adsabs/AstroCLIMB huggingface dataset:
Paper: Results of the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC)
Authors: R. Hložek, A. I. Malz, K. A. Ponder, M. Dai, G. Narayan, E. E. O. Ishida, T. Allam Jr, A. Bahmanyar, X. Bi, R. Biswas, K. Boone, S. Chen, N. Du, A. Erdem, L. Galbany, A. Garreta, S. W. Jha, D. O. Jones, R. Kessler, M. Lin, J. Liu, M. Lochner, A. A. Mahabal, K. S. Mandel, P. Margolis, J. R. Martínez-Galarza, J. D. McEwen, D. Muthukrishna, Y. Nakatsuka, T. Noumi, T. Oya, H. V. Peiris, C. M. Peters, J. F. Puget, C. N. Setzer, Siddhartha, S. Stefanov, T. Xie, L. Yan, K.-H. Yeh, W. Zuo
Figure caption: Relative numbers of objects of each class between the training (left) and test (right) data of PLAsTiCC. The size of the boxes is proportional to the relative numbers in each set and the absolute numbers are in parentheses. The simulated ≃8000 objects in the training set were distributed across the data classes in a different ratio compared to the test data of over 3.5 million objects.
Paper: Results of the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC)
Authors: R. Hložek, A. I. Malz, K. A. Ponder, M. Dai, G. Narayan, E. E. O. Ishida, T. Allam Jr, A. Bahmanyar, X. Bi, R. Biswas, K. Boone, S. Chen, N. Du, A. Erdem, L. Galbany, A. Garreta, S. W. Jha, D. O. Jones, R. Kessler, M. Lin, J. Liu, M. Lochner, A. A. Mahabal, K. S. Mandel, P. Margolis, J. R. Martínez-Galarza, J. D. McEwen, D. Muthukrishna, Y. Nakatsuka, T. Noumi, T. Oya, H. V. Peiris, C. M. Peters, J. F. Puget, C. N. Setzer, Siddhartha, S. Stefanov, T. Xie, L. Yan, K.-H. Yeh, W. Zuo
Figure caption: Correlation tests for the simulated WFD PLAsTiCC data. We used this test to detect any spurious correlations between object ID and the type and other properties provided to the contestants. We disambiguate Galactic and extragalactic sources and consider the WFD and DDF data separately as there are physical correlations that are introduced when aggregating these groups, e.g., all Galactic variables will have a host redshift of z = 0, and all sources within the four DDFs will show strongly correlated values of the Milky Way reddening.
Paper: Results of the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC)
Authors: R. Hložek, A. I. Malz, K. A. Ponder, M. Dai, G. Narayan, E. E. O. Ishida, T. Allam Jr, A. Bahmanyar, X. Bi, R. Biswas, K. Boone, S. Chen, N. Du, A. Erdem, L. Galbany, A. Garreta, S. W. Jha, D. O. Jones, R. Kessler, M. Lin, J. Liu, M. Lochner, A. A. Mahabal, K. S. Mandel, P. Margolis, J. R. Martínez-Galarza, J. D. McEwen, D. Muthukrishna, Y. Nakatsuka, T. Noumi, T. Oya, H. V. Peiris, C. M. Peters, J. F. Puget, C. N. Setzer, Siddhartha, S. Stefanov, T. Xie, L. Yan, K.-H. Yeh, W. Zuo
Figure caption: The distribution of the submissions to PLAsTiCC and the log of the PLAsTiCC metric score as a function of time since the start of the challenge relative to the start of the challenge. The three colored lines indicate the performance of the three prize-winning entries. As the challenge neared completion, the scores started to asymptote to metric scores of near unity. Note that the competition remains “live” to this day, hence the few submissions received after the closing deadline.
Paper: Results of the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC)
Authors: R. Hložek, A. I. Malz, K. A. Ponder, M. Dai, G. Narayan, E. E. O. Ishida, T. Allam Jr, A. Bahmanyar, X. Bi, R. Biswas, K. Boone, S. Chen, N. Du, A. Erdem, L. Galbany, A. Garreta, S. W. Jha, D. O. Jones, R. Kessler, M. Lin, J. Liu, M. Lochner, A. A. Mahabal, K. S. Mandel, P. Margolis, J. R. Martínez-Galarza, J. D. McEwen, D. Muthukrishna, Y. Nakatsuka, T. Noumi, T. Oya, H. V. Peiris, C. M. Peters, J. F. Puget, C. N. Setzer, Siddhartha, S. Stefanov, T. Xie, L. Yan, K.-H. Yeh, W. Zuo
Figure caption: Demographic information for entrants to PLAsTiCC. Only a small fraction of 1315 participants with known demographics were part of the astronomy community. Many of the participants have some data science background. These data were determined from the Kaggle entries or GitHub user pages of the entrants, future studies will include self-identification information from participants.
Paper: Results of the Photometric LSST Astronomical Time-series Classification Challenge (PLAsTiCC)
Authors: R. Hložek, A. I. Malz, K. A. Ponder, M. Dai, G. Narayan, E. E. O. Ishida, T. Allam Jr, A. Bahmanyar, X. Bi, R. Biswas, K. Boone, S. Chen, N. Du, A. Erdem, L. Galbany, A. Garreta, S. W. Jha, D. O. Jones, R. Kessler, M. Lin, J. Liu, M. Lochner, A. A. Mahabal, K. S. Mandel, P. Margolis, J. R. Martínez-Galarza, J. D. McEwen, D. Muthukrishna, Y. Nakatsuka, T. Noumi, T. Oya, H. V. Peiris, C. M. Peters, J. F. Puget, C. N. Setzer, Siddhartha, S. Stefanov, T. Xie, L. Yan, K.-H. Yeh, W. Zuo
Figure caption: The precision and recall as a function of redshift for the SN Ia objects (top two panels) and TDE (bottom two panels). The average value of the threshold used across the classifiers is indicated in the text on the figure. The shaded distributions in each panel show the fractional distribution of the numbers of the transients as a function of redshift. The total number of transients in the sample is also indicated. The evolution with redshift of the metrics depends both on the redshift distribution of the objects and the evolution of the light curves with changing redshift.
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:  φ-velocity distribution in the crust of a neutron star during toroidal oscillations as in Figure 24 with a fluid core and a Tait–Murnaghan EoS crust where both are decoupled from each other via the spherical harmonics approach.
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: Kinetic energy oscillations for the Tait–Murnaghan EoS crust, decoupled via spherical harmonics decomposition of the CCI from the fluid core. The oscillations agree well with the previously explored approximation where we reduced the EoS pressure acceleration for crust particles by κ = 104.
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: The rms’s of spherical harmonics coefficients Vlm  and W  lm   during the simulated toroidal oscillations of the neutron star crust.
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: Toroidal oscillations with a frozen core for the three star setups in Figure 14.
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: Velocity distribution in the crust and core of a neutron star after relaxation at time t ∼ 0.05 s and after toroidal velocity initialization with a fluid core and a Tait–Murnaghan EoS crust at t ∼ 0.005 s. The decoupling was done via the density gradient.
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 particle kinetic energy in the crust and the core for the case of a solid crust with reduced EoS acceleration (κ = 104) that is decoupled from the fluid core. The decoupling is done using the particle positions to determine the normal to the CCI.
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:  φ-velocity distribution in the neutron star crust and core. The crust is decoupled from the core via the particle position. The core is a fluid while the crust is modeled with a solid with a reduced EoS acceleration by κ = 104.
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: Kinetic energy oscillations for the Tait–Murnaghan EoS crust, decoupled via the particle position from the fluid core. The oscillations follow the previously explored approach to reduce the EoS acceleration of crust particles by κ = 104.
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:  φ-velocity and von-Mises stress distribution in the crust and core of a neutron star during toroidal oscillations as in Figure 24 with a fluid core and a Tait EoS crust.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Comparisons between central velocity dispersions. Measurements on LRS2 spectra are plotted along the x-axis. The first three panels show mean dispersions from the uv and orange channels, whereas the fourth and fifth panels show only uv or orange channel dispersions, respectively. On the y-axes are plotted independent dispersions by Lauer et al. (2014; left panel; 37 BCGs), published SDSS dispersions (second panel; 23 BCGs), and our refitted dispersions on SDSS spectra (third to fifth panels; 23 BCGs). χ 2 values are given as text labels. Minimum error bars are adapted, such that χ 2 = 1 in the middle panel. The standard deviation of the velocity dispersion differences is also given in the text labels and is in units of kilometers per second.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Edge-on projection of the FP (black line) for normal Es. Green data points are included, and gray data points are discarded before the fit. The y-axis is proportional to the total galaxy brightness M tot. This is achieved by rotating the 3D data point distribution by an angle ﹩\theta =\arctan (0.5)=26\buildrel{\circ}\over{.} 57﹩ around the ﹩\mathrm{log}({\sigma }_{{\rm{e}}8})﹩-axis, such that the resulting vertical axis is proportional to ﹩2\cdot \mathrm{log}({r}_{{\rm{e}}})+\mathrm{log}\langle {I}_{{\rm{e}}}\rangle \propto {M}_{\mathrm{tot}}﹩. Afterward, the points are rotated by an FP slope-dependent angle φ around the new vertical axis, such that the plane is viewed edge-on. We calculate φ = 8.°48 numerically. Point sizes are proportional to their weight, which is proportional to the inverse of the luminosity function of our sample at the given galaxy luminosity.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Comparison between the measured velocity dispersions in the uv (left) and or (right) channels, depending on the polynomial orders. The numbers after the “×” and “+” symbols on the axes labels refer to the orders of the applied multiplicative and additive polynomials, respectively. That is, first-order multiplicative (×1) and fourth-order additive polynomial (+4) on the x-axis, and fourth-order multiplicative (×4) and no additive polynomial on the y-axis.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Comparison between the measured velocity dispersions in the uv (left) and or (right) channels, depending on the stellar library. The values on the x-axis correspond to the X-shooter stellar library, and the values on the y-axis correspond to the MILES stellar library. Fourth-order multiplicative and no additive polynomials are applied.
Paper: Minor Mergers Are Not Enough: The Importance of Major Mergers during Brightest Cluster Galaxy Assembly
Authors: Matthias Kluge, Ralf Bender
Figure caption: Comparison of Lick indices of standard stars measured by Worthey et al. (1994; x-axis) and measured by us on LRS2 spectra (y-axis). Blue, orange, and red colors correspond to uv, orange, and red LRS2 channels, respectively. The continuous gray line shows the 1:1 relation, and the dashed line is the fit that minimizes the squared orthogonal residuals. There is no data for the Fe4668 line, because it falls between the uv and orange channels. All units are in [Å] apart from Mg1, Mg2, CN1, CN2, and all TiO lines, which are measured in [mag]. The compared standard stars are: HD101501, HD132142, HD64606, HR2600, HR3369, HR3418, HR3422, HR3427, HR3428, HR6136, HR6159, and HR7576.
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: Accretion luminosity vs. absolute K-band magnitude. Red stars show YSOs in CMa-ℓ224, blue circles show MYSOs (Cooper et al. 2013), light green “+” symbols show MYSOs from SMC (Ward et al. 2017), green crosses show MYSOs from LMC (Ward et al. 2016), violet open squares show YSOs in Orion (Manara et al. 2012), and orange triangles show low-mass YSOs in Perseus (Fiorellino et al. 2021). The dashed lines show linear fits separately for each of the data sets with the same colors. The gray line shows a linear fit to all data points. All luminosities have been corrected for extinction.
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: Accretion luminosity vs. star luminosity. The symbols are the same as in Figure 10. The dashed line shows a linear fit to the data. All luminosities have been corrected for extinction.
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: Histogram of the accretion luminosities (L acc) based on Brγ line luminosity (Table 3) measured toward YSOs in CMa-ℓ224 (in dark orange). The median value of L acc is indicated at the top of the plot. The orange and yellow hatched histograms show the distribution of L acc for sources classified by Sewiło et al. (2019) as, respectively, Class I and Class II YSO candidates.
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: Distribution of accretion luminosity in the main filament in CMa-ℓ224 (blue color scale). Class I sources are marked with hexagon and Class II sources with star symbols. Black circles mark targets without A V estimation. The three regions identified by Sewiło et al. (2019) are marked with gray circles.
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: Cumulative distributions of accretion luminosities for clusters A (solid), B (dashed), and C (dotted line), as defined in Sewiło et al. (2019). Sources without A V estimates are excluded.
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: KMOS K-band continuum maps for single YSO candidates. Source names are provided in the upper right corners (No. in Table 2). The contour levels are 0.25, 0.5, and 0.75× the K-band continuum peak. Only pixels with a continuum flux density above 3σ are 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 A1, but for the faintest sources in the sample: Nos. 11, 14, 26, and 69 (see Table 2). The continuum was integrated over the entire K-band spectrum in every pixel to increase the signal-to-noise ratio.
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 2-1 S(1) line at 2.2477 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(3) line at 2.4237 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: Maps in several H2 lines in source No. 47, which shows detections of the most highly excited H2 lines in the entire sample (see Table 2).
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 CO ν = 2-0 line at 2.29 μm. Colors correspond to the line fluxes at each pixel (detections above 2σ), and white contours show the continuum emission in K band (see also Appendix A).
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 for the H Brγ line at 2.1661 μm. Colors correspond to the line fluxes at each pixel (detections above 2σ), and white contours show the continuum emission in K band (see also Appendix A).
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 C8, but the maps show the CO ν = 3-1 line at 2.32 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: Similar to Figure C8, but the maps show the CO ν = 4-2 line at 2.35 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: Similar to Figure C8, but the maps show the CO ν = 5-3 line at 2.38 μm.
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 3D Verney implosion simulation at approximately 100 s. The top half corresponds to one-eighth of a setup with 1.2 million particles distributed in a regular grid while the bottom half is one-eighth of 8.8 × 105 particles that have first been relaxed in an external potential. We add one-quarter of a gray half sphere with a radius of 3 cm to show the location of the analytic 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: The three NST setups with crust and core, composed of N = 2.8 × 104, 9.5 × 104, and 2.2 × 105 particles in total. N  C  gives the number of particles in the crust only. The left side of the stars shows the distinction into crust particles (gray) and core particles (white) while the color-coded right side shows the density. In all three cases, the crust is defined as a layer of particles at a density of ∼1.4 × 1014g cm−3 ∼ 0.5ρ sat. The circle in the top left of each star gives the smoothing length of a crust particle, marking the particle’s SPH neighbors as the particles located within the circle. The particle distributions are achieved with relaxation steps (1) and (2), as described in Section 5.1.
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 total, internal, and kinetic energies in the 3D Verney implosion simulation for grid and relaxed initial particle configurations.
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: Cross section of the 3D Taylor anvil, initialized by placing particles in a lattice, with the pressure field on the left and the plastic strain on the right at 80 μs. The dashed outline shows the shape of the rod from Burton et al. (2015) at the same time for the CCH2 (left) and CGR (right) schemes.
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: Foot of the Taylor anvil in Figure 10 as viewed from the bottom. The plastic strain is color coded.