adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Metallicities derived by CYCLE-STARNET from LAMOST DR8 MRS spectra of nine open clusters, shown as a function of their effective temperatures. If reported in the OCCAM survey catalog (Donor et al. 2020), the ranges of the clusters’ metallicities are shown as red shading; otherwise, blue shading shows the [Fe/H] ranges from the open clusters catalog (Bossini et al. 2019; Monteiro et al. 2020; Dias et al. 2021). The means and dispersions are marked using the corresponding colors. Gray symbols represent values calculated by LAMOST MRS samples in each panel.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Repeated errors of LAMOST MRS stellar parameters and chemical abundances derived by CYCLE-STARNET, plotted as a function of S/N. The 1σ values of the errors in each S/N bin are represented by black dots, and the fitting relationship is shown by a red curve with the corresponding expression in the upper right corner of each panel. In the top panel, we show the number of spectra in each S/N bin with light blue bars. Except for [C/Fe], the number (ratio) of spectra in each S/N bin for other elements is basically the same as that shown in the top panel.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Residuals between LAMOST MRS elemental abundances with respect to the reference values of the member stars of nine clusters (ASCC 16, ASCC 19, ASCC 21, Melotte 20, Melotte 22, NGC 2632, NGC 2682, NGC 6811, and NGC 752), shown as a function of spectral S/N. The blue horizontal lines are the value of zero in each panel. The error bars of the mean bias in the S/N bins ([10, 50], [50, 100], [100, 150], [150, 200], and [200]) are shown in red, and 1σ of the residuals represent its precision for each element in the legend.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: The elemental abundances by CYCLE-STARNET are displayed with gray points with errors as a function of T eff of the clusters (Melotte 20, Melotte 22, NGC 2682, NGC 752, NGC 1039, NGC 2168, NGC 2281, and Stock 2), also, the chemical abundance reference values and their errors (from the OCCAM DR17 catalog) of the clusters are shown with red shading.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Distribution of CYCLE-STARNET estimates of nine open clusters in the Kiel diagram, color coded by their metallicities. The MIST isochrones are drawn based on the cluster’s ages and metallicities provided by Bossini et al. (2019), Monteiro et al. (2020), and Dias et al. (2021), except for Stock 2.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Same as Figure 13 but for the elements by CYCLE-STARNET (this work) and SPCANet (Wang et al. 2020) as a function of elements [X/Fe]. The residual represents [X/Fe]SPCANET − [X/Fe]this work.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Density distributions in the Kiel diagram of LAMOST MRS stellar parameters by LASP (top left) and SPCANet (Wang et al. 2020; top right). Comparisons of three stellar parameters between the two methods are shown in the bottom panels, and the red dotted lines indicate the one-to-one lines.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: The S/N density distributions of the LAMOST DR8 MRS blue (top panel) and red (bottom panel) arms as a function of the Gaia photometric G magnitude. The error bars in red represent the S/Ns of the blue (top panel) and red (bottom panel) arms in different G magnitude bins, each of which spans 0.5 mag.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Color–absolute magnitude diagram of the LAMOST DR8 MRS objects color coded by number density in log scale. Here the magnitude is calculated without extinction correction.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: LAMOST DR8 observation footprints. The low-resolution survey (LRS) is shown in blue, and the median-resolution survey (MRS) is in red.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Training losses of CYCLE-STARNET as a function of epochs. The loss function of CYCLE-STARNET consist of three parts: transfer loss (X synth−>obs, X obs−>synth), cycle loss (X synth−>synth, X obs−>obs, X synth−>obs−>synth, X obs−>synth−>obs), and adversarial loss(C synth(X real), C synth(X fake), C obs(X real), X obs(X fake)).
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: The t-SNE test pairs of two of 10,000 synthetic spectra X_synth, 10,000 LAMOST MRS observed spectra X_obs, 10,000 X_synth_obs spectra, 10,000 X obs_synth in the observed (bottom right panel) and synthetic (bottom left panel) domains and their shared features (top right panel) mapped in two-dimensional hyperparameter space by CYCLE-STARNET.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Comparison of three stellar basic parameters between the LAMOST DR8 MRS (CYCLE-STARNET) and APOGEE (ASPCAP) DR16 (top panels), GALAH DR3 (middle panels), and RAVE DR6 (bottom panels) survey data sets, color coded by the number density. From left to right, the panels are for T eff, log g, and [Fe/H]. The number of samples, medians, and scatters of the differences of each stellar parameter are marked in each panel. The residuals vary with each stellar parameter and are shown below. The dashed lines are the reference lines.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Distribution of LAMOST DR8 MRS stellar parameters (Flagquality = 0) by CYCLE-STARNET in the Kiel diagram color coded by [Fe/H] (left panel) and number density (right panel). The MIST isochrones are superimposed on the left panel. The dashed and solid lines represent ages of 1.5 and 8 Gyr, respectively. For each age, red, yellow, light blue, and dark blue represent a [Fe/H] of −1.0, −0.5, 0, and +0.5 dex, respectively.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Residual density distribution of log g between LAMOST MRS by CYCLE-STARNET and the Kepler DR25 asteroseismic catalog (top panel). The bottom panel shows that of LAMOST MRS and the APOKASC catalog for their common stars. In each panel, the value of the horizontal lines is zero. Bias is given as the median of the residuals combined with the 84% and 16% quantiles.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Residual density of elemental abundances between LAMOST DR8 MRS by CYCLE-STARNET and APOGEE DR16 ASPCAP in the left panels and GALAH DR3 in the right panels. The distribution of the residuals is displayed beside the density distributions. The bias and scatter of each element is given in the individual figure panel legends. The dashed line is the value of zero in each panel.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Distribution of elemental abundances [X/Fe] estimated by CYCLE-STARNET, plotted as a function of [Fe/H] for LAMOST DR8 MRS, color coded by number density in the log scale.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Comparisons (top panels) and residuals (bottom panels) of three stellar parameters (T eff in the left panels, log g in the middle panels, and [Fe/H] in the right panels) between LAMOST MRS by CYCLE-STARNET and the PASTEL catalog. Biases and scatters for the comparisons of three stellar parameters are error-weighted and calculated.
Paper: Stellar Parameters and Chemical Abundances Estimated from LAMOST-II DR8 MRS Based on Cycle-StarNet
Authors: Rui Wang, A-Li Luo, Shuo Zhang, Yuan-Sen Ting, Teaghan O'Briain
Figure caption: Density distribution Kiel diagram of LAMOST DR8 MRS by CYCLE-STARNET, APOGEE (ASPCAP) DR16, GALAH DR3, and RAVE DR6. The colors indicate the number densities of the spectra in the log scale.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Left: G-band absolute magnitude as a function of ﹩{({G}_{\mathrm{bp}}-{G}_{\mathrm{rp}})}_{0}﹩ color. Right: dereddened (J − K)0 vs. (W1 – W2)0 color–color diagram. Note that all dots are M-giant candidates that were classified through LAMOST spectra. We use different colors to distinguish misidentified stars, which include early-type stars (green), M dwarfs (red) and white dwarf binaries (orange).
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: The M-giant templates from M0 to M6.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: The median of V  ϕ , V  R , and V  Z  for LAMOST M giants, as a function of (R, Z). The bounds of the “main branch”, “north branch”, and “south branch” are labeled by black lines, pink lines, and green lines, respectively. The north branch lies along (R, Z) = (13.5, 1.53), (14.5, 2.81), and (15.5, 4.1) kpc, and is labeled in the left panel by pink crosses. The south branch lies along (R, Z) = (13.5, −1.7), (14.5, −2.625), (15.5, −3.54), and (16.5, −4.46) kpc, and is labeled in the left panel by green crosses. The Monoceros area is labeled by a red square. The dark curves label the boundary of the region with median V  ϕ  > 160 km s−1 shown on the left.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Top-left panel: (J − K)0 vs. M  J  relation for the M-giants samples. The inset histogram shows the scatter around the M  J,fit relationship, which has a dispersion of 0.64 dex. Top-right panel: distance modulus comparison between our new photometric derived relation vs. Gaia EDR3 distance derived by Bailer-Jones et al. (2021). Bottom panel: further distance modulus comparison of the two different methods. The orange dots and error bars represent the median and standard deviation of each bin.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Spatial distribution of our Sgr stars. The arrows show the 3D velocity distribution for Sgr stars in the X–Z plane (right handed). The purple dot marks the location of the Sgr dwarf galaxy (Sgr core). The Galactic center is marked with “GC” and a cyan dot. In the right panel, the gray dots represent Sgr stars from Yang et al. (2019) and the red dots are our data.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Left: metallicity distribution of APOGEE M giants vs. (W1 – W2)0 color. The red line shows the best-fit relationship. Right: the lines correspond to log(age) = 9, 9.5, 10 PARSEC isochrones with mass = 0.6, 0.7, and 0.8 M ⊙, respectively.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Left and median panel: the density map of Gaia DR3 and APOGEE DR17 radial velocities vs. our radial velocities. Right panel: median residuals of the radial velocity as a function of G 0 mag. The error bars represent the 68.3% confidence intervals on the measurements of the medians.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Spectrum examples of C-N and C-H stars in our LAMOST-derived catalog.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: The sky distribution of M-giants sample in equatorial coordinate. The red dots represent our M-giants sample from LAMOST DR9, the blue dots represent the M-giants sample from LAMOST DR5.
Paper: Value-added Catalog of M-giant Stars in LAMOST DR9
Authors: Jing Li, 静 李, Lin Long, 琳 龙, Jing Zhong, 靖 钟, Lin Tang, 琳 唐, Bo Zhang, 博 章, Songmei Qin, 梅 秦松, Yirong Chen, 容 陈易, Zhengzhou Yan, 洲 闫正, Li Chen, 力 陈, Xiang-Xiang Xue, 香 薛香, Jinliang Hou, 良 侯金, Jian-Rong Shi, 施建荣
Figure caption: Galactocentric spatial distribution of the confirmed M giants in LAMOST DR9.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Two-dimensional illustration of the ghost cell interpolation methods using (a) the mass-conservation formula and (b) normal interpolation. Thick lines indicate the boundaries between Blocks. The Block on the top-left corner is on the coarser level, while the other Blocks are on the finer level. Thin solid lines indicate active cells, while thin dotted lines indicate ghost cells. Open/filled circles are active/ghost cells on the coarse level, while open/filled squares are active/ghost cells on the finer level. Open triangles are active cells on the finer level used only for calculating restricted potential. (a) The ghost cell values are calculated so that the area-averaged gradients across the level boundaries match using the mass-conservation formula. (b) The ghost cell values are calculated using the trilinear prolongation and volume-weighted restriction operators. See the text for details.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: An example of a multigrid level hierarchy with mesh refinement in two dimensions. Thick tiles represent Multigrids (associated with MeshBlocks) and Octets, while thin tiles are cells within each Multigrid. (a) Level 0 consisting of 4 × 3 cells. (b) Level 1 with 8 × 6 cells. (c) Level 2 with the first level of Octets. (d) Level 3 with the second refinement level of Octets. (e) Level 4 where each Multigrid is refined to 2 × 2 cells. (f) Level 5 with Multigrids consisting of 4 × 4 cells.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Two-dimensional representations of the interpolation stencils. The coarse grids are shown with solid lines, while the fine grids are shown with dotted lines. The fine and coarse cell indices are marked with small and capital letters, respectively. (a) Restriction: the filled circle is calculated using the volume-weighted average of open squares. (b) Prolongation: the open square is calculated using trilinear (bilinear in two dimensions) interpolation using filled circles. (c) FMG prolongation: the open square is calculated using tricubic (bicubic in two dimensions) interpolation using filled circles and triangles. The sizes of the symbols qualitatively correspond to the weighting coefficients, while circles are positive and triangles are negative.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Schematic graphs of the multigrid algorithms with four levels. (a) The multigrid iteration method with the V(1,1) cycles. (b) The FMG with the V(1,1) cycles. The legends are as follows: filled circles (•): smoothing operations. Filled squares (▪): obtaining the coarsest-grid solution. Downward solid segments: restriction. Upward solid segments: prolongation. Downward dotted line: restriction operation at the beginning of the full multigrid algorithm. Upward double-solid segments: FMG prolongation.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: The convergence behavior for the sinusoidal wave test on uniform grids. (a)–(c) The volume-weighted rms of the errors and defect vs. the number of iterations. The blue lines and orange lines show the results of the FMG and MGI algorithms with various resolutions. The zeroth iteration points for MGI correspond to the initial guess, while the first iteration points for FMG are the results after the first FMG sweep. The black dotted line shows the convergence factor of 0.125. (d) The error compared to the analytic solution vs. the resolution. The black dashed–dotted line shows second-order convergence.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Weak scaling test of the multigrid solvers on uniform grids with different MeshBlock sizes (higher is better). The orange solid lines depict one sweep of FMG. The blue dashed lines show FMG with 10 V-cycle iterations. Red dotted line: MHD with MeshBlocks of 643. The gray dashed–dotted line shows FFT with MeshBlocks of 643. The vertical dotted line corresponds to one full node containing 40 cores. Note that FMG significantly outperforms FFTs, and is only a small fraction of the compute time for MHD.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Same as Figure 5 but for the convergence behavior for the binary potential test with AMR. The errors in panels (a) and (b) are normalized as in Equations (31) and (30).
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: The results of the Jeans wave test at t = 1.5. (a) A stable case with n Jeans = 0.5 using FMG with N iter = 0. (b) An unstable case with n Jeans = 1.1 using fully converged gravitational potential. (c) An unstable case with n Jeans = 1.1 using FMG with N iter = 0. Note that the plotted quantities and ranges of the color bars are different, but in all of the panels, red indicates a density increase and blue denotes density decrease compared to the initial condition. The stripe pattern in panel (a) is not due to the numerical error in the gravity solver but to the loss of significance by subtraction between close values, because the density perturbation is much smaller compared to the background density.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Results of an MHD protostellar collapse simulation with ρ c = 10−8 g cm−3. (a) Poloidal density slice with velocity vectors on large scales. (b) Equatorial density slice with velocity vectors on scales of the pseudo-disk. (c) Poloidal density slice with velocity vectors on scales of the first core. (d) Plasma beta with magnetic field direction vectors on large scales. (e) Radial velocity on large scales. (f) Rotational velocity on large scales. Note the length of velocity vectors in panels (a)–(c) corresponds to different speeds.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: The results of the binary potential test with the root grid resolution of h = 1/64. (a) The density and MeshBlock distribution. (b) The analytic solution. (c) The result obtained with just one sweep of FMG. (d) The defect. (e) The error compared to the analytic solution. (f) The error compared to the fully converged discretized solution. The ranges of the color bars is adjusted to clearly show the distributions, and the maximum values of the errors and defect are shown in the panels.
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: Distribution of the normalized error against the analytic solution of the binary test problem (Equation (31)). (a) The fully converged solution on the AMR grid. (b) The fully converged solution obtained using only the root level. Black lines show the boundaries between MeshBlocks. The range of the color bar in panel (b) is 10 times larger than that in panel (a).
Paper: The Athena++ Adaptive Mesh Refinement Framework: Multigrid Solvers for Self-gravity
Authors: Kengo Tomida, James M. Stone
Figure caption: The strong and weak scaling tests on AMR with FMG and N iter = 3 (higher is better). Blue dashed lines: the strong scaling of the multigrid solver. Orange solid lines show the weak scaling of the multigrid solver. Red dotted lines depict the weak scaling of the MHD solver for comparison. The strong scaling runs with 36 cores and 323 MeshBlocks are not shown because they exceed the memory limit per node.