adsabs/AstroCLIMB huggingface dataset:
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Vertical profiles of the mean radiative intensity J (black) and energy flux (green; positive shown with dotted) for the FidH+ run (left) and Static model (right), where negative values are shown with dotted lines. The radiative intensities in the upward (δ → ∞; I+; red) and downward (δ → −∞; I−; blue) directions are shown. Small arrows depict the direction of each radiative variable.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: 2D distributions of the density (top panels) and temperature (bottom panels) for κirr = 10 cm2 g−1 at t = 365 yr: OpNoH (left), OpH+ (middle), and OpH− (right). The lines are the same as in panels (a) and (e) of Figure 1. Note that the irradiation front is shown with cyan dotted–dashed lines. The upper wind region is mainly displayed.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Temperature distribution normalized by (R/au)−0.5 at t = 365 yr in the FidH− model, with the x-axis being the logarithmic radius and the y-axis being δ. We plot the surfaces where optical depth equals unity (τr,xuv = 1, purple dotted line; τr,irr = 1, blue dotted–dashed line; τθ,disk = 1, red dashed line) and isodensity contours at levels {10−4, 10−3, 10−2, 10−1, 0.3, 0.7} from the midplane.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Same as Figure 1, but for FidH+.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Same as Figure 1, but for FidH−.
Paper: PSR J1838−0655: X-Ray Observations with NICER and NuSTAR
Authors: Xian-Ao Wang, Han-Long Peng, Jin-Tao Zheng, Shi-Qi Zhou, Wen-Tao Ye, Ming-Yu Ge, Xiang-Hua Li, Shi-Jie Zheng
Figure caption: Pulse profiles observed by NICER and NuSTAR are presented. For NICER, the profiles were derived by stacking observations spanning MJD 58250 to 60630. Panel (a) shows the 0.5–3 keV profile, and Panel (b) shows the 3–10 keV profile. For NuSTAR, the profiles were obtained by combining two distinct observations and merging data from the FPMA and FPMB detectors. Panel (c) presents the 3–10 keV profile, and Panel (d) shows the 10–79 keV profile. All profiles are divided into 25 phase bins, with two full cycles plotted for each.
Paper: PSR J1838−0655: X-Ray Observations with NICER and NuSTAR
Authors: Xian-Ao Wang, Han-Long Peng, Jin-Tao Zheng, Shi-Qi Zhou, Wen-Tao Ye, Ming-Yu Ge, Xiang-Hua Li, Shi-Jie Zheng
Figure caption: Step timing analysis of PSR J1838−0655 using NICER data. Panel (a): the best-fit timing residuals during MJD 58250–60630. Panel (b): frequency residuals after subtracting the preglitch timing model. Panel (c): the evolution of ﹩\dot{\nu }﹩. The glitch epoch at MJD 59300.00(2) is indicated by the black dashed line.
Paper: PSR J1838−0655: X-Ray Observations with NICER and NuSTAR
Authors: Xian-Ao Wang, Han-Long Peng, Jin-Tao Zheng, Shi-Qi Zhou, Wen-Tao Ye, Ming-Yu Ge, Xiang-Hua Li, Shi-Jie Zheng
Figure caption: The unfolded spectra observed by NuSTAR, Chandra, and NICER. The top panel shows the joint spectral fit of Chandra, NuSTAR, and NICER data, while the bottom panel presents the residuals. The red crosses represent the Chandra spectrum in the 2–10 keV band, the black and green crosses correspond to the NuSTAR FPMA and FPMB spectra in the 3–79 keV, and the blue crosses correspond to the NICER spectra in the 1.3–9 keV, respectively. The solid lines represent the best-fit model curves for each instrument.
Paper: PSR J1838−0655: X-Ray Observations with NICER and NuSTAR
Authors: Xian-Ao Wang, Han-Long Peng, Jin-Tao Zheng, Shi-Qi Zhou, Wen-Tao Ye, Ming-Yu Ge, Xiang-Hua Li, Shi-Jie Zheng
Figure caption: Phase-resolved spectral analysis of PSR J1838−0655. The black pulse profile represents the combined result of the two NuSTAR observations, stacking both FPMA and FPMB data, folded using the ephemeris of the first NICER segment in the 3–79 keV. The profile is divided into 25 phase bins. The black triangles and gray squares represent the photon indices obtained with the background estimated from a 0.1-phase-wide off-pulse region and a 60″–120″ annulus in 10 phase bins, respectively.
Paper: PSR J1838−0655: X-Ray Observations with NICER and NuSTAR
Authors: Xian-Ao Wang, Han-Long Peng, Jin-Tao Zheng, Shi-Qi Zhou, Wen-Tao Ye, Ming-Yu Ge, Xiang-Hua Li, Shi-Jie Zheng
Figure caption: The horizontal axis is defined relative to the glitch epoch (MJD 59300), with zero corresponding to the glitch time. Shows the observed changes in the spin-down rate relative to the preglitch value (black points) and the predicted evolution from the best-fit vortex creep model (solid red line).
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: The acceleration experienced by the star in the FID-anti and FID-fric models. The blue, red, and orange lines represent the acceleration components in the x-, y-, and z-directions, respectively. Solid and dashed lines correspond to the FID-anti model, while the dotted lines represent the FID-fric model. The gray and black dashed–dotted lines represent the GAMMA-anti and MASS-anti models. The solid lines depict the instantaneous acceleration, whereas the other lines indicate the mean values over 15 orbital periods.
Paper: MC-BLOS: Automated Software for Determining the Line-of-sight Component of Magnetic Fields Associated with Molecular Clouds 
Authors: Mehrnoosh Tahani, John Ming Ngo, Jennifer Glover, Ryan Clairmont, Gabriel M. Zarazua, René Plume
Figure caption: Final BLOS maps of the Perseus molecular clouds using the NearExt5 parameter set, positioning the reference point (green circles) further from the cloud (i.e., high-extinction regions) by increasing the high-extinction threshold multiplier from 2 to 5. The background color image shows extinction, and the circles represent BLOS strengths (without uncertainties). Red (blue) circles indicate magnetic fields pointing away from (toward) the observer, without displaying associated uncertainties. This parameter set demonstrates how reference points can be positioned at greater distances from the cloud while still producing BLOS results consistent with those from other parameter sets (see bottom right panel of Figure 6).
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: The mass accretion rate per area at x = −Lx. The red and blue lines correspond to the FID-anti and FID-fric models, respectively. The solid lines depict the instantaneous ﹩{\dot{m}}_{{\rm{area}}}﹩, while the dashed lines represent the mean values averaged over 15 orbital periods.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Gas density ρ in the z = 0 plane (i.e., the orbital plane; left column) and the x = 0 plane (right column) at the tevo = 15 P snapshot of the fiducial model. The star is located at the origin, with color indicating gas density and black velocity streamlines representing the gas flow pattern. The white dashed circle indicates the characteristic standoff distance, ﹩{R}_{0}\approx {[\dot{m}{v}_{{\rm{src}}}/(4\pi {\rho }_{0}\Vert {{\boldsymbol{v}}}_{{\rm{g}}}|{|}^{2})]}^{1/2}﹩, where the total pressure of the outflow balances that of the incoming ambient medium (A. Gruzinov et al. 2020; X. Li et al. 2020).
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Gas density ρ in the z = 0 plane (i.e., the orbital plane) at tevo = 15 P for the PG-45 (left panel) and PG-0 (right panel) models. The white dashed circle indicates the characteristic standoff distance R0.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 1 but for the star without outflow in the fiducial model. The white dashed circle indicates the Bondi radius, ﹩{R}_{{\rm{B}}}=2Gm/({c}_{{\rm{iso}}}^{2}+\Vert {{\boldsymbol{v}}}_{{\rm{g}}}|{|}^{2})﹩.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: The acceleration experienced by the star in the PG-45 (upper panel) and PG-0 (lower panel) models. Both models include scenarios with and without stellar outflows.
Paper: Active Galactic Nucleus Star Dynamics Under the Influence of Outflow–Ambient Interactions
Authors: Muxin Liu, Lile Wang, Peng Peng
Figure caption: Similar to Figure 1 but for the MASS-anti model.
Paper: Simultaneous Ion Arrival Times during the Rise Phase of 3He-rich Solar Energetic Particle Events
Authors: G. M. Mason, A. Kouloumvakos, G. C. Ho, R. C. Allen, R. Gómez-Herrero, I. Cernuda, R. F. Wimmer-Schweingruber, J. Rodríguez-Pacheco
Figure caption: (a) Differential energy spectra for the SEP event starting 2022 November 14 (event 4 in Table 1). The yellow box shows the energy interval used for timing analysis, which is the lowest interval covered by all species. (b) The ion arrival times for mass 3 and heavier vs. 1/v (hr/au). The yellow box shows same energy interval for analysis. The solid blue line shows the estimated location of particle dispersion line, and the dashed line is offset by 15 minutes to show nominal uncertainty.
Paper: Simultaneous Ion Arrival Times during the Rise Phase of 3He-rich Solar Energetic Particle Events
Authors: G. M. Mason, A. Kouloumvakos, G. C. Ho, R. C. Allen, R. Gómez-Herrero, I. Cernuda, R. F. Wimmer-Schweingruber, J. Rodríguez-Pacheco
Figure caption: 3He-rich SEP event starting 2022 November 14 (event 4 in Table 1). (a) SIS-a 15 minute average time–intensity profiles of H, 3He, 4He, O, and Fe ions of 0.226–0.320 MeV nucleon−1. (b) red line: SIS-a/b (sunward/antisunward) telescope intensity ratios for 3He (30 minute average); dashed black line: SIS-a pitch angle (degrees). The yellow shaded area shows the time interval during the rise phase used to calculate average arrival times.
Paper: Simultaneous Ion Arrival Times during the Rise Phase of 3He-rich Solar Energetic Particle Events
Authors: G. M. Mason, A. Kouloumvakos, G. C. Ho, R. C. Allen, R. Gómez-Herrero, I. Cernuda, R. F. Wimmer-Schweingruber, J. Rodríguez-Pacheco
Figure caption: Mean arrival times of 0.226–0.320 MeV nucleon−1 ions for each event in Table 1. The purple line at the bottom shows scatter-free flight time as a function of radius; numbers on flight time points correspond to event numbers in Table 1. (a) Heavy ion arrival times compared to O. The thick pink line is for all species C–Fe, except O. (b) Ion arrival times compared to 4He. C–Fe points include O.
Paper: Simultaneous Ion Arrival Times during the Rise Phase of 3He-rich Solar Energetic Particle Events
Authors: G. M. Mason, A. Kouloumvakos, G. C. Ho, R. C. Allen, R. Gómez-Herrero, I. Cernuda, R. F. Wimmer-Schweingruber, J. Rodríguez-Pacheco
Figure caption: Histograms of 0.226–0.320 MeV nucleon−1 ions summed over all events in Table 1. (a) 3He–4He mass range; (b) mass 10–100 amu. Labeled peaks correspond to species used in timing analysis.
Paper: Simultaneous Ion Arrival Times during the Rise Phase of 3He-rich Solar Energetic Particle Events
Authors: G. M. Mason, A. Kouloumvakos, G. C. Ho, R. C. Allen, R. Gómez-Herrero, I. Cernuda, R. F. Wimmer-Schweingruber, J. Rodríguez-Pacheco
Figure caption: Heavy ion abundance ratios for 0.226–0.320 MeV nucleon−1 ions for each event in Table 1. The dashed purple line is the average from the survey of 34 3He-rich events by G. M. Mason et al. (2024).
Paper: The Study of the Circumnuclear Environment of Accreting Supermassive Black Holes with Realistic X-Ray Spectral Models
Authors: G. Dimopoulos, C. Ricci, S. Paltani
Figure caption: A comparison between the retrieved spectra. The spectra are continuum subtracted and then the ratio has been calculated for two configuration. First, a simple torus with equatorial column density NH = 1024 cm−2 and covering factor 0.6. Second, the RXTOPO with the same torus and three different polar cone column densities (﹩{\mathrm{log}}\,\left({N}_{{\rm{H}}}/{{\rm{cm}}}^{-2}\right)﹩ = 23.0–23.5–24.0). The three observing angles are selected so that at 20° no medium is intercepted, at 45° the cone is intercepted, and at 80° the torus is intercepted.
Paper: The Study of the Circumnuclear Environment of Accreting Supermassive Black Holes with Realistic X-Ray Spectral Models
Authors: G. Dimopoulos, C. Ricci, S. Paltani
Figure caption: The XMM-Newton EPIC (black points) and NuSTAR (red and blue points) data for NGC 424 along with the best fit model. The individual components are also present. The bottom panel shows the ratio between the data and the model.
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: (a) Pyroxene quadrilateral illustrating the compositional variations in pyroxenes. Colored symbols represent individual spot analyses of pyroxene grains from this study. For comparison, the pyroxene compositional range for sample 60025 is from O. James et al. (1991), and that for clast 3 A of sample 60016 is from N. Marks et al. (2019). (b) The An# [molar Ca/(Ca + Na + K)] in plagioclase is plotted vs. Mg# [molar Mg/(Mg + Fe)] for mafic minerals (pyroxene and olivine) present in clasts from CE-6 in this study. Results from pMELTS thermodynamic calculations for specific partial melts of Mg-suite analog sources with varying amounts of KREEP are represented by colored curves (T. C. Prissel & J. Gross 2020; S. M. Elardo & D. F. Astudillo Manosalva 2023). Arguin 002 is an evolved, KREEP-free Mg-suite rock (Z. Wang et al. 2025b).
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: CI chondrite-normalized REE patterns illustrating possible parental melt compositions for plagioclase and pyroxene in the clasts analyzed in this study. The REE mineral-melt partitioning parameterizations used are from J. J. Papike et al. (1996), L. J. Hallis et al. (2014), C. Sun et al. (2017), and N. Dygert et al. (2020). For the plagioclase Eu partition coefficient, we used DEu = 1.21, as calculated by N. Dygert et al. (2020) at 1100°C. Calculated ranges for possible pristine FAN parental melts and Apollo Mg-suite parental melts are from S. M. Elardo & D. F. Astudillo Manosalva (2023). The experimental melt composition of adding 0% KREEP and 5%–15% KREEP for the Mg suite is from S. M. Elardo et al. (2020). NWA 10401 and Arguin 002 are two lunar KREEP-free Mg-suite rocks, and their calculated parental magmas are from J. Gross et al. (2020) and Z. Wang et al. (2025b). The composition of pure high-K KREEP is from P. H. Warren (1989).
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: BSE images of noritic anorthosite and FAN clasts from CE-6 soil. (a) Noritic anorthosite (clast 4–28); (b) norite (clast 5–48); (c) anorthosite (clast 12–1); (d) anorthosite (clast 1–175). Mineral abbreviations: Opx—orthopyroxene; Pl—plagioclase; Aug—augite; Cpx—low-Ca pyroxene; Tro—troilite; Ilm—ilmenite.
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: CI chondrite-normalized REE values for plagioclase and orthopyroxene in clasts 4–28 and 1–175. The CI chondrite REE abundances are from W. F. McDonough & S.-S Sun (1995). The REE profiles for FAN and Mg-suite rocks are compiled from J. J. Papike et al. (1997), C. Floss et al. (1998), and J. J. Kent et al. (2017). Data for the norite from CE-6 lunar soil are from B. Su et al. (2025). The REE data of plagioclase and orthopyroxene for sample 60016 are from N. Marks et al. (2019), and those for sample 60025 are from C. Floss et al. (1998).
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: CI chondrite-normalized REE abundances for bulk-rock samples. Clast 1–175, identified as a pure anorthosite, is represented by in situ LA-ICP-MS analysis of plagioclase composition to approximate its bulk composition. Sample 4–28 reflects a modal bulk composition, while sample 12–1 represents a solution-based composition. Comparative data for Apollo norites are from C.-Y. Shih et al. (1993); anorthosite sample 60025, from O. James et al. (1991); sample 60016, from Y. Nakamura et al. (1973) and N. Marks et al. (2019); troctolite sample 76535, from L. A. Haskin et al. (1974); and noritic anorthosite 67215, from M. D. Norman et al. (2003).
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: Analysis of Al2O3 (wt%) and Mg# within the CE-6 region. (a) The locations and Mg# of the Copernican-aged craters (C1–C5, as reported in S. Gou et al. 2025) nearby the CE-6 landing region. The basemap is the Mg# map, which is based on KAGUYA multiband imager (MI) spectral data and the one-dimensional convolutional neural network (1D-CNN) algorithm derived from L. Zhang et al. (2023). (b) Mg# vs. Al2O3 contents are plotted for the CE-6 sample (circles) and the young craters (squares). The dashed polygon and shaded patches (i.e., Mg-suite, CE-5 mare basalt, magnesian anorthosites (MANs), FANs, and lunar feldspathic meteorites (FMT)) are modified after S. Gou et al. (2025).
Paper: Petrogenesis of Lunar Farside Highland Lithologies: Implications for Lunar Crust Formation
Authors: Jiaqi Zheng, Qi He, Zaicong Wang, Jun Huang, J. F. Pernet-Fisher, Yiheng Li, Xu Chen, Keqing Zong, Ioannis Baziotis, Long Xiao, Zhenbing She
Figure caption: Parental melts of KREEP-poor rocks of REE modeling and chondrite-normalized REE patterns for a KREEP-free LPUM during partial melting and fractional crystallization. The modeled REE contents of the source region, 0.5% partial melts from the source, and evolved melts (dashed gray curves) at varying degrees of fractionation (50%–90%) are shown. The modeled REE contents of the 5%–15% assimilation of KREEP are also shown.
Paper: Lithium Abundances of Main-sequence Stars in the Old Open Cluster NGC 188: Probes of Stellar Evolution beyond the Solar Age 
Authors: Qinghui Sun, Constantine P. Deliyannis, Bruce A. Twarog, Barbara J. Anthony-Twarog
Figure caption: A(Li) as a function of Teff (left panel) and mass (right panel) for main-sequence stars in NGC 188. The same symbols are used for NGC 188 as in Figure 1, while only SM is shown. The observed data are shown as colored symbols in both panels. In the left panel, the SSET model for Pleiades is shown as a blue line. The A(Li)–Teff trend for Pleiades (120 Myr; S. J. Margheim 2007; J. Bouvier et al. 2018; R. M. Maderak et al. 2021), Hyades/Praesepe (650 Myr; J. D. Cummings et al. 2017), NGC 752 (1.8 Gyr; A. M. Boesgaard et al. 2022), M67 (4.5 Gyr; G. Pace et al. 2012), and NGC 188 (6.3 Gyr) are shown in colored lines as denoted in the legend. The circles are A(Li) detections, while the downward triangles are A(Li) 3σ upper limits. For comparison, we mark the Sun at 5777 K (1 M⊙) and A(Li) = 1.05 dex (J. R. King et al. 1997) using a red ⊙ symbol. Open symbols mark upper main-sequence stars (12.9 < V < 13.5 mag) in M67, while filled symbols denote lower main-sequence stars (V > 13.5 mag).
Paper: Lithium Abundances of Main-sequence Stars in the Old Open Cluster NGC 188: Probes of Stellar Evolution beyond the Solar Age 
Authors: Qinghui Sun, Constantine P. Deliyannis, Bruce A. Twarog, Barbara J. Anthony-Twarog
Figure caption: V magnitude as a function of Teff for main-sequence stars in NGC 188. The single members (SM), binary members (BM), members with uncertain multiplicity (?M), and single likely members (SM?) are shown in different symbols, as denoted in the legend. Stars with cluster membership probability greater than 0.5 from T. Cantat-Gaudin et al. (2018) are shown in small red dots.
Paper: Theoretical Perspective on the Occurrence of Electrostatic Solitary Waves and Double Layers in Ganymede’s Wake Region
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Variation of critical Mach number, M0 (solid curves), and maximum Mach number, ﹩{M}_{{\rm{\max }}}﹩ (dashed–dotted curves), with the number density of H3+ ions, ni,3,0 for (a) slow ion-acoustic mode, (b) fast ion-acoustic mode 1, and (c) fast ion-acoustic mode 2. The normalized parameters are ni,1,0 = 0.13, ne,0 = 0.87, nb,0 = 0.13, σi,1 = 0.2, σi,2 = 0.2, σi,3 = 0.5, σb = 0.1, vb,0 = 0.001, and κ = 6.
Paper: Theoretical Perspective on the Occurrence of Electrostatic Solitary Waves and Double Layers in Ganymede’s Wake Region
Authors: R. Rubia, M. B. Dhanya, Kuldeep Singh, Ioannis Kourakis
Figure caption: Variation of critical Mach number, M0 (solid curves), and maximum Mach number, ﹩{M}_{{\rm{\max }}}﹩ (dashed–dotted curves), with the σi3 for (a) slow ion-acoustic mode, (b) fast ion-acoustic mode 1, and (c) fast ion-acoustic mode 2. The normalized parameters are ni,1,0 = 0.13, ni,1,0 = 0.33, ne,0 = 0.87, nb,0 = 0.13, σi,1 = 0.2, σi,2 = 0.2, σb = 0.1, vb,0 = 0.001, and κ = 6.
Paper: Lithium Abundances of Main-sequence Stars in the Old Open Cluster NGC 188: Probes of Stellar Evolution beyond the Solar Age 
Authors: Qinghui Sun, Constantine P. Deliyannis, Bruce A. Twarog, Barbara J. Anthony-Twarog
Figure caption: A(Li) as a function of Teff for main-sequence stars in NGC 188. The same symbols are used for NGC 188 as in Figure 1, while only SM and BM are shown. For comparison, we show A(Li) in NGC 188 from the literature (L. M. Hobbs & C. Pilachowski 1988; S. Randich et al. 2003), with the one common star linked by a gray line. The circles are A(Li) detections, while the downward triangles are A(Li) 3σ upper limits.
Paper: Lithium Abundances of Main-sequence Stars in the Old Open Cluster NGC 188: Probes of Stellar Evolution beyond the Solar Age 
Authors: Qinghui Sun, Constantine P. Deliyannis, Bruce A. Twarog, Barbara J. Anthony-Twarog
Figure caption: Spectral synthesis of two SMs near 5900 K, showing a lithium detection (star 4763) and an upper-limit case (star 2895). The blue dashed line shows the observed spectrum, the black line shows the no-Li case, and the red line shows either the best fit for the A(Li) detection or the value corresponding to the 3σ upper limit.