adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Resolved Stellar Populations Early Release Science Program. V. DOLPHOT Stellar Photometry for NIRCam and NIRISS
Authors: Daniel R. Weisz, Andrew E. Dolphin, Alessandro Savino, Kristen B. W. McQuinn, Max J. B. Newman, Benjamin F. Williams, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Karin M. Sandstrom, Andrew A. Cole, Jack T. Warfield, Evan D. Skillman, Roger E. Cohen, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, Michael C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Leo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Erik J. Tollerud, Andrew Wetzel
Figure caption: Figures output by WebbPSF that show variations in the telescope alignment, wave front, and encircled energy as a function of time over the period. At select epochs, we compute the effects of small, large, and no perturbations to the telescope stability on DOLPHOT photometry.
Paper: Metallicities and Refined Stellar Parameters for 52 Cool Dwarfs with Transiting Planets and Planet Candidates
Authors: Rebecca Gore, Steven Giacalone, Courtney D. Dressing, Emma V. Turtelboom, Ashley Schroeder, Charles D. Fortenbach, Kevin K. Hardegree-Ullman, Jon K. Zink, Andrew W. Mayo, Joshua E. Schlieder, Jessie L. Christiansen
Figure caption: The observed spectrum for EPIC 212048748 compared with the IRTF standard spectrum (offset vertically for visual clarity) of HD 36395 (M1.5V; top) Gl 381 (M2.5V; middle), Gl 273 (M3.5V; bottom) within the highlighted J, H, and K bands. The bottom panels display the residuals between the observed and standard spectra, with Gl 381 providing the best match to the data. Data strongly influenced by telluric contamination has been masked out.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Comparison between M tot, R  e , and μ  e  of UDGs (dark blue) and non-UDG cluster members (light blue) from our A1656 sample, as well as galaxies from the reference field analyzed for A1656 (brown). Galaxies with a counterpart in Yagi et al. (2016) are depicted in red. The M tot−μ  e  cutoff is indicated by the black line. The basis for this plot is Figure 37 in Kormendy et al. (2009) with updates in Figure 2 in Kormendy & Bender (2012), Figure 14 in Bender et al. (2015), and Figure 16 in Kluge et al. (2020) including BCGs (orange), ellipticals (green), classical bulges (green), and spheroidals (gray).
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Comparison between M tot, R  e , and μ  e  of UDGs (dark blue) and non-UDG cluster members (light blue) from our A262 sample, as well as galaxies from the reference field analyzed for A262 (brown). The M tot−μ  e  cutoff is indicated by the black line. The basis for this plot is Figure 37 in Kormendy et al. (2009) with updates in Figure 2 in Kormendy & Bender (2012), Figure 14 in Bender et al. (2015), and Figure 16 in Kluge et al. (2020) including BCGs (orange), ellipticals (green), classical bulges (green), and spheroidals (gray).
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Correlations between M tot and μ 0 for UDGs (dark blue) and non-UDGs (light blue) in A1656 (top) and A262 (bottom), as well as galaxies from the reference field analyzed for the respective cluster (brown). Galaxies with a counterpart in Yagi et al. (2016) are depicted in red. The basis for this plot is Figure 3 in Kormendy (1985) with updates in Figure 1 in Binggeli (1994) and in Figure 1 in Kormendy et al. (2009). For elliptical and cD galaxies, μ 0 corresponds to the highest surface brightness resolved by HST.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Axis ratio distribution of all UDGs (red) and non-UDGs (blue), as well as of all galaxies from the reference field (black) and all galaxies rejected by the M tot−μ  e  cutoff (orange). The number of objects is given in brackets. The median axis ratio of each distribution is depicted as a vertical dotted line.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption:                       ﹩u^{\prime} -g^{\prime} ﹩ vs. ﹩g^{\prime} -r^{\prime} ﹩ color–color diagrams for A1656. Red points represent the 14 galaxies with a spiral morphology in the HST observations, blue points represent our final A1656 galaxy sample, and black points represent all galaxies that were rejected by the bicolor and red sequence selection.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: HST color images of galaxies rejected from our sample by the M tot−μ  e  selection cutoff with a spiral morphology covered by HST archival images.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: HST color images of galaxies in our final sample with a spiral morphology covered by HST archival images.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Total V-band magnitude vs. Sérsic index n of UDGs (dark blue) and non-UDGs (light blue) in our sample, as well as ellipticals, S0 bulges, and (bright) spheroidals from Kormendy et al. (2009; green). Uncertainties are only shown for UDGs for better clarity.
Paper: Ultradiffuse Galaxies—A Distinct Population? Dwarf Galaxies in the Coma Cluster and A262 from Deep u′–g′–r′ Wendelstein Imaging Data
Authors: Raphael Zöller, Matthias Kluge, Benjamin Staiger, Ralf Bender
Figure caption: Comparison between WWFI ﹩g^{\prime} ﹩ band (left) and HST F475W (right) data of selected UDGs.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: The left panels display the relationship between the errors of different atmospheric parameters and S/N in the r band, where red dots represent the median values within each region with a bin of 10. The red dashed line in this panel indicates S/N = 80. The right panels show the relationship between the errors of different atmospheric parameters and S/N for three different temperature ranges in small boxes, where the points in the right panel are the median values of each bin and different colors represent the different temperature regions.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: Spectral subtraction results of J045614.62+101506.9 with resolutions of 1800 and 250. From top to bottom, these are the Hα, Ca II H and K, and Ca II IRT lines.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: The left panel shows the statistical results of spectral subtypes for the sample. The number above each bin indicates the number of corresponding spectral subtypes. The right panel shows the statistical results of the sample atmospheric parameters and their errors. The parameters for both panels come from data provided by LAMOST DR10.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: Comparison of stellar parameters T eff (left panel), ﹩\mathrm{log}g﹩ (middle panel), and RV (right panel) between the LAMOST DR10 and Gaia DR3 data sets. The color bars of each panel represent the number density, where the density increases as the color changes from blue to red. The black line in each subplot represents x = y.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: H-R diagram of the sample stars. The top panel is the color–magnitude diagram of our samples, where the color bar represents the number density. The lower left panel shows the position of each star on the H-R diagram, where the color bar represents the value of [Fe/H]. The lower right panel shows the distribution of the sample density on an H-R diagram, where the color bar represents the count density.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: The left panels show the S/N distributions for G-type stars in the ugriz bands from 10 to 100 in intervals of 10. The right panels show the S/N distributions in the ugriz bands from 100 to 800 in intervals of 100.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: The left panel displays the distribution of data with S/N r above 10 in LAMOST DR10 G-type stars. The right panel displays their spatial distributions in the Galaxy.
Paper: Magnetic Activity of Millions of G-type Stars Based on the LAMOST DR10 Low-resolution Spectral and TESS Light-curve Surveys and the Future CSST Survey
Authors: Tianhao Su, Li-yun Zhang, Liu Long, Prabhakar Misra, Xianming L. Han, Gang Meng, ZiLu Yang, Qingfeng Pi
Figure caption: The fraction of active G-type stars in different spectral subtypes.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: Distribution of orbital periods (period), temperature (T  p , T  s ), temperature ratio (T  s /T  p ), orbital inclination (i ncl), fill-out factor (f), mass ratio (q), and relative radius (R  p , R  s ) for the 11,111 ASAS-SN short-period CBs. The period distribution has a peak of around 0.35 days. The temperature distribution of primary and secondary stars peaks at approximately 5750 K (the red short dashed lines) and 6000 K (the green short dashed lines), respectively. The orange short dashed lines represent a temperature ratio of 1, the left side represents the A-type CBs, and the right side represents the W-type CBs. The distributions of the orbital period, temperature (T  p , T  s ), temperature ratio (T  s /T  p ), inclination (incl), and relative radius (R  p , R  s ) roughly obey normal distributions (the blue solid line), the distributions of the mass ratio (q) and the fill-out factor (f) obey log-normal distributions (the red solid line).
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: The 2D kernel density graph between the mass ratio and fill-out factor of ASAS-SN short-period CBs. The red horizontal short dashed lines and vertical short dashed lines represent a fill-out factor of 0.5 and a mass ratio of 0.25, respectively. The green solid line indicates the trend between mass ratio (q) and fill-out factor (f). There are very few samples in the upper right region; thus, CBs with a deep fill-out factor and high-mass ratio are more worthy of attention and study.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: The blue dots represent the phased ASAS-SN light curves. Using the NNs and MCMC algorithm model to obtain the posterior distribution of the parameters as the input parameters. The red line represents the light curves generated by the NN model with the input parameters. The green X line and symbol represent the light curves generated by Phoebe using the same input parameters. Top row: two example targets used the non-third-light model to get the parameters. Bottom row: two example targets used the third-light model to get the parameters, and the luminosity ratios of the third light are about 68% and 27%, respectively.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: The 2D kernel density graph between the orbital period and the temperature ratio. The green short dashed lines represent the temperature ratio as 1. The upper and lower parts of the short dashed lines represent the W-type and the A-type CBs, respectively.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: The 2D kernel density graph between the orbital period and the temperature of the primary stars. It shows a clear correlation between the orbital period and the temperature of short-period CBs (usually the late-type CBs), the longer the period, the higher the temperature.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: The 2D kernel density graph between the orbital period and the temperature, mass ratio, orbital inclination, and fill-out factor. There are no certain correlations between orbital period with mass ratio, orbital inclination, and fill-out factor.
Paper: Physical Parameters of 11,100 Short-period ASAS-SN Eclipsing Contact Binaries
Authors: Xu-Zhi Li, 旭志 李, Qing-Feng Zhu, 青峰 朱, Xu Ding, 旭 丁, Xiao-Hui Xu, 小慧 徐, Hang Zheng, 航 郑, Jin-Sheng Qiu, 锦盛 邱, Ming-Chao Liu, 明超 刘
Figure caption: Projected distribution of the 11,145 short-period ASAS-SN contact binaries in equatorial coordinates (Hammer projection). The points are colored by period. The red line indicates the Galactic plane.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Comparisons between typical predicted errors (y-axis) from the UaRA-net and 1σ uncertainties of the relative residuals (x-axis) for the training set in T eff bins with S/N ∈{20, 40}. To avoid crowding, five representative wavelengths at 3205, 3429, 4252, 7206, and 9207 Å are plotted.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: The medians (left column) and 1σ uncertainties (right column) of relative residuals of the training set with S/N ∈{20, 40} for different T eff bins. The relative residuals are defined in Equation (2).
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: (a) A subunit of the proposed network, where C, W, and 1 in C*W*1 are the indicators of the number of channels, width, and height of the feature map, respectively. (b) Overall architecture of the proposed network.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Similar to Figure 4, but for the testing set with S/N ∈{20, 40, 80}. It is worth mentioning that the spectra with S/N = 80 are not in the training set.
Paper: A Star-based Method for the Precise Flux Calibration of the Chinese Space Station Telescope Slitless Spectroscopic Survey
Authors: Lin Yang, Haibo Yuan, Fuqing Duan, Ruoyi Zhang, Bowen Huang, Kai Xiao, Shuai Xu, Jinming Zhang
Figure caption: Similar to Figure 2, but for the testing set with S/N ∈{20, 40, 80}. It is worth mentioning that the spectra with S/N = 80 are not in the training set.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: Angle-averaged 1D profiles (initial conditions) for the models b18.3-high (top) and n16.3-high (bottom). Mass fractions of species as a function of the radius (left) and the density, temperature, and radial velocity as a function of radius (right). The ages are 19.0 and 22.3 hr after the explosion for the former and latter models, respectively.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: The gas temperatures of Lagrange meshes as a function of time after the explosion. The values are obtained from the 1D radiation hydrodynamical calculation results with the angle-averaged 1D profiles based on the 3D hydrodynamical model (the model b18.3-high; Ono et al. 2020). Each line shows the time evolution for each Lagrange mesh. The colors denote the corresponding initial positions (radii). The two straight lines represent the power-law evolutions with the powers of −1 and −2 corresponding to γ ad = 4/3, and γ ad = 5/3, respectively.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: The photospheric temperatures (left) and the radial velocities at the photospheres (right) as a function of time after the explosion for the U, B, V, R, and I bands calculated by a 1D radiation hydrodynamical code with the angle-averaged 1D profiles based on the 3D hydrodynamical model (the model b18.3-high; Ono et al. 2020) as the initial condition. Arithmetic averages (mean) and arbitrary extrapolations (extend; see the text) are also plotted.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: 1D calculation results with the angle-averaged profiles for the model b18.3-high (Ono et al. 2020) with the parameters, f h = 10−2, f d = 1.0, and t s = 500 days (top panels), and f h = 5 × 10−3, f d = 1.0, and t s = 500 days (bottom panels, corresponding to the model b18.3-mean). Left panels: time evolution of the total amounts of CO and SiO and the seed atoms, carbon, oxygen, and silicon, compared with the estimations (including theoretical calculations) for CO and SiO in previous studies, LD92 (Liu et al. 1992), LD94 (Liu & Dalgarno 1994), LD95 (Liu & Dalgarno 1995), ALMA (Matsuura et al. 2017), and L+20 (Liljegren et al. 2020). Right panels: time evolution of the fluxes for CO vibrational bands, Δv = 1 (fundamental), Δv = 2 (first overtone), …, Δv = 6, compared with the observed light curves for Δv = 1 (BD93; W+93; Bouchet & Danziger 1993; Wooden et al. 1993, respectively), and Δv = 2 (M+89, 93; BD93; Meikle et al. 1989, 1993; Bouchet & Danziger 1993, respectively).
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: 1D calculation results of the models, b18.3-mean (top panels), b18.3-sphel (middle panels), and b18.3-sphel-pure (bottom panels). Left panels: the time evolution of the amounts of diatomic molecules and several seed atoms compared with the estimation for CO and SiO (points) in the previous studies (for the details, see the caption of Figure 14). Right panels: time evolution of the gas temperatures of the tracer particles; the colors denote the initial positions of the particles. As a reference, power-law evolutions of the powers of −1 and −2 are shown.
Paper: The Impact of Effective Matter Mixing Based on Three-dimensional Hydrodynamical Models on the Molecule Formation in the Ejecta of SN 1987A
Authors: Masaomi Ono, Takaya Nozawa, Shigehiro Nagataki, Alexandra Kozyreva, Salvatore Orlando, Marco Miceli, Ke-Jung Chen
Figure caption: 1D calculation results with the angle-averaged profiles for the model b18.3-high (Ono et al. 2020) with the parameters, f h = 10−2, f d = 1.0, and t s = 500 days. Left (right) panel: time evolution of the gas temperatures (gas densities) of the tracer particles; the colors denote the initial positions of the particles. As a reference, power-law evolutions of the powers of −1, −2 (left), and −3 (right) are also shown.