adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Trends of sodium abundance vs. the [C+N+O/Fe] abundance ratio. Giants classified based on asteroseismic analysis form the background from Mosser et al. (2014) and Yu et al. (2018; small filled circles; see key). The underluminous stars from Li et al. (2022) are shown by orange squares. The abundance ratios of the normal giants and the underluminous stars are from APOGEE DR17. The normal-luminosity-RC CDGs, and the overluminous-RC CDGs from our study are represented by blue circles and red triangles, respectively. Large black squares are the previously known wGb stars that have asteroseismic data from Hon et al. (2021), and the small black circles are the rest of the known wGb stars from literature with carbon abundances from high-resolution spectra. The Li-rich giants (black crosses) are from the Yan et al. (2021) study. These Li-rich giants are the low-spectral-resolution RC sample that have good-quality APOGEE DR17 data. In total, we have a sample of 59 Li-rich RC stars for comparison with the CDGs. Six of our normal-luminosity-RC CDGs are included in the Li-rich study of Yan et al. (2021). We use the solar abundance of C, N, O, and Na as derived by Grevesse et al. (2007).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Various CNO abundance ratios and sums along with sodium, magnesium, and aluminium abundances against [Fe/H] for our CDGs (large symbols). A large sample of RC stars from Vrard et al. (2016) form the background sample (small circles). All abundances are from APOGEE DR17. Average error bars are shown on the lower right of each subplot. Solar abundances are from Grevesse et al. (2007).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Top panel: comparison of the average seismic masses of the RC CDGs using Equations (1), (3), and (4) (M avg;  see the text for details), vs. the nonseismic masses from Equation (5). The horizontal error bars show the 1σ standard deviation around the average seismic masses for each star. Bottom panel: comparison of the seismic radii and radii calculated from the Stefan–Boltzmann law.
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Our CDG sample is shown in the Toomre diagram. Dashed lines show constant values of the total space velocity, ﹩{v}_{\mathrm{tot}}\,={\left({U}_{\mathrm{LSR}}^{2}+{V}_{\mathrm{LSR}}^{2}+{W}_{\mathrm{LSR}}^{2}\right)}^{\mathrm{1/2}}﹩ at 70 and 180 km s−1 demarcating thin disk and thick disk components, respectively (Nissen 2004; Venn et al. 2004).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Top panel: LAMOST low-resolution spectra of the CDGs. Note that KIC 8352953 is the only RGB CDG in our sample. Bottom panel: comparison of the observed LAMOST medium-resolution spectra and synthetic spectra of KIC 8879518 for different Li abundances. Synthetic spectra (green solid line) of A(Li) = 3.2 dex best fits the observed spectra. The first five CDGs in the top panel and the CDG in the bottom panel show strong Li absorption lines at 6707.8 Å.
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Comparison of the seismic masses of the previously known wGb stars with TESS data determined using Equation (3), vs. their masses determined using the nonseismic mass Equation (5).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Comparison of various mass estimates of the RC CDGs using Equations (1)–(5).
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Hertzsprung–Russell diagram (left) and log(g)seis as a function of [C/Fe] (right). Our APOGEE-KEPLER common sample forms the background in a color scale that represents the number density of stars; darker colors indicate higher density. Dwarfs and subgiants (blue dots), inert He-core giants ascending the RGB for the first time (gray dots), and He-core burning giants (red dots) are shown. Kernel density histograms are included to show the log(g) and [C/Fe] distributions for various parts of the sample, with the color scheme following the background sample, and the dashed histogram showing our final C-deficient sample. We superimpose model tracks in the log(g)-[C/Fe] plane for comparison (see the text for model details). Starting with an initial [C/Fe] = 0.0, the models show a reduction of [C/Fe] by ≈0.05–0.2 dex, due to FDU dilution. As some dwarf stars have lower [C/Fe], which may reflect a lower initial abundance, we offset the 2 M ⊙ model (which has the larger C-depletion) by −0.15 dex to match the lower envelope of those stars. This indicates the expected lower limit of [C/Fe] for later phases of evolution (dashed model line). The vertical dashed line at [C/Fe] = −0.4 dex denotes the cut we use to define carbon-deficient stars (see the text for details). The larger symbols (filled circles) show our carbon-deficient sample. Large red circles are RC stars, and the two large gray circles are RGB stars. Formal error bars are shown on the bottom-right end of each subplot. The top and right panels of the right subplot show kernel density histograms for the normal giants (solid lines) and RC CDGs (dashed red line). We use the solar abundance of C as derived by Grevesse et al. (2007).
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Wide-band spectra of diffuse γ-ray emission for the DC propagation model, assuming an extra component with an ECPL spectrum. The left panel is for the inner Galaxy region, and the right one is for the outer Galaxy region. Note that the ARGO-YBJ and ASγ data in the left panel are for a different region of 25° < l < 100° and ∣b∣ < 5°, and the ARGO-YBJ upper limit for the right panel is for 130° < l < 200° and ∣b∣ < 5° (Bartoli et al. 2015; Amenomori et al. 2021). Source masks of these analyses are also different.
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Seismic diagram of our RC CDGs, which have known ΔΠ1 and Δν (11 stars; large filled red circles). Giants classified based on asteroseismic analysis form the background from Mosser et al. (2014; small filled circles; see key), in a color scale that represents the number density of stars; darker colors indicate higher densities.
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Comparison between the DC model-predicted diffuse γ-ray spectra and the ASγ data (Amenomori et al. 2021) for a region of 25° < l < 100° and ∣b∣ < 5°. An extra ECPL component is also added to account for the data. The same mask as adopted in the ASγ analysis is applied to the model curves. The other data are the same as Figure 3, whose ROIs are different from the ROI of ASγ.
Paper: Asteroseismology Sheds Light on the Origin of Carbon-deficient Red Giants: Likely Merger Products and Linked to the Li-rich Giants
Authors: Sunayana Maben, Simon W. Campbell, Yerra Bharat Kumar, Bacham E. Reddy, Gang Zhao
Figure caption: Carbon abundance as a function of ﹩\mathrm{log}(L/{L}_{\odot })﹩ for our RC CDGs. As can be seen in the Gaussian kernel density histogram above, the luminosity distribution is bimodal. This bimodality is discussed in detail in Section 3.6. We use the solar abundance of C as derived by Grevesse et al. (2007).
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Best-fitting results for spectra of Li, Be, B, C, and O nuclei, for the DC model (top panels) and DR model (bottom panels), compared with the measurements (Cummings et al. 2016; Aguilar et al. 2017, 2018; Yuan 2019).
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Wide-band spectra of diffuse γ-ray emission for the DC propagation model without masks, compared with Fermi-LAT data (magenta points). The labels of different lines are the same as those in Figure 2. The other data with masks are also shown for comparison.
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Wide-band spectra of diffuse γ-ray emission. Left panels are for the inner Galaxy region, and right panels are for the outer Galaxy region. The top two panels show the model predictions of the DC model, and the bottom two are for the DR model.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Our stellar NLTE yttrium-to-iron abundance ratios as a function of metallicity for 65 stars and the compilation from LTE studies from the literature (brown circles). The compilation was made of data from Honda et al. (2004), Hansen et al. (2012), Bensby et al. (2014), Roederer et al. (2014), and Reggiani et al. (2017). The same symbols are used as in Figure 10.
Paper: NLTE Analysis of Y I and Y II in the Atmospheres of FGK Stars
Authors: Sofya Alexeeva, Yu Wang, Gang Zhao, Feng Wang, Yong Wu, Jianguo Wang, Hongliang Yan, Jianrong Shi
Figure caption: Differences in differential abundance [Y/H] between NLTE and LTE for 65 investigated stars.
Paper: A Broadband X-Ray Study of the Dwarf Nova SS Cyg during Quiescence and Outburst
Authors: Anirban Dutta, Vikram Rana, Koji Mukai, Raimundo Lopes de Oliveira
Figure caption: Multiple strong line emission features seen in the RGS spectra during the quiescence (top) and outburst (bottom) phases.
Paper: Galactic Diffuse γ-Ray Emission from GeV to PeV Energies in Light of Up-to-date Cosmic-Ray Measurements
Authors: Rui Zhang, Xiaoyuan Huang, Zhi-Hui Xu, Shiping Zhao, Qiang Yuan
Figure caption: Model-predicted spectra of protons (top left), helium nuclei (top right), positrons (bottom left), and total electrons plus positrons (bottom right), compared with the measurements. Solid lines are for the DC model and dashed lines are for the DR model. For protons and helium nuclei, the “-high” and “-low” results correspond to the uncertainties of the measurements by indirect experiments. Higher curves at low energies (≲10 GeV) are unmodulated spectra to fit the Voyager-1 data.
Paper: A Broadband X-Ray Study of the Dwarf Nova SS Cyg during Quiescence and Outburst
Authors: Anirban Dutta, Vikram Rana, Koji Mukai, Raimundo Lopes de Oliveira
Figure caption: Spectrum and ratio (data/model) plot of the outburst-phase joint XMM-EPIC and NuSTAR data.
Paper: A Broadband X-Ray Study of the Dwarf Nova SS Cyg during Quiescence and Outburst
Authors: Anirban Dutta, Vikram Rana, Koji Mukai, Raimundo Lopes de Oliveira
Figure caption: Spectrum and ratio (data/model) plot of the quiescence-phase joint XMM-EPIC and NuSTAR data, including a partial covering absorber and Compton reflection, model Q1 (top), and including only the Compton reflection component, model Q2 (bottom).
Paper: A Broadband X-Ray Study of the Dwarf Nova SS Cyg during Quiescence and Outburst
Authors: Anirban Dutta, Vikram Rana, Koji Mukai, Raimundo Lopes de Oliveira
Figure caption: Comparison of three iron lines in the quiescence and outburst phases. The spectrum and ratio (data/model) plot is shown for PN data only. The quiescence-phase data are shown in black, and the outburst-phase data are shown in red.
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: NIR spectra of J064722.95+031644.6 taken with IGRINS on board the Lowell Discovery Telescope (upper panel) and with the Triple Spectrograph on P200 (lower panel). For the sake of clarity, only spectra in the K band are shown. The IGRINS spectrum was smoothed by an 11-pixel boxcar and the TSpec by a 7-pixel wide boxcar. The upper panels show the normalized IGRINS spectrum around the CO v = 2–1 overtone band, Al I, Na I, Ca I, and Mg I in the IGRINS spectrum. For reference, the CO first overtone band in the giant K star is shown in blue. The blue dashed vertical lines indicate the wavelengths of the lines at the systematic source velocity. The deep and narrow features around Na I and Ca I are due to the imperfect subtraction of telluric absorption lines and cosmic rays.
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: The broadband SEDs for nine YSOs marked in Figure 5. The sixth source (ID 5) is not shown because of the blending of two sources in the optical band. o1 is our source J0647. Nonsimultaneous photometric data are collected from Pan-STARRS (blue), Two Micron All Sky Survey (2MASS; cyan), UKIDSS (green), IRAC of Spitzer (yellow), AllWISE data release (orange), and Herschel PACS (red). The large difference between 2MASS and UKIDSS data as well as the drop from the Pan-STARRS Y to J band in object 9 is due to variability rather than contamination. The best-fitted YSO model is shown in a solid blue line.
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: Nearby star formation in 5.′6 ×7.′2 images in the PACs red (160 μm) and blue (70 μm) bands of Herschel, IRAC 1 (4.5 μm) of Spitzer, and the i band of Pan-STARRS (panels from left to right). The positions of nine YSO candidates are marked in red, and J0647 is labeled o1 (yellow circle).
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: The SED of J0647 in the quiescence (orange circles connected by dashed lines). For comparison, the binned TSpec of 2020 October 6 and quasi-simultaneous NEOWISE fluxes are shown in black squares, and the NEOWISE fluxes at the peak of the eruption in 2017 are also plotted (blue diamonds). Note that Tspec below 1.5 μm may be affected by systematic background subtraction. The best-fit model to TSpec and its constituted components are shown as solid lines.
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: Pre-eruption images (35″ × 46″) of J0647 in the IR and optical. From left to right: Herschel 160 and 70 μm, Spitzer 4.5 and 3.6 μm, UKIDSS K, H, and J, Pan-STARRS i. The green circle (3″ in radius) marks the position of J0647 (o1), while the blue circle labels the nearby YSO (Y1). J0647 is not visible in the image at wavelengths shorter than the K band.
Paper: A Gigantic Mid-infrared Outburst in an Embedded Class I Young Stellar Object J064722.95+031644.6
Authors: Tinggui Wang, Jiaxun Li, Gregory N. Mace, Tuo Ji, Ning Jiang, Qingfeng Zhu, Min Fang
Figure caption: The profiles of H2 lines from the IGRINS spectrum. Regions strongly affected by OH absorption lines are masked by cyan bars.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Top: circular apertures selected for the study of the different parts of the galaxy overlapped on the 8 μm (left) and [C II] images (right). The colors are as in Figure 6. Bottom: SED for the apertures, multiplied by a factor of Δ = 10016−i , where i is the identification number of the aperture shown on the right side of the plot.
Paper: New and Improved Lyα Reconstructions for M and K Dwarfs
Authors: Angeli Sandoval, Allison Youngblood, R. O. Parke Loyd, Kevin France
Figure caption: Lyα reconstructions for the eight M dwarfs and four K dwarfs. The black histogram represents the STIS G140M/E140M data. The blue and purple dashed lines represent the reconstructed intrinsic emission line for the star, where the former represents the profile convolved with the instrument line spread function and the latter has not been convolved. The black dashed line shows the ISM absorption component, which when multiplied by the reconstructed emission line gives the best-fit profile (pink line). The gray-shaded regions highlight residual geocoronal emission that was masked from the fit.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Intensity, velocity, and velocity dispersion maps for the H I, Hα, [C II], and CO lines of Arp 25. These lines show the distribution of neutral and ionized atomic hydrogen (H I and Hα) and of the warm and cold molecular hydrogen ([C II] and CO). The beam of each observation is shown as a black circle in the bottom left corner of each intensity map. The images show the lopsided emission from the ionized atomic and warm molecular hydrogen, while the neutral atomic and cold molecular gas emission is more uniform across the galaxy. A gradient in velocity is clearly visible, while a somewhat enhanced velocity dispersion is visible along the shock region.
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Adaptive kernel histogram of the velocity distribution of the NGC 2300 group. Velocities of single members are indicated with vertical segments. The vertical orange line and the horizontal orange segment correspond to the velocity and dispersion of the group computed with the biweight estimator (1985 and 255 km s−1).
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Infrared emission from Arp 25 observed with Spitzer (8 and 24 μm) and SOFIA/HAWC+ in the C, D, and E bands. The white circles in the left-low corner of each map correspond to the beams of each observation.
Paper: New and Improved Lyα Reconstructions for M and K Dwarfs
Authors: Angeli Sandoval, Allison Youngblood, R. O. Parke Loyd, Kevin France
Figure caption: Comparison between the reconstructed Lyα fluxes of this work and those of Youngblood et al. (2016). The dashed colored lines represent constant flux ratios between the reconstructions of the two works. For example, the black 1:1 line shows perfect agreement, while the 0.2:1 line corresponds to a 5× smaller flux in this work than compared to Youngblood et al. (2016).
Paper: Shock Enhanced [C II] Emission from the Infalling Galaxy Arp 25 
Authors: Dario Fadda, Jessica S. Sutter, Robert Minchin, Fiorella Polles
Figure caption: Coverage of the FIFI-LS observations (white contour) over a composite HST image of Arp 25 obtained from WFC3 images in the 275, 336, 438, 555, and 814 nm bands. Credit: ESA/Hubble & NASA, P. Sell. Acknowledgment: L. Shatz.
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Existence diagrams for an asymmetric bi-ion plasma mixture. The existence domain of solitary waves associated with the fast and with the slow IA mode (in the asymmetric model) are shown vs. the streaming (beam) speed U for (a) κ  e  = 20; (b) κ  e  = 4; (c) κ  e  = 3; (d) κ  e  = 2, and for fixed values of δ 1 = 2δ 2 = 2/3, U 1 = − U and U 2 = 2U. The fast mode is shown in blue color and the slow mode is in red. The solid curves correspond to M  s , while the dashed curves correspond to M  l .
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Fast-mode solitons in the symmetric model, for different κ  e  in a beam-free plasma. (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (fast mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of κ  e . We have taken U = 0, M = 1.1 and δ = 0.5. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Slow-mode solitons in an asymmetric beam plasma system, for different spectral index κ  e . (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (slow mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of κ  e . We have taken U = 1.5, M = 0.8, and δ = 0.5 in these plots. The same curve style and color has been adopted among the three panels, as a guide to the eye).
Paper: On the Existence of Subsonic Solitary Waves Associated with Reconnection Jets in Earth’s Magnetotail
Authors: Kuldeep Singh, Steffy Sara Varghese, Frank Verheest, Ioannis Kourakis
Figure caption: Slow-mode solitons in the symmetric model, for different κ  e . (a) Pseudopotential curve profile S(ϕ) vs. electrostatic potential ϕ. Panels (b) and (c), respectively, depict the (fast mode) IA electrostatic potential pulse (ϕ) and the bipolar electric field (E) profiles vs. the traveling space coordinate ξ, for different values of κ  e . We have taken U = 1.5, M = 0.65, and δ = 0.5 in this plot. The same curve style and color has been adopted among the three panels, as a guide to the eye.