adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution of Low Surface Brightness Ultrathin Galaxies: The Role of Dark Matter Halo and Bar Formation on Disk Thickness
Authors: K. Aditya, Arunima Banerjee
Figure caption: The time evolution of the stability criterion Q. In the top two panels, we show the models c2, c6, and c12, and in the following panels, we show their massive counterparts with a higher stellar mass fraction. We indicate the typical extent of the stellar disk with a vertical dashed line at 4RD. The horizontal line indicates the criterion for marginal stability: Q = 1.
Paper: Evolution of Low Surface Brightness Ultrathin Galaxies: The Role of Dark Matter Halo and Bar Formation on Disk Thickness
Authors: K. Aditya, Arunima Banerjee
Figure caption: The time evolution of the bar instability criterion X. In the top two panels, we show the models c2, c6, and c12, and in the following panels, we show their massive counterparts with a higher stellar mass fraction. The horizontal line indicates the bar instability criterion: X = 1.1.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: CO2 escape rates are sensitive to interpolation approaches. Leftmost panel: atmospheric escape rate as a function of XUV flux, scaled to Earth’s present-day value. The dots and connected lines represent output from F. Tian (2009) and F. Tian et al. (2009). The rightmost points for super-Earths are extrapolated by F. Tian (2009). The dashed line shows the energy-limited escape rate assuming an efficiency of 0.1. We interpolate their model output, and our results for near-Earth-sized planets are sensitive to the interpolate approach used; (b)–(g) show this sensitivity. In (b) and (c), we interpolate ﹩{\mathrm{log}}\,{F}_{\,\rm{xuv}\,}﹩ with planetary mass Mp; (d) and (e) interpolate ﹩{\mathrm{log}}\,{F}_{\,\rm{xuv}\,}﹩ with the logarithm of planetary mass (﹩{\mathrm{log}}\,{M}_{p}﹩); (f) and (g) exclude Mars data and assume the escape rate scales with gravitational potential energy (GMp/Rp), interpolating between Fxuv and Rp/(GMp). The upper panels illustrate how the escape rate varies with XUV flux for different planetary masses, while the lower panels show how the escape rate changes with planetary mass for various XUV flux levels. The dots represent benchmark output obtained from the leftmost panel, which is used for interpolation. Overall, the linear planetary mass provides higher escape rate estimates for near-Earth-sized planets compared to the other methods.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: The ratio of EUV luminosity to X-ray luminosity is shown as a function of X-ray luminosity. The X-ray flux is calculated for a 0.5 solar-mass star evolving from 1 Myr to 1 Gyr. The blue line and shaded region represent the results from G. W. King & P. J. Wheatley (2020) including uncertainties. Additional colorful lines, labeled with wavelength ranges in Å, are obtained from Table 4 of G. W. King et al. (2018), where the left bracket indicates the X-ray range and the right bracket indicates the EUV range. The dotted black line is derived from C. P. Johnstone et al. (2021).
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Carbon loss rate as a function of semimajor axis for planets with CO2-dominated atmospheres orbiting a Solar-like star at t = 1 Myr. The shaded region represents the range between the maximum and minimum values under certain assumptions. The uncertainties are broken down as follows: (a) Using the center values of γ for EUV extrapolation and an interpolation of CO2 escape rates to Mp (linear), the uncertainty comes solely from the choice of X-ray model. (b) Adopting the J12+G16 X-ray model and linear escape rate interpolation, the uncertainty arises only from the EUV extrapolation. (c) Using the J12+G16 X-ray model and center EUV extrapolation values, the uncertainty stems only from escape rate interpolation. (d) Incorporating all uncertainties. The uncertainties from the X-ray model and EUV extrapolation are of the same order of magnitude. The uncertainty from the interpolation method of CO2 escape rates is more significant for near-Earth-sized planets but negligible for super-Earths. The total uncertainty results in the loss rates for an eight-Earth-radius planet overlapping with those of a one-Earth-radius planet.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: The fraction of carbon sequestered in the mantle relative to the total carbon mass after complete magma ocean solidification, shown as a function of planetary mass, for a pure-CO2 atmosphere (left) and a pure-CH4 atmosphere (right). The fraction increases with planetary mass due to the solubility law, which governs surface pressure, and the reduced atmospheric column mass at higher gravity with a given surface pressure. The blue line represents the lowest initial carbon case in our study, where the carbon-to-planetary mass ratio is 10−4Mp, while the pink line corresponds to the most carbon-rich case, 10−2Mp. A higher initial carbon concentration in the magma ocean results in more carbon being retained in the mantle post-solidification. Solid lines indicate a conservative solid-melt partition coefficient, while dashed lines represent a higher partition coefficient, following L. Elkins-Tanton (2008).
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Sample size required to detect the trend—measured bulk densities increase with increasing Teq—as a function of relative measurement uncertainties in radius and mass, for two different assumptions of the variance of the solid body’s density (Comp Var): (a) fixed Earth-like composition; (b) Gaussian scatter with σ = 1/3 the difference between pure-silicate and Earth-like. The vertical and horizontal dashed lines indicate the average relative uncertainties in mass and radius for current-day observations (see Section 4.3.1) for sample details. The contour lines are smoothed by a Gaussian filter, and the remaining wiggles are artifacts of the Monte Carlo and smoothing.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Upper panels: the ratio of X-ray luminosity to bolometric luminosity evolves over time for stellar masses from 0.1 M⊙ to 1 M⊙. The left panel presents the parameterization from F. Selsis et al. (2007), while the right panel shows the results obtained by combining data from A. P. Jackson et al. (2012) and E. F. Guinan et al. (2016). Lower panels: the X-ray luminosity scaled to solar X-ray flux evolves over time.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: The loss rate per surface area for an N2/O2 atmosphere is shown as a function of XUV flux and planetary mass, interpolated/extrapolated from R. D. Chatterjee & R. T. Pierrehumbert (2024). The dark purple region indicates where hydrostatic escape occurs, with the escape rate fixed at 10−17 kg s−1 m−2. The white dashed lines show bounds to the energy-limited regime.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: Stellar luminosity (Lbol) normalized to the Sun’s luminosity at the present-day (L⊙), and stellar radius (R*) normalized to the Sun’s radius (R⊙) vs. time from the model of I. Baraffe et al. (2015) for star masses ranging from 0.1 to 1.0 M⊙.
Paper: The Cosmic Shoreline Revisited: A Metric for Atmospheric Retention Informed by Hydrodynamic Escape
Authors: Xuan Ji, 纪璇, Richard D. Chatterjee, Brandon Park Coy, Edwin Kite
Figure caption: The N2/O2 loss rate as a function of XUV flux. In our Monte Carlo simulations, we randomly sample the ϵN2O2 from a uniform distribution between 0 and 1. The variations in escape rates resulting from this sampling are illustrated by the colorful lines.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Correlations among burst rate, average burst duration, average burst fluence, and extragalactic (+halo) DM for the repeating FRBs in our sample. As discussed in Section 4.1, we do not subtract a Galactic halo contribution from the total DM. We only include sources for which we have ≥2 bursts with the complex raw voltages recorded. The shown Spearman p-values and correlation coefficients are the median value from 1000 MC iterations in which we iterate over the measured parameter uncertainties and calculate a new p-value and correlation coefficient at each iteration. Uncertainties are calculated using the median absolute deviation from the median (MADFM).
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The 1.3 mm continuum emission (Panel (A)) and the 12CO(2−1) emission moment maps of NGC 7052 derived from our ALMA data: integrated intensity (Panel (B)), intensity-weighted mean LOS velocity (Panel (C)), and intensity-weighted LOS velocity dispersion (Panel (D)). The synthesized beam of the observation is illustrated in the lower-left corner of each map as a black ellipse. Panel (E): The integrated spectrum extracted within a square box of ﹩4\mathop{.}\limits^{^{\prime\prime} }4\times 4\mathop{.}\limits^{^{\prime\prime} }4﹩ (or 1.5 × 1.5 kpc), the horizontal dotted–dashed line represents the zero flux level. Panel (F): A position–velocity diagram extracted along the major axis with an adopted systemic velocity vsys = 4610 km s−1 and a PA Γ = 63﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Panel (A): Our MGE fitting approach for the nuclear 12CO(2−1) gas emission, where we fit the two emission peaks separately. In each MGE fit, the yellow regions indicate masked areas, including one emission peak and the overlapping region, which are excluded from the fit. Panel (B): A 2D superposition of the two MGE fits: MGE 1 (red) and MGE 2 (green) over the ALMA 12CO(2−1) observation. The dashed lines in the same colors mark the peak positions, which also represent the centers of MGE 1 and MGE 2. Panel (C): Same as Figure 4, showing a comparison between the ALMA surface mass density and the reconstructed model from MGE 1 and 2 at the same contour levels.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The ALMA 12CO(2−1) integrated intensity (contours), which are overlaid on the HST/Wide Field Planetary Camera 2 Wide Field Camera F814W image to highlight the coincidence of the gas distribution with the dust plane.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The comparison of HST/WFPC2 WFC F814W images with its MGE model is shown in 2D surface brightness density within the FoV of 80″ × 80″ (left) and zoom into 7″ × 7″ at the center (right). Black contours represent the data, while red contours represent the model, highlighting their agreements at corresponding radii and contour levels. Yellow regions indicate the masked areas containing foreground stars, bad pixels, and the central dust disk.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Left: Overlay of the HST/Wide Field Planetary Camera 2 Wide Field Camera F814W image with the high-resolution (beam size of 5″) C-band (6 GHz) VLA image clearly illustrates the jet at a PA of ∼18﹩\mathop{.}\limits^{^\circ }﹩5, which corresponds to ∼45° relative to the dust plane. Right: Overlay of the Pan-STARRS r-band image with the 1.4 GHz NVSS contours (beam size of 45″) highlighting the extent of the large-scale radio lobes.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: A comparison of 12CO(2−1) moment maps among our ALMA data (left), the best-fitting KINMS model applied the SKYSAMPLER tool (middle), and the best-fitting KINMS model assumed a sum of two center-offset Gaussians (right) to spatially describe the 12CO(2−1) distribution shows a strong agreement between the two. For each moment map (data vs. model), we used the same colorbar. Other demonstrations are all as similar as Figure 5.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The morphological distribution of 12CO(2−1) gas is shown along a cut through the major axis, passing through the center and the two emission peaks of the integrated intensity map of NGC 7052. Our ALMA data is plotted in black, while our analytically axisymmetric model of two center-offset Gaussian functions for the gas surface brightness, is shown in green.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Cumulative mass comparison between our MGE model constrained from the WFC image and the model constrained by M. D. Smith et al. (2021) with the PC image. Both constraints used the same HST observations.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The cumulative molecular gas mass reconstructed from our gas MGE models is validated against the estimate from the 12CO(2−1) emission observed with the Nobeyama 45 m single-dish telescope (Z. Wang et al. 1992).
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: Top panel: residuals from continuum-subtracted 6–7 keV Resolve spectrum showing a wealth of complex Fe K lines marked using vertical dashed lines. The He-like Fe XXV emission complex dominates the residuals, showing a mix of forbidden and recombination transitions. An inset plot shows a zoomed-in view of 6.9 keV, capturing weak H-like Fe XXVI absorption line features. Bottom panel: steppar results for absorption line energy and normalization after scanning a narrow Gaussian absorption to the continuum model. The red, green, and blue contours correspond to 68%, 90%, and 99% confidence levels.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: Model-fitted unfolded XRISM spectra for Resolve (top panel) and Xtend (bottom panel) instruments, respectively, by using a combination of diskbb, power-law, and Gaussian models.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: Best-fitted photemis model fitted to the 5–8 keV Resolve spectrum is shown. The top and bottom panels represent the decomposition of model components and residuals, respectively.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: Best-fitted JeTCAF model fitted spectra in the 2–10 keV energy band are shown. The top and bottom panels represent the Resolve and Xtend instruments, respectively. The bottom windows of each panel show the residuals of the fits.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: The Xtend spectrum in the range 6.3–7.3 keV is shown in the upper panel. The middle and lower panels represent the fitted continuum in the 2–0 keV energy band, ignoring the 6.3–7.3 keV region.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: The Resolve spectrum in the range 6.3–7.3 keV is shown in the upper panel. The lower panel represents the fitted continuum in the 2–10 keV energy band, ignoring the 6.3–7.3 keV region.
Paper: Distinct Fe K Line Complexes in MAXI J1744−294 Revealed by XRISM High-resolution Spectroscopy
Authors: Kaushik Chatterjee, Santanu Mondal, Biswaraj Palit, Chandra B. Singh, Sujoy Kumar Nath, Mayukh Pahari, Brajesh Kumar, Wei Wang, Hsiang-Kuang Chang, Xiaowei Liu
Figure caption: Model-fitted unfolded XRISM spectra for Resolve (top panel) and Xtend (bottom panel) instruments, respectively, by using a combination of kerbb, power-law, and Gaussian models.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Luminosity vs. time for X56 = 0.04 from t ≈ 2 to 8 hr. The legend provides the angle from which the observer views the SN. We compare against the light curve predicted by A. L. Piro (2012) labeled “Analytics” describing an SN without shock-heated ejecta.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Slice plots showing density (top) and temperature (bottom) on the ϕ = 0° plane after evolving the material leaving the edge of the original simulation to t = 2 hr after the explosion for X56 = 0.04.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Illustration of spherically symmetric ejecta impacting a spherical donor, with variable definitions. The ejecta momentum is decomposed into its components tangentially and normally to the donor surface, the latter being imparted to the donor.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Plots showing temperature and the τ = 1 and τ = 10 optical thickness isolines on the ϕ = 0° plane at t = 5.0 hr (top) and t = 18.5 hr (bottom) assuming X56 = 0.04.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Luminosity vs. time for X56 = 0.08 from t ≈ 2 to 8 hr. The legend provides the angle from which the observer views the SN. We compare against the light curve predicted by A. L. Piro (2012) labeled “Analytics” describing an SN without shock-heated ejecta.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Luminosity vs. time for X56 = 0.04 up to ≈1 day after the SN at various viewing angles.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Diagram of our numerical setup highlighting several features of the resulting wake.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Temperature as a function of θ at τ = 1 (integrated radially) for a set of times after the explosion.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Radiation energy density at the measurement radius Rm vs. θ at various times.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Slice plots showing density (top) and temperature (bottom) on the ϕ = 0° plane 200 s after the SN. The red arrows indicate the location of the secondary shock.
Paper: The First Day of a Type Ia Supernova from a Double-degenerate Binary
Authors: Gabriel Kumar, Logan J. Prust, Lars Bildsten
Figure caption: Several properties of the ejecta measured at rout = 10.8 R⊙ plotted vs. θ at various times. The density (upper left) shows a rapid drop-off at small θ, differing from D. Kasen (2010). The transverse velocity (upper right) illustrates the positions of the shocks and shows rarefaction waves between them. The temperature (lower left) reveals that the shock-heated ejecta are much hotter than the unshocked gas, causing much of the shocked ejecta to be radiation pressure dominated (lower right).