_{{\rm{H}}\,{\rm\small{I}}})﹩ and ﹩\beta \,(\mathrm{WIM})=\beta \,({\mathrm{WNM}}_{{\rm{H}}\,{\rm\small{I}}})﹩, in order to fit for ﹩{\tau }_{353}/{N}_{{\rm{H}}}\,(\mathrm{WIM})﹩, and ﹩{\chi }_{{\rm{H}}}^{{\mathrm{WNM}}_{{\rm{H}}\,{\rm\small{I}}}}=0.0﹩ and ﹩{\chi }_{{\rm{H}}}^{\mathrm{WIM}}=1.0﹩. The lines show the mean of the posterior distribution, and the shaded regions show the 1σ confidence regions.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Workflow from our dust coagulation models with DustPy to the hydrodynamic simulations with PLUTO to the radiative transfer modeling with RADMC-3D. Used methods and tools are shown as dark-blue boxes. Input parameters and intermediate results are shown in light blue. The results of our work are schematically displayed as orange boxes. The details of our methodology are laid out in Section 3 (DustPy and cooling times), Section 4 (PLUTO simulations and results), and Section 5 (radiative transfer and synthetic observations with RADMC-3D).
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Vertical velocities in units of the local speed of sound in our six PLUTO runs after 500 orbital timescales at 50 au. The isothermal run shows a snapshot after only 200 orbits. White contours mark the position at which the critical cooling time for the VSI is reached (Equation (3)), i.e., VSI is theoretically possible within the white lobes.
Paper: All We Are Is Dust in the WIM: Constraints on Dust Properties in the Milky Way’s Warm Ionized Medium
Authors: J. L. West, B. M. Gaensler, M.-A. Miville-Deschênes, N. Mahajan, J. Dechant, F. Boulanger, P. G. Martin, I. A. Zelko
Figure caption: Posterior distribution for the MCMC blackbody fitting of the WNMH I parameters.
Paper: All We Are Is Dust in the WIM: Constraints on Dust Properties in the Milky Way’s Warm Ionized Medium
Authors: J. L. West, B. M. Gaensler, M.-A. Miville-Deschênes, N. Mahajan, J. Dechant, F. Boulanger, P. G. Martin, I. A. Zelko
Figure caption: Posterior distribution for the MCMC fitting of τ(WIM) parameter.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Dust concentration in a steady-state radial pressure bump, embedded in a power-law density profile. Within the pressure bump, we find excellent agreement between our numerical simulation and the predicted profiles.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Vertical diffusion test for our passive dust fluid in PLUTO. We assume a vertically isothermal disk in hydrostatic equilibrium. The resulting dust density distribution agrees well with the analytic prediction.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Radial dust advection tests based on Youdin & Shu (2002).
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Strain surface plots and entropy slices for model s40o1 during the bounce phase. The x and y axes form the equator of the supernova; the z-axis indicates the axis of rotation. For the top two panels, the distance from the origin to a point on the green surface represents the detected h + along that direction. The bottom two panels are entropy slices, with overlaid velocity profiles (arrows). (a) Strain surface plot for h + just after bounce. The star denotes the direction along which the largest h + would be received, what we denote as the preferred viewing angle. (b) Strain surface plot for a toy model of an axisymmetric prolate ellipsoid of mass 1 M ⊙ with polar radius c = 62 km, and equatorial radii a = b = 60 km, with velocity at the pole ﹩\dot{c}=600﹩ km s−1, ﹩\dot{a}=\dot{b}=0﹩ km s−1, replicating the strain surface distribution for bounce seen in Figure 2(a). We note the fluid-like nature of the PNS (deviating from a solid-body ellipsoid) makes assigning a single polar velocity difficult—thus, the discrepancies in the magnitude of the estimate. Nevertheless, our goal is to describe the geometry of the GW distribution, which agrees quite well. (c) Entropy slice through the pole (z-axis) from model s40o1 2 ms after bounce. Notice the PNS surface (solid black line: 1011 g cm−3) slightly prolate, after being deformed from the infalling matter. The PNS will ringdown, finally achieving an equilibrium as an oblate spheroid, due to centrifugal effects. For scale, every centimeter on the page corresponds to 5.6 × 109 cm s−1. (d) Entropy slice through the equator from model s40o1 2 ms after bounce display the axisymmetry of the PNS before convective instabilities create asymmetries.