adsabs/AstroCLIMB huggingface dataset:
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). V. The Complete SMUDGes Catalog and the Nature of Ultradiffuse Galaxies
Authors: Dennis Zaritsky, Richard Donnerstein, Arjun Dey, Ananthan Karunakaran, Jennifer Kadowaki, Donghyeon J. Khim, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: Top panel: candidates found or missed in MzLS/BASS that are present in the DECaLS/DES catalog. Bottom panel: candidates found or missed in DECaLS/DES that are present in the MzLS/BASS catalog. Detection: inadequate or no wavelet detections (Section 3.1, Step 4); Sérsic: Failed to meet our Sérsic screening criteria (Section 3.1, Step 6); Galfit1: Failed our initial GALFIT screen (Section 3.1, Step 8); Galfit2: Failed our final GALFIT estimates (Section 3.1, Step 9); Classifier: Failed to meet the probability threshold required by our automated classifier (Section 3.4).
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). V. The Complete SMUDGes Catalog and the Nature of Ultradiffuse Galaxies
Authors: Dennis Zaritsky, Richard Donnerstein, Arjun Dey, Ananthan Karunakaran, Jennifer Kadowaki, Donghyeon J. Khim, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: Cirrus contamination within DR9 of the Legacy Survey footprint. Regions in black exceed our dust proxy thresholds of either 0.1 MJy sr−1 for WISE 12 μm map or 0.05 for τ 353 and comprise ∼28% of the entire footprint. The Galactic plane is shown in orange.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: Left panel shows the collected Type 2 AGNs in the BPT diagram (contour filled by bluish colors) of O3HB vs. N2HA. Solid and dashed purple lines show the dividing lines between different kinds of narrow-emission-line galaxies in Kewley et al. (2006), Kauffmann et al. (2003a), H II galaxies, composite galaxies, and AGNs. In left panel, small circles plus error bars in dark green show the collected 156 Type 2 AGNs with apparent long-term variabilities. The middle panel and right panel show the distributions of redshift and [O III] line luminosity (L O3) of the 14,353 collected Type 2 AGNs (histogram filled by blue lines) and of the 155 Type 2 AGNs with apparent long-term variabilities (histogram filled by dark green lines). The individual Type 2 AGNs SDSS J075736.47+532557.1 (plate-mjd-fiberid = 1870-53383-0466) has measured redshift to be zero in SDSS; therefore, the SDSS J075736.47+532557.1 is not included in the middle panel and right panel.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: CSS V-band light curves of SDSS 0271-51883-0252 and 1239-52760-0047. In each panel, symbols in different colors show the light curves with different CSS IDs as shown in legends. And the light curve shown in dark green is the final accepted CSS light curve.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: Top left panel shows the spectrum (in dark green) of SDSS 2374-53765-0174 and the corresponding SSP method determined host-galaxy contributions (in red). Bottom left panel shows the line spectrum of SDSS 2374-53765-0174 by the SDSS spectrum minus the host-galaxy contributions. Top right panel shows the best descriptions (in red) to the emission lines (in dark green) around Hα by multiple Gaussian functions, in the line spectrum shown in bottom left panel. In the bottom region of the top right panel, solid and dashed lines in blue show the determined first and second narrow [N II] components, solid and dashed lines in pink show the determined first and second narrow [S II] components, and solid and dashed purple lines show the determined first and second narrow components in Hα. Bottom right panel shows the residuals calculated by the line spectrum minus the best-fitting results and then divided by uncertainties of the spectrum. In the bottom right panel, solid and dashed red lines show residual = 0, ±1, respectively.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: Left panel shows properties of ﹩\mathrm{ln}(\sigma /(\mathrm{mag}/{\mathrm{days}}^{0.5}))﹩ and ﹩\mathrm{ln}(\tau /\mathrm{days})﹩ of the 156 Type 2 AGNs with apparent long-term variabilities. Vertical dashed blue lines and horizontal dashed red lines show the available ranges of ﹩\mathrm{ln}(\sigma /(\mathrm{mag}/{\mathrm{days}}^{0.5}))﹩ and of ﹩\mathrm{ln}(\tau /\mathrm{days})﹩ from the OGLE-III quasars in Kozlowski et al. (2010). Right panel shows distributions of NP of the 156 Type 2 AGNs (histogram filled by dark green lines) with apparent long-term variabilities and the other Type 2 AGNs (histogram filled by blue lines).
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: TDE roughly expected variabilities described by t −5/3 shown in solid red line in the long-term CSS light curve of SDSS 0747-52234-0400.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: Left panel shows spectrum (in dark green) of SDSS J075736.47+532557.1 (plate-mjd-fiberid = 1870-53383-0466) with apparent Ca II λ3934, 3969 Å absorption features marked by vertical red line. Right panel shows the spectrum around Hα to ensure no broad component in Hα.
Paper: Systematic Research of Low-redshift Optically Selected SDSS Type 2 AGNs but with Apparent Long-term Optical Variabilities from Catalina Sky Survey. I. Data Sample and Basic Results
Authors: XueGuang Zhang
Figure caption: Distributions of CSS V-band magnitude of the 156 Type 2 AGNs (histogram filled by dark green lines) and with apparent long-term variabilities and the 12,881 Type 2 AGNs (histogram filled by blue lines).
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Comparison of the radial profiles of several quantities between our code Gmunu and the reference codes (AGILE-BOLTZTRAN, VERTEX, and GR1D) at the moment of core bounce. For instance, we compare rest-mass density ρ, radial velocity v  r /c, matter temperature T, matter entropy per baryon s, neutrino root mean squared energy ﹩\sqrt{\langle {\epsilon }_{{\nu }_{i}}^{2}\rangle }﹩, and electron fraction Y  e . The solid lines show the numerical results obtained by Gmunu. A shock is formed at ∼10 km, and the matter entropy reaches 3 k B/baryon at the shock. Our results generated by Gmunu are quantitatively agreeing with the reference solution produced by AGILE-BOLTZTRAN (dashed–dotted lines), VERTEX (dotted lines), and GR1D (dashed lines).
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Evolution of central matter entropy per baryon (s, upper panel), electron, and total lepton number fractions (Y  e  and Y lep ≡ Y  e  + Y  ν , lower panel) as functions of central density ρ  c  of a collapsing 15 M⊙ star before core-bounce. The solid lines show the numerical results obtained by Gmunu. Note that the evolution of lepton numbers is highly sensitive to the implementations of the multigroup coupling and radiation advection in optically thick regions. Our results agree very well with the results of AGILE-BOLTZTRAN (dashed–dotted lines), VERTEX (dotted lines), and GR1D (dashed lines).
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Comparison of the numerical solutions obtained by utilizing Gmunu (red dots) and the analytic solutions (black solid lines) of the energy advection test introduced by Müller et al. (2010). Three cases are considered in this test: namely, we consider (i) just the shape velocity profile without gravitational fields (left column); (ii) just the gravitational fields without velocity profile (middle column); and (iii) both the shape velocity profile and gravitational fields (right column). The upper panels show the shifted velocity profile v  r  + 1 (blue solid lines), conformal factor ψ (orange solid lines), and lapse function α (green solid lines) in different cases. The middle and lower panels compare of the simulated results of the rescaled average neutrino energy 〈ε〉/〈ε〉∞ and the redshift-corrected luminosity L rs/L rs,∞ obtained by utilizing Gmunu (red dots) and the analytic solutions (black solid lines). In all cases, results returned by Gmunu are in agreement with the analytic expressions. This test demonstrates that Gmunu is able to handle the frequency advection terms in the evolution of radiations, which corresponds to gravitational redshift and Doppler shift affects of the radiation with different frequencies.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Upper panel: the relative variation of the central rest-mass density ρ  c  of the hot neutron star in time. Middle panel: time evolution of far-field neutrino luminosities measured by an observer comoving with fluid at 100 km of a hot neutron star. The luminosities are zero for t ≲ 3 ms as the neutrino signals are not yet arrived at the extraction point. Lower panel: the fast Fourier transform of the central rest-mass density, and the luminosities of electron and antielectron neutrinos. The amplitude of the fast Fourier transform of the central rest-mass density (navy solid line) has been rescaled for a better visualization. The vertical dashed lines represent the known eigenmode frequencies (Galeazzi et al. 2013). The eigenmode frequencies we obtained are in good agreement with the one in Galeazzi et al. (2013), Neilsen et al. (2014).
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of far-field neutrino root mean squared energies (﹩\sqrt{\langle {{\epsilon }_{\nu }}^{2}\rangle }﹩, left panel) and luminosities (L  ν , right panel) measured by an observer comoving with fluid at 500 km of a collapsing 15 M ⊙ star. The solid lines show the numerical results obtained by Gmunu. To compare the deleptonization burst and the early post-bounce evolution of the luminosity of electron-type neutrino more in detail, we changed the scale after t > 30 ms (upper right panel). The evolution of these neutrino quantities is again highly sensitive to the implementation and essential to the predictions of observational signatures. Our results agree very well with the reference results produced by AGILE-BOLTZTRAN (dashed–dotted lines), VERTEX (dotted lines), and GR1D (dashed lines).
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: The radiation energy density profile at t = 1, where the initial conditions are kept fixed for x ≤ − 0.4 during the entire evolution. The radiation beam propagates from left to right, and is blocked by the optically thick cylinder (white dashed line) with high absorption opacity ﹩{\bar{\kappa }}_{a}={10}^{6}﹩. As a result, this cylinder split the beam into two. The two beams keep propagating to the right, and a shadow is cast behind the cylinder.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Time evolution of the shock radius. The solid lines show the numerical results obtained by Gmunu. The reference results produced by AGILE-BOLTZTRAN, VERTEX, and GR1D are shown with dashed–dotted line, dotted line, and dashed line, respectively. The shock radius predicted by Gmunu is mostly agreeing with GR1D for t − t bounce ≲ 40 ms while it is approximately 10 km larger since then. Since then, it goes between the result of AGILE-BOLTZTRAN and GR1D.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: The radiation energy density profile scaled with r 2 at different time slides. The radiation propagates spherically from the source to outside, and is blocked by the optically thick sphere (white dashed line) with high absorption opacity ﹩{\bar{\kappa }}_{a}={10}^{6}﹩. As in the single beam case (see Figure 7), this sphere absorbs radiations and causes a shadow behind it.
Paper: General-relativistic Radiation Transport Scheme in Gmunu. I. Implementation of Two-moment-based Multifrequency Radiative Transfer and Code Tests
Authors: Patrick Chi-Kit Cheong, 志杰 張, Harry Ho-Yin Ng, Alan Tsz-Lok Lam, Tjonnie Guang Feng Li
Figure caption: Comparison of the energy density profile E at time t = 1, 2, 3, 4 to the analytic solution (gray solid lines). Since the simulation starts from t = 1, the result is identical to the analytic solution. As shown in the figure, results produced by utilizing Gmunu agree with the analytic solution.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption:  K-band spectra of YSO candidates in the CMa-ℓ224 star-forming region, which show the H Brγ line in emission. All spectra are continuum subtracted and normalized to the peak flux density in the range from 1.97 to 2.47 μm. Red horizontal lines show spectral ranges most affected by telluric lines; the range at 2.0 μm has been removed for clarity.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with Brγ and H2 emission lines and CO bandhead in absorption.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with Brγ emission line and CO bandhead in absorption.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with H2 emission lines and CO bandhead in absorption.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with Brγ and H2 emission lines.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with only H2 emission lines.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with Brγ absorption line.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with CO bandhead in emission.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Integrated maps of the H2 1-0 S(1) line at 2.1218 μm for a subsample of sources where the extended H2 emission is detected (see Table 2). Colors correspond to the line fluxes at each pixel (detections above 3σ), and white contours correspond to the continuum emission in K band (see also Appendix A). Source names are provided in the upper right corners (No. in Table 2). We note that source No. 88 (G224.4514−00.7054) has a nondetection of the continuum emission at 2.1218 μm.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with no emission lines and no CO or Brγ absorption lines.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Similar to Figure C1, but for the H2 1-0 S(0) line at 2.2235 μm. Only emission above 2σ is shown.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Similar to Figure C1, but for the H2 1-0 Q(1) line at 2.4066 μm. Only emission above 2σ is shown.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra with CO bandhead in absorption.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra from double sources—continuation.
Paper: Investigating the Impact of Metallicity on Star Formation in the Outer Galaxy. I. VLT/KMOS Survey of Young Stellar Objects in Canis Major
Authors: Dominika Itrich, Agata Karska, Marta Sewiło, Lars E. Kristensen, Gregory J. Herczeg, Suzanne Ramsay, William J. Fischer, Benoît Tabone, Will R. M. Rocha, Maciej Koprowski, Ngân Lê, Beata Deka-Szymankiewicz
Figure caption: Spectra from three pairs of double sources.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: One quadrant of the particle distribution with corresponding plastic strain in the 2D Verney implosion simulation at 137 μs for a triangular particle initialization with (a) η = 1.6, and (b) η = 3.5; as well as a ring initialization with (c) η = 3.5, and (d) η = 1.6. The small red circles in panels (c) and (d) visualize the particle’s smoothing length. The black ring shows the position of the stopping radius.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Particle distribution and plastic strain in the 2D Verney implosion simulation. For compactness, only one half of the simulation space is shown. The left side shows the initial setup. The right side shows the particles at 137 μs, when 99.9% of the initial kinetic energy has dissipated. The black ring shows the position of the stopping radius.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Total, kinetic, and internal energy per unit length of the 2D Verney implosion together with the results from Howell & Ball (2002). Thick lines correspond to the triangular lattice particle initialization with η = 1.6, while thin lines show the energy for the ring initialization with η = 3.5.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Percentage of dissipated kinetic energy with respect to its initial value for the 2D Verney implosion.
Paper: Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: I. Sagert, O. Korobkin, I. Tews, B.-J. Tsao, H. Lim, M. Falato, J. Loiseau
Figure caption: Time evolution of the dissipated kinetic energy for the grid and relaxed particle initializations.