adsabs/AstroCLIMB huggingface dataset:
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: An example for a star where we measure a confident P rot, EPIC 211033487. Left: light curve for this star. Middle: Lomb–Scargle periodogram; the red dashed line is white noise, which is calculated by the rms of powers. Right: phase-folded light curve using the P rot.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: CMDs of NGC 1817, NGC 6774, NGC 6819, and M67. Black filled circles are cluster members with P ≥ 0.9. Blue circles are BSS candidates. The red solid line and red dotted line represent the PARSEC isochrones and binary sequences, respectively. The gray solid line is the red limit by the MSTO color and the binary sequence as the red boundary. The black dashed line is ZAMS as the blue limit.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: CMDs and isochrone fittings of 16 OCs. The black dots are the members with P > 0.9.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Distribution of BFs for 16 clusters. The clusters are arranged in increasing order of age. The black dots are BFs obtained in this work, and gray rectangles indicate the range of BFs obtained by previously published work. The subplot is the BF of systems as a function of logarithmic age. The red dashed line is the result of Donada et al. (2023).
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Comparison of our cluster parameters with literature reference values from Cantat-Gaudin et al. (2020). The black dashed line is the 1:1 line.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Positions in α and δ, VPDs, CMDs, and ϖ as a function of G mag for the cluster M67. In all four panels, the field stars are given by gray dots, and cluster stars are given by the circles with gradient colors. The color bar presents membership probability.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: The longitude–latitude maps of MHD variables in the simulation with α = 1.2. (a) The fixed B  r  on the inner boundary sphere at 2.5 R ⊙. (b) The number density at 2.5 R ⊙ given as the initial value. (c) The number density at 2.5 R ⊙ in the quasi-steady state. (d) The radial component of the magnetic field, B  r , at the outer boundary sphere at 19.0 R ⊙, in the quasi-steady state. (e) The fixed V  r  on the inner boundary sphere at 2.5 R ⊙. (f) The plasma temperature at 2.5 R ⊙ given as the initial value. (g) The plasma temperature at 2.5 R ⊙ in the quasi-steady state. (h) The radial component of plasma velocity, V  r , at the outer boundary sphere at 19.0 R ⊙, in the quasi-steady state.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: The radial profiles of the radial component of plasma speed V  r  in time-relaxed states with various values of the boundary-polytrope index, α = 1.0, 1.2, 1.4, 5/3, 3.0, and 100.0. The asterisks (*) placed to the left of the values of α > 5/3 are to remind readers that α is a parameter regulating the behavior of the boundary treatment and does not have implications for physical processes in the lower solar corona. From top to bottom, the profiles from the simulations for (a) CR 2126, (b) CR 2059, and (c) CR 2095 are shown. The radial profiles are sampled at the latitude of 0° (the solar equator) and the Carrington longitude of 180°.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: Comparisons of the radial profiles of the radial component of plasma speed V  r  for CR 2126, derived with simulations with different values of the specific heat ratio (γ = 1.01, 1.1, 1.2, 1.3, 1.46, and 5/3) in the MHD equations. The case with γ = 1.01 corresponds to the near-isothermal case. The value of 1.46 is the one inferred from the Helios data analysis (Totten et al. 1995). The boundary values of V  r  at 2.5 R ⊙ are fixed and identical among these cases. The radial profiles are sampled at the latitude of 0° (the solar equator) and the Carrington longitude of 180°.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: The simulated boundary density (left) and temperature (right) in the relaxed state with various values of the boundary-polytrope index (α = 1.0, 1.2, and 5/3) and 100.0. The boundary number density is nearly fixed all through the simulation with α = 100.0 (d), and the boundary temperature is fixed with α = 1.0 (e). Notice that in each column, the overall shapes well resemble each other, but the values are substantially different. A smaller (greater) value of α yields higher (lower) boundary plasma density and lower (higher) boundary plasma temperature.
Paper: Boundary Treatment for the Subsonic/Alfvénic Inner Boundary at 2.5 R ⊙ in a Time-dependent 3D Magnetohydrodynamics Solar Wind Simulation Model
Authors: Keiji Hayashi, Chin-Chun Wu, Kan Liou
Figure caption: Comparison of the radial profiles of the radial component of plasma speed V  r  derived from (a) the standard reference case, (b) the case without the characteristics-based boundary treatment, and (c) the case without the characteristics-based boundary treatment, but with higher boundary temperature. The radial profiles are sampled at the latitude of 22.°5 south and the Carrington longitude of 180°.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The observed NOMAD UVIS spectrum compared to the computed bidirectional reflectance spectra using the 20–40 μm narrow size distribution and the previously derived k (GRS2) of the three Martian dust analogs.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: In the left panel, we present the NOMAD UVIS spectrum and the computed bidirectional reflectance spectra for the MMS-2 analog using power-law size distributions with power-law indices 1.0 and 1.5 in the range of 2–40 μm. Furthermore, we present the bidirectional reflectance spectrum computed by using the optical constants of Wolff et al. (2009) and a power-law size distribution with index 3.0. The right panel shows the number distributions.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Comparison of age and mass estimates for ∼15,000 LAMOST stars using our α EM models and the YY (Yi et al. 2008) stellar isochrones with input [α/Fe] = 0.1 dex. The red line represents the 1:1 line. Dispersion of the relative age and mass difference are marked in the figure.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Comparison of masses and ages of ∼4000 GALAH sample stars from our α EM models, OEM models, and the GALAH DR3 VAC (Buder et al. 2021). The red line represents the 1:1 line. Dispersion of the relative age and mass difference is marked in the figure.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Likelihood distributions of mass and age for two example stars from GALAH. The red solid line represents the Gaussian function that fits to the likelihood distribution. Solid and dashed vertical lines indicate the mean and standard deviation of the Gaussian profile. The fundamental parameters and chemical abundance for these stars are shown in Table 5.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Color-coded stellar number density distribution of the sample stars from LAMOST (a) and GALAH (b) in the age–[O/Fe] plane, based on the ages from α EM models. The black solid lines represent the fitting for age–abundance relations by local nonparametric regression.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Color-coded stellar number density distribution of the sample stars from LAMOST in the age–[Fe/H] (a) and age–[O/Fe] (b) plane. The black solid lines represent the fitting for age–abundance relations by local nonparametric regression.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Distribution of fractional age difference as a function of [Fe/H] for sample stars from LAMOST (a) and GALAH (b), color-coded by [O/α]. The overplotted solid lines represent the median and standard deviation of fractional age difference for fake stars in each [Fe/H] bin, with a bin size of 0.1 dex.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Comparison of the ages determined with α EM and OEM models for mock stars, color-coded by age uncertainty. These stars are divided by their [Fe/H] and [O/α] values. Black dashed lines show the agonic line.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Color-coded stellar number density distribution of the sample stars from GALAH in the age–[Fe/H] (a) and age–[O/Fe] (b) planes. The symbols are the same as those defined in Figure 9.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Panel (a) shows the color-coded stellar number density distributions of mock stars on the H-R diagram. Panels (b)–(c) show the comparison of T eff and [Fe/H] distributions between mock data and observational data.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: X-ray diffraction analyses of the MMS-2 analog: (a) dust as received, (b) 20–40 μm fraction (previously milled dust) and (c) 20–40 μm fraction (not milled dust); this last one showing an increased proportion of a quartz phase (black circles). 2θ corresponds to the spacing between the crystals or atoms in the samples, determined by the angle of diffraction from the incident X-ray beam sent into the sample.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The derived imaginary parts of the refractive indices using GRS1 shapes and the smoothed-out diffuse reflectance spectra for the JSC Mars-1 (top), MMS-2 (middle), and MGS-1 (bottom) analogs.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: An illustration of the model for retrieving refractive indices. (1) Geometric optics is used to compute single-scattering properties of individual particle sizes, (2) the obtained single-scattering properties are averaged over the measured size distribution, (3) the regolith is simulated by using the averaged particles as diffuse scatterers in a vacuum.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The measured reflectance of the MMS-2 sample compared to the computed spectra using the GRS1 shapes with the retrieved k MMS2 (GRS2) and the GRS2 shapes with the k MMS2 (GRS1).
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: Projected surface area distributions (left) and number distributions (right) of the JSC Mars-1, the MMS-2, and the MGS-1 20–40 μm size fractions.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The shapes used in the sensitivity study. From left to right: sphere, GRS1, polyhedron, and GRS2.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The derived k values of the JSC Mars-1, MMS-2, and MGS-1 samples using GRS1 and GRS2 shapes.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: The diffuse reflectance spectra of the JSC Mars-1, MMS-2, and MGS-1 analogs.
Paper: Optical Constants of Martian Dust Analogs at UV–Visible–Near-infrared Wavelengths
Authors: Julia Martikainen, Olga Muñoz, Teresa Jardiel, Juan Carlos Gómez Martín, Marco Peiteado, Yannick Willame, Antti Penttilä, Karri Muinonen, Gerhard Wurm, Tim Becker
Figure caption: GRS1 particles used in the model (right) compared to the MMS-2 FESEM image (left).
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: (a) The data observed by the Learmonth solar radio system. (b) The data observed by the 6–15 GHz solar radio observation system.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: The vector-point diagram (VPD) of M67. The gray points are all sources of M67. The sources inside the red circle are sample sources of M67.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: The correlation of errors (photometry, parallax, and proper motions) with the magnitude of G. The gray points are all Gaia DR3 for M67 within a radius of 10° from the cluster center. The sources in blue are those with G err ≤ 0.005 mag.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Data processing flow of the digital receiver.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Solar radio bursts observed by the observation system of the left and right rotations.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: The display change process of the observation system from pointing toward the sky to pointing toward the Sun.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Distribution of the membership probabilities for the sample sources in the M67 field.
Paper: A New 6–15 GHz Solar Radio Observation System
Authors: Lei Zhang, 磊 张, Yanrui Su, 艳蕊 苏, Zhao Wu, 昭 武, Shuwang Chang, 树旺 常, Yao Chen, 耀 陈, Fabao Yan, 发宝 严
Figure caption: Dynamic spectrum of solar radio bursts used for calibrating data.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Stellar evolution tracks of two example stars calculated with αEM (black) and OEM (red) models. Panel (a) shows the tracks of a star with [α/Fe] ∼0.1 and [O/Fe] ∼0.5 (LAMOST SPECID: 20140313-HD145243N315530B-01-084); panel (b) shows the tracks of a star with [α/Fe] ∼0.2 and [O/Fe] ∼0 (LAMOST SPECID: 20141112-HD083415N451147V01-03-165). At fixed mass and metal mixture (fixed color and line type), the input [Fe/H] values of tracks (from left to right) are shown. The blue dots and error bars are the observed values and uncertainties of example stars, while the blue squares represent the observational error box. The atmosphere parameters and chemical abundance for these stars are shown in Table 4.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Stellar evolution tracks of fixed mass (M = 0.6, 0.7, 0.8, 0.9, 1.0, 1.1, 1.2 M ⊙) computed with αEM and OEM models. In each panel, the [Fe/H] range is 0, −0.2, −0.4, −0.6, −0.8, and −1.0 (from right to left). The solid lines and dashed lines represent the tracks with input [O/Fe] = 0.1 and 0.5, respectively. All tracks have the same input [α/Fe] (0.1 dex) values. The Z values of each track are presented in Table 3.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: Comparisons between the P rot data for benchmark populations with the Amard et al. (2019) model (a) and Spada & Lanzafame (2020) model (b). The ages corresponding to the solid lines in panels (a) and (b) are 120 Myr, 700 Myr, 1 Gyr, 2.5 Gyr, and 4 Gyr from bottom to top. Clusters excluded from benchmark populations either have little P rot data or are too young to show color–period relations.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption:  P rot versus ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ of clusters with ages older than Praesepe. Solid lines are fits to the data.
Paper: Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Liu Long, Shaolan Bi, Jinghua Zhang, Xianfei Zhang, Liyun Zhang, Zhishuai Ge, Tanda Li, Xunzhou Chen, YaGuang Li, LiFei Ye, TianCheng Sun, JianZhao Zhou
Figure caption: The color–period diagrams for 16 OCs. Black dots are MS single stars and gray diamonds are binary candidates.
Paper: Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
Authors: Tiancheng Sun, Zhishuai Ge, Xunzhou Chen, Shaolan Bi, Tanda Li, Xianfei Zhang, Yaguang Li, Yaqian Wu, Sarah A. Bird, J. W. Ferguson, Jianzhao Zhou, Lifei Ye, Liu Long, Jinghua Zhang
Figure caption: Color-coded stellar number density distributions of the targets from LAMOST (left column) and GALAH (right column) in the Kiel diagram ((a)–(b)) and the [α/Fe]–[O/Fe] space ((c)–(d)). The red dashed lines in panels (c)–(d) indicate the 1:1 relation. The gold pentagrams represent the input metal mixtures (shown in Table 2) of the stellar model grid.