adsabs/AstroCLIMB huggingface dataset:
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Left: relative accelerations parallel (top) and perpendicular (bottom) to the jet of moving knots in FSRQs (red circles), BL Lac objects (blue squares), and RGs (green triangles) vs. their angular distances from the core of the jet. Right: the same accelerations vs. the average projected linear distance downstream of the core.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the average flux of a knot relative to the average flux of the core, ﹩\langle {S}_{\mathrm{core}}\rangle ﹩, for the stationary (left) and moving (right) features in FSRQs (top), BL Lac objects (middle), and RGs (bottom).
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Light curves of moving knots B11 in the FSRQ 1510−089 (red circles), B11 in the BL Lac object 0954+658 (blue squares), and K8 in the RG 0415+379 (green triangles). The dotted lines represent the least-squares fits to the flux density decays of the knots. The data and fits for B11 and K8 have been shifted by −1.5 and −3.0 from their normalized values, respectively.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the relative flux densities of quasi-stationary features for the different subclasses—FSRQs (top), BL Lac objects (middle), and RGs (bottom).
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of all calculated (left) and typical (defined in Section 5.3, right) Doppler factors of variability, δ var, derived for reliable moving knots in FSRQs (top), BL Lac objects (middle), and RGs (bottom). The typical δ var for the BL Lac object 1101+384 is shown in the last bin to condense the axis.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of all calculated (left) and typical (defined in Section 5.3, right) viewing angles in FSRQs (top), BL Lac objects (middle), and RGs (bottom), derived from the apparent speeds and variability Doppler factors of reliable knots. Note the different scales in each panel.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of all calculated (left) and typical (defined in Section 5.3, right) Lorentz factors, Γ, in FSRQs (top), BL Lac objects (middle), and RGs (bottom), derived from the apparent speeds and variability Doppler factors of reliable knots.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Typical Doppler factor of variability for each source vs. the maximum brightness temperature of the core, A0, for resolved (closed symbols) and unresolved (open symbols with right-facing arrows, component size a ≤ 0.02 mas) epochs. FSRQs are shown in red circles, BL Lac objects in blue squares, and RGs in green triangles.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Comparisons of the physical parameters of blazar jets derived in this work (x-axis) with those derived in Jorstad et al. (2017; y-axis, filled circles) and Liodakis et al. (2018; y-axis, open circles). A gray dotted line showing a 1:1 relation is shown in each panel, and the p-value of a WRS test between the derived values (from Table 14) is given in the legend.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions for FSRQs, BL Lac objects, and RGs of the percent difference between the observed viewing angle Θ◦ and expected viewing angle ﹩{{\rm{\Theta }}}_{\max }\approx {{\rm{\Gamma }}}^{-1}﹩. A gray dotted line has been added at zero difference.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of physical parameters (a) δ var, (b) Γ, and (c) Θ◦ of reliable knots in the RG 0415+379. Red curves represent best-fit Gaussian distributions to the data. See the text for details.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Comparison between opening semi-angles, θ ◦ of sample sources, derived using methods A and B (see the text for details). The gray dotted line indicates ﹩{\theta }_{\circ }^{{\rm{A}}}={\theta }_{\circ }^{{\rm{B}}}﹩.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Observed viewing angle Θ◦ vs. theoretical viewing angle ﹩{{\rm{\Theta }}}_{\max }\approx {{\rm{\Gamma }}}^{-1}﹩ for reliable knots in FSRQs (red circles), BL Lac objects (blue squares), and RGs (green triangles).
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Number of individual VLBI epochs and AGNs: all available in the Astrogeo database, and those where we managed to determine the jet direction.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Example of a VLBI image with an extended jet and a successfully measured jet direction indicated by the arrow. The arrow here and in the figures below indicates the jet orientation, as determined in our analysis. The arrow ends mark the positions of the two Gaussian components in our structure model.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Distribution of angular distances between the core and the jet components for jet direction measurements at each frequency band. These distances indicate the scales probed by our analysis.
Paper: Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei
Authors: A. V. Plavin, Y. Y. Kovalev, A. B. Pushkarev
Figure caption: Example of a VLBI total intensity map with no detected jet structure. Here and in the subsequent figures, the beam size (FWHM) is indicated by the ellipse in the lower left corner.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Distributions of the age of reliable knots in the host-galaxy frame, ﹩{T}_{\mathrm{age}}^{s}={T}_{\mathrm{age}}/(1+z)﹩ (left), and plasma frame, ﹩{T}_{\mathrm{age}}^{\mathrm{plasma}}={\delta }_{\mathrm{var}}{T}_{\mathrm{age}}/(1+z)﹩ (right), in FSRQs (top), BL Lac objects (middle), and RGs (bottom). Values in parentheses are the number of knots in each distribution. Note that the age scale is neither linear nor logarithmic.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Flux decay rate k for reliable knots vs. the age of the feature in the host-galaxy frame, ﹩{T}_{\mathrm{age}}^{s}﹩, for FSRQ (red circles), BL Lac object (blue squares), and RG knots (green triangles). Fits to the model ﹩k\,=\,-a{({T}_{\mathrm{age}}^{s})}^{-b}﹩ are plotted in the same color as the subtype of blazar, with values as indicated in the legend.
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Maximum γ-ray flux ﹩{S}_{\gamma ,\max }﹩ (scaled by 10−8 ph cm−2 s−1) vs. (a) apparent speed β app and (b) Doppler factor δ var of the “typical” knot in FSRQs (red circles), BL Lac objects (blue squares), and RGs (green triangles).
Paper: Kinematics of Parsec-scale Jets of Gamma-Ray Blazars at 43 GHz during 10 yr of the VLBA-BU-BLAZAR Program
Authors: Zachary R. Weaver, Svetlana G. Jorstad, Alan P. Marscher, Daria A. Morozova, Ivan S. Troitsky, Iván Agudo, José L. Gómez, Anne Lähteenmäki, Joni Tammi, Merja Tornikoski
Figure caption: Maximum γ-ray flux, ﹩{S}_{\gamma ,\max }﹩ vs. maximum core flux density at 43 GHz, ﹩{S}_{43,\mathrm{core}\,\max }﹩, for FSRQs (red circles), BL Lac objects (blue squares), and RGs (green triangles).
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Left: functions Φ ab  (red line) and Ψ ab  (blue line), with respect to ϵ defined in Equation (G64). Right: functions ϵΦ ab  ∼ R  ab  (red line) and ϵ 2Φ ab  ∼ Q  ab  (blue line), where the temperature is fixed. Corresponding approximations for small drifts with Φ ab  = 1 are also plotted (dotted lines). Function ϵΦ ab  reaches maximum 0.57 at ϵ = 0.97, and function ϵ 2Φ ab  reaches maximum 0.70 at ϵ = 1.51. It is possible to conclude that the small drift approximation is reasonably accurate up to ϵ = 0.5, and that very small values ϵ ≪ 1 are actually not required. Even though we did not calculate the runaway effect for higher-order moments, out of curiosity we include a function ϵ 3Φ ab  (black dashed line) that does not decrease to zero for large drifts, but instead converges to a constant value of 1.33.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Normalized damping rate ζ  i  = ω  i /(∣k ∥∣v th∥) for a parallel propagating ion sound wave as a function of k ∥ λ mfp, where λ mfp is a mean-free path. Red line: Braginskii-type (isotropic) 13-moment model with quasistatic stress tensor and heat flux. Green line: Braginskii-type 13-moment model with evolution equations for the stress tensor and heat flux. Blue line: bi-Maxwellian 16-moment model with evolution equations for parallel and perpendicular pressures and (gyrotropic) heat fluxes. Magenta line: Landau fluid model with the quasistatic heat fluxes of Snyder et al. (1997).
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Heat conductivities ﹩{\kappa }_{\perp }^{a}﹩ and ﹩{\kappa }_{\times }^{a}﹩. Left: ion species, normalized as κ  i  m  i  ν  ii /p  i . Right: electron species, normalized as κ  e  m  e  ν  ei /p  e . For large values of x, the BGK asymptotic profiles ﹩{\kappa }_{\times }^{a}﹩ (dashed lines) match the Braginskii results exactly, whereas for ﹩{\kappa }_{\perp }^{a}﹩ (solid lines) the results differ by a proportionality constant.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Ion viscosities of the BGK model (red) and of the Braginskii model (black), normalized as ﹩{\hat{\eta }}^{i}={\eta }^{i}{\nu }_{{ii}}/{p}_{i}﹩ vs. the ratio x = Ω i /ν  ii . Left: perpendicular viscosities ﹩{\eta }_{1}^{i},{\eta }_{2}^{i}﹩. Right: gyroviscosities ﹩{\eta }_{3}^{i},{\eta }_{4}^{i}﹩. For large values of x, the BGK asymptotic profiles for ﹩{\hat{\eta }}_{3}^{i}=1/(2x)﹩ and ﹩{\hat{\eta }}_{4}^{i}=1/x﹩ become independent of collisional frequencies and match the asymptotic profiles of Braginskii exactly. The BGK asymptotic profiles for ﹩{\hat{\eta }}_{1}^{i}=1/(4{x}^{2})﹩ and ﹩{\hat{\eta }}_{2}^{i}=1/{x}^{2}﹩ have the correct functional dependence, but differ from the Braginskii asymptotes by a proportionality constant. The BGK operator reproduces the ion viscosity of Braginskii with surprisingly good accuracy.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Left: proton thermal conductivity ﹩{\hat{\kappa }}_{a}﹩ (red), given by (N15), and alpha particle thermal conductivity ﹩{\hat{\kappa }}_{b}﹩ (black), given by (N16). Middle: proton frictional heat flux given by β 0a  (N22). Right: alpha particle frictional heat flux given by β 0b  (N23). Note the surprising change of sign of β 0b  for N  a  > 0.57. We have verified that the same effect is present in the simplified 13-moment model of Burgers (1969)–Schunk (1977).
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Electron viscosities, normalized as ﹩{\hat{\eta }}^{e}={\eta }^{e}{\nu }_{{ei}}/{p}_{e}﹩ vs. the ratio ∣x∣ = ∣Ω e ∣/ν  ei . The results are less precise than for the ions in Figure 3, especially for small values of x; nevertheless, the same conclusions are obtained.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Normalized viscosities of the proton and alpha particle plasma, according to (N26). Collisions with electrons are neglected, in an analogous fashion to Braginskii. Left: proton viscosity ﹩{\hat{\eta }}_{{aa}}﹩ (red) and alpha particle viscosity ﹩{\hat{\eta }}_{{bb}}﹩ (black). Right: “cross-viscosity” ﹩{\hat{\eta }}_{{ab}}﹩.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Viscosities of deuterium and tritium plasma, according to (N36). Left: deuterium viscosity ﹩{\hat{\eta }}_{{aa}}﹩ (red) and tritium viscosity ﹩{\hat{\eta }}_{{bb}}﹩ (black). Right: “cross-viscosity” ﹩{\hat{\eta }}_{{ab}}﹩.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Left: deuterium thermal conductivity ﹩{\hat{\kappa }}_{a}﹩ (red) and tritium thermal conductivity ﹩{\hat{\kappa }}_{b}﹩ (black), given by (N30). Middle: deuterium frictional heat flux, given by β 0a  (N32). Right: tritium frictional heat flux given by β 0b  (N33). Note that the frictional heat fluxes  q  b u are defined with opposite signs in (N31) and (N19).
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: RMSE between MAVEN observations and MSWIM2D output for 2016–2019 at various source–target angular separations. Data are binned in intervals of 60 days. RMSE between model and observation for each variable in each interval are provided in (a). Note that solar wind speed is on a secondary vertical axis to increase detail. (b) Depicts the angular separations between MAVEN/MARS and OMNI (blue) and STEREO-A (orange). The vertical dashed lines show the alignment of MAVEN with either Earth or STEREO-A.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: Time-series comparison of MSWIM2D (red) and New Horizons SWAP-observed solar wind (black) for 2012–2019. (a) Proton number density per cubic centimeter, with the highest resolution in gray and the 10 day running average in black. (b) Solar wind bulk flow speed in kilometers per second. (c) Model thermal pressure and New Horizons SWAP total (PUI plus solar wind) pressure. The blue vertical dashed line marks the Pluto flyby on 2015 July 14. Note the dual horizontal axis, providing both date and radial coordinate in astronomical units.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: Time-series comparison of MSWIM2D (red) and MAVEN-observed solar wind (black) for 2018. The variables plotted are (a) proton number density per cubic centimeter, (b) bulk flow speed in kilometers per second, (c) proton temperature in kelvin, (d) radial magnetic field component in nT, (e) tangential magnetic field component in nT, (f) z-component of the magnetic field in nT, and (g) absolute angular difference between source spacecraft and MAVEN in degrees.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: RMSE between New Horizons observations and MSWIM2D output for 2012–2019 at various source–target angular separations. Data are binned in intervals of 60 days. The RMSE between model and observation for each variable in each interval is provided in (a). Note that density and pressure are plotted on the left axis, and speed is plotted on the right axis. (b) Depicts the angular separations between New Horizons and OMNI (blue/darker) and STEREO-A (orange/lighter). The vertical dashed lines show the alignment of New Horizons with either Earth or STEREO-A, including a shift in azimuth to account for motion along Earth’s orbit. Note the dual horizontal axis, providing both date and radial coordinate in astronomical units.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: Correlations between MAVEN observations and MSWIM2D output for 2015–2019. The variables plotted are (a) proton number density per cubic centimeter, (b) bulk flow speed in kilometers per second, (c) proton temperature in kelvin, and (d) magnetic field strength in nT. Trend lines have fixed intercepts at (0, 0), with the equation of each line provided on the plot. The RMSE and the correlation coefficient r are also shown for each variable.
Paper: MSWIM2D: Two-dimensional Outer Heliosphere Solar Wind Modeling
Authors: Timothy B. Keebler, Gábor Tóth, Bertalan Zieger, Merav Opher
Figure caption: Time-shifting required to fill the inner boundary using time series from two spacecraft. Black tick marks correspond to ∼40° intervals along the orbit of spacecraft 1 (OMNI/ACE, DSCOVR, etc.). The time shift required to fill a boundary cell at a given rotation is provided in black. Red tick marks and time shifts correspond to spacecraft 2 (STEREO) in a similar manner.
Paper: Generalized Fluid Models of the Braginskii Type
Authors: P. Hunana, T. Passot, E. Khomenko, D. Martínez-Gómez, M. Collados, A. Tenerani, G. P. Zank, Y. Maneva, M. L. Goldstein, G. M. Webb
Figure caption: Comparison of normalized collisionless heat fluxes ﹩{\hat{q}}_{\parallel a}={\zeta }_{a}+(2{\zeta }_{a}^{3}-3{\zeta }_{a})R({\zeta }_{a})﹩ in a weakly damped regime with real-valued ζ  a . Left: the imaginary part of ﹩{\hat{q}}_{\parallel a}﹩. Right: the real part of ﹩{\hat{q}}_{\parallel a}﹩. The colors are described in the text. Our Braginskii-type models do not contain these collisionless heat fluxes.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The distribution of the peculiar tangential velocities for 323 CBe stars identified from the LAMOST MRS DR7. A Maxwellian velocity distribution was fitted to the peculiar tangential velocities.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: Representation for the performance of ResNet applied to the featured Hα spectra in the validation set. The upper-left panel shows the TP detection of the learning module, and 209 spectra in the validation set with predicted Be spectra features were identified with the true label. The lower-right panel shows the TN detection for 205 prelabeled non-Be stars. The upper-right panel shows the null detection of any prelabeled non-Be stars identified as a Be star in the set, suggesting that none of the Be-star spectral features were missed by the learning model. The lower-left panel shows the spurious detection of Be stars due to misclassification. The ResNet model achieves an accuracy of 99.5%.
Paper: Identification of New Classical Be Stars from the LAMOST Medium Resolution Survey
Authors: Luqian Wang, 璐茜 王, Jiao Li, 蛟 李, You Wu, 优 吴, Douglas R. Gies, Jin Zhong Liu, 进忠 刘, Chao Liu, Yanjun Guo, 彦君 郭, Xuefei Chen, 雪飞 陈, Zhanwen Han
Figure caption: The G BP − B RP VS G  G  color–magnitude diagram for CBe stars identified from the LAMOST MRS DR7 database. The newly identified CBe stars from this work are plotted in blue and the prior known CBe stars crossmatched from literature are in black.