adsabs/AstroCLIMB huggingface dataset:
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Flux sky map for a boosted fireball model, generated using the FIREFLY code. We have plotted the flux distribution along the plane perpendicular to the observer. The zero on the x-axis denotes the merger center. The flux map starts as sharp and near the merger. Around 900 days, the dominant region appears to come from behind the merger, a little over 1018 cm away from the center. This shows the emergence of the counterjet. The sky flux map is drawn for five instances in time: 10, 50, 75, 230, and 900 days.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: Pictorial representation of the sky map calculation. Contributions from a particular emission region (﹩\hat{{\boldsymbol{r}}}﹩) along the line of sight (﹩\hat{{\boldsymbol{n}}}﹩) are considered, and integrated over the entire domain. The line of sight is fixed at an angle of θ obs. Its flux at the observer plane at d  L  ≈ 40 Mpc from the merger is calculated.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: The four-velocity evolution of the fireball. The red curve reflects the angular profile in the beginning of the simulation. The following colored plots are at various epochs under consideration in this paper. The boosted fireball starts with a narrow opening angle θ obs 1/Γ B  0.25 rad. It then spreads out as the fireball evolves.
Paper: Could the Recent Rebrightening of the GW170817A Afterglow Be Caused by a Counterjet?
Authors: Ranadeep G. Dastidar, Paul C. Duffell
Figure caption: The same as Figure 3. This figure shows the evolution of the boosted fireball energy profile. The energy per unit solid angle is plotted at various epochs.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: Comparison of ﹩\mathrm{log}({L}_{\mathrm{CaII}{\rm{K}}}/{L}_{{\rm{H}}\alpha })﹩ vs. accretion rate between magnetospheric accretion models (background) and observations (dots). Models are colored by [Ca/H], with purple representing solar abundance (1) and depletion increasing toward red. The grayed-out region represents the magnetospheric models without the contribution of the WTTS. Solid lines represent the median value for a given model abundance (1, 0.5, 0.1, 0.01) and dashed lines represent the 16th and 84th percentiles for the lowest and highest abundance values of the models, respectively. Typical uncertainties for observations are shown in the lower right corner.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: Probability density of abundance by number, colored according to the presence of gaps(red, TD), substructures (green, SubS), or absence of both (blue, FD) in each system. The black dashed lines represent ﹩\left({{N}}_{{\rm{Ca}}}/{{N}}_{{\rm{H}}}\right)/{\left({{N}}_{{\rm{Ca}}}/{{N}}_{{\rm{H}}}\right)}_{\odot }=0.7﹩.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: [Ca/H] vs. log(﹩\dot{{M}}﹩). The black line represents the best fit from the Markov Chain Monte Carlo linear regression; our 1σ confidence intervals are shown in gray.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: [Ca/H] vs. M ⋆ The gray region highlights the [Ca/H] ≤ −1 region, the minimum abundance we are able to detect for M ⋆ > 1. No relationship between the stellar mass and Ca abundance is found.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption:  M dust vs. [Ca/H]. Upper limits are indicated as arrows. No relationship between M dust and [Ca/H] is found.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: Probability density of the abundance by number, colored by star-forming region.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: Distribution of abundance by number, colored according to the presence (red, TD/SubS) or absence of structure in the disk (blue, FD) in each system.
Paper: Using the Ca II Lines in T Tauri Stars to Infer the Abundance of Refractory Elements in the Innermost Disk Region
Authors: Marbely Micolta, Nuria Calvet, Thanawuth Thanathibodee, Gladis Magris C., Carlo F. Manara, Laura Venuti, Juan Manuel Alcalá, Gregory J. Herczeg
Figure caption: [Ca/H] vs. R68. No relationship between R68 and [Ca/H] is found.
Paper: The IMF Clock Angle Effect on the Tail Cross Section of the Martian Magnetic Pileup Boundary and Bow Shock
Authors: Y. K. Yuan, 义铠 袁, M. Wang, 明 王, J. Y. Lu, 建永 吕, J. H. Chen, 静涵 陈, N. Cheng, 诺 程
Figure caption: Fitting results of MPB and BS tail cross sections at X = –4 R  M . The black arrow is the direction of the IMF clock angle, panel (a) is λ = 0°, and panel (b) is λ = 90°. The red line represents BS, the blue solid line represents the dayside crustal fields MPB, and the blue dotted–dashed line represents nightside crustal fields MPB.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Time–distance profiles in position angles (measured in degrees counterclockwise from to the solar north) ((a)) and kinematics ((b)–(f)) of the EUV wavefront, with an interval of 1 minute at altitudes from 1.05 to 1.25 R ⊙ for the 2011 September 22 event. In panel (a), the two vertical dotted lines indicate the time period during which the inclination angle is measured and averaged; the horizontal solid line marks the time span used to calculate the average speed in Column (6) of Table 1 and Figure 8; the horizontal dashed line denotes the position angle of the source region of the EUV wave (i.e., the eruption site). In panels (b)–(f), the solid curve represents the apparent wavefront speed (v w), which is the multiplication of the derivative of the time–distance profile in (a) (converted to radians) and the corresponding altitude, where the derivative is computed by the DERIV.pro function in the IDL; the cyan solid curve is the actual speed calculated by multiplying the apparent speed with the sine of the inclination angle; the green dashed–dotted curve indicates the fast magnetosonic speed (v fms) given by an MHD model at each altitude (see the text); the black and cyan curves are the fast magnetosonic Mach number (M fms = v w/v fms) scaled by the right axis, corresponding to the apparent and actual wavefront speeds, respectively; the pink text labels the approximate Universal Time for each closest data point.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Still running-difference EUV images of SDO/AIA 211 Å for five of the selected six events except for the 2013 May 13 event. (a)–(e) show a clear inclination of the primary wavefront. (f) displays the forward inclination of the transmitted wavefront in the 2017 September 10 event. The angles in units of degrees are the average inclination angles of the wavefronts over specified time periods (see text and the note of Table 1). The cyan diamonds mark the eruption sites. The dashed circles denote the heights from 1.05 to 1.25 R ⊙ with an increment of 0.05 R ⊙.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Similar to Figure 2, but for the 2015 May 5 event. The additional thick dotted line (horizontal in panel (a) and vertical in panels (b)–(f)) marks the approximate position of the boundary of a north polar coronal hole from where the EUV wave is transmitted. The two vertical dashed lines in panel (a) indicate the time period in which the inclination angle of the transmitted wavefront is estimated and averaged (see Table 1 and the text).
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Similar to Figure 2, but for the 2013 November 7 event.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Similar to Figure 2, but for the 2013 May 13 event. The difference from Figure 2 is that there are no types of lines related to the wavefront inclination.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Angular distances of the EUV wavefront, CME boundary, and white-light shock flank for the six events. Each panel contains a composite of running-difference images of SOHO/LASCO C2 and SDO/AIA 211 Å. The C2 time is overlaid on the image, and the AIA time is around when the EUV wave disappears. The white line marks the position angle of the eruption site, which is given in Column (2) of Table 2. The cyan line indicates the position angle where the EUV wavefront vanishes at all altitudes, from which the maximum travel distance of the EUV wavefront is obtained (see Column (3) of Table 2). The thick pink dashed line denotes the position angle of the CME boundary at the inner edge of the field of view (FOV) of LASCO C2 around the time when the EUV wave disappears, and the corresponding angular distance to the eruption site is given in Column (4) of Table 2. The pink solid line marks the position angle of the white-light shock flank at the inner edge of LASCO C2 FOV when the shock flank reaches its maximum distance from the eruption site (also provided in Column (5) of Table 2). The cyan arc and the corresponding text indicate the angular distance between the cyan line and the pink solid line. The pink arrow points to the white-light shock flank, which shows that the shock has laterally expanded to the opposite side with a maximum distance larger than 90°. The cyan arrow in panel (f) indicates the southward shock flank interacting with a streamer.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Cropped SDO/AIA images for the 2013 May 13 ((a)–(b)), 2013 November 7 ((c)–(d)), and 2020 November 29 ((e)–(f)) events. In the left panels are AIA 211 Å images, where the corona is enhanced using the SolarSoftWare routine aia_rfilter (see http://aia.cfa.harvard.edu/rfilter.shtml for details), and the cyan curves represent PFSS-extrapolated closed magnetic field lines by the pfss package in SolarSoftWare (see https://www.lmsal.com/~derosa/pfsspack/). In (b) and (f) are the same images as in their corresponding left panels, but the contrast is adjusted to highlight the coronal features. In (d) is an AIA 304 Å image corresponding to the 211 Å image in (c). The arrow in (b) points to a plausible coronal cavity indicating the PFSS-extrapolated loops in (a). The arrows in (d) indicate two prominences (filaments), possibly in the PFSS-derived loop system in (c). The white arrows in (f) mark two small diffuse bright features corresponding to the PFSS-extrapolated loops near position angle 65° in (e); the black arrow in (f) denotes a small prominence possibly related to the loops near position angle 36° in (e). The inset overlaid in (f) is an AIA 211 Å image on December 4 taken after the limb near position angle 65° rotates to on-disk, which is superimposed with contours of positive (cyan) and negative (red) 20 Gauss line-of-sight magnetic fields from SDO/HMI (J. Schou et al. 2012). The ticks on the solar limb scale the position angle in degrees.
Paper: Hybrid Simulations of the Martian Magnetotail Twist
Authors: Jingyi Zhou, Kaijun Liu, Riku Jarvinen, Esa Kallio, Kun Cheng, Shuai Zhang, Qi Liu, Yuqi Liu, Yan Wang, Ruohan Wang, Xinye Wang, Xuanyu Shang, Zhongyuan Xu, Yi Yuan
Figure caption:  YZ cuts of the normalized BX  at X = −1.5 R M ((a)–(d)) and −3.5 R M ((e)–(h)) in the four simulations of Group A, as labeled on the top of each column. The overlaid cyan, green, and yellow curves in each panel represent the locations of the neutral current sheet in the corresponding simulations with the same conditions of the IMF and crustal fields (if included) in Groups B, C, and D, respectively. They are to be compared with the white region separating the positive lobe (+BX , red area) and negative lobe (–BX , blue area) in the same panel, which indicates the position of the neutral sheet in an individual simulation of Group A. In addition, the black dashed circle represents Mars’ shadow and the vertical dashed line is at Y = 0. Finally, the white and black arrows in (a) depict how the twist angle (﹩{\theta }_{{\rm{Twist}}}﹩) is defined (see text for details).
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: (a) and (b) Average speed (v EUV) and average fast magnetosonic Mach number (M fms) of the EUV wavefronts at altitudes from 1.05 to 1.25 R ⊙; the dashed curve represents the mean value of all the events at these altitudes; the average time span is marked by the horizontal solid line in panel (a) of Figures 2–7 for each event, respectively. (c) The average speed (u EUV) of the EUV wavefronts compared with the lateral expansion speed of white-light CME-driven shocks (v WL); u EUV is the averaged speeds in panel (a) over all the five altitudes for each event, which is also listed in Column (6) of Table 1; the average lateral expansion speed v WL is from the fit of the ellipsoid model (see the text) and is given in Column (7) of Table 1; the dashed line is a one-to-one visual guide.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Similar to Figure 2, but for the 2020 November 29 event.
Paper: Hybrid Simulations of the Martian Magnetotail Twist
Authors: Jingyi Zhou, Kaijun Liu, Riku Jarvinen, Esa Kallio, Kun Cheng, Shuai Zhang, Qi Liu, Yuqi Liu, Yan Wang, Ruohan Wang, Xinye Wang, Xuanyu Shang, Zhongyuan Xu, Yi Yuan
Figure caption: The projection of three sets of magnetic field lines in (a) Run B1 and (b) Run D1 onto the XY plane. The magnetic field lines in one specific set all go through a group of points with the same X- and Y-values but different Z-values (as indicated by the green points). Each set contains seven lines in different colors according to their Z-values, as labeled on the right. The orange dashed lines mark the location of Y = −0.2 R M. The black and cyan dots on the orange dashed lines illustrate the SW flow at Z = 1.8 and 1.2 R M, respectively (see text for details). The black circle around the origin in each panel represents Mars.
Paper: Limb Observations of Global Solar Coronal Extreme-ultraviolet Wavefronts: The Inclination, Kinematics, Coupling with the Expanding Coronal Mass Ejections, and Connection with the Coronal Mass Ejection Driven Shocks
Authors: Huidong Hu, Bei Zhu, Ying D. Liu, Chong Chen, Rui Wang, Xiaowei Zhao
Figure caption: Similar to Figure 2, but for the 2017 September 10 event. The additional thick dotted lines (horizontal in panel (a) and vertical in panels (b)–(f)) indicate the boundaries of a south polar coronal hole where the EUV wave is transmitted. The two vertical dashed lines in panel (a) mark the time period where the inclination angle is measured and averaged for the wavefront after being transmitted by the coronal hole.
Paper: Hybrid Simulations of the Martian Magnetotail Twist
Authors: Jingyi Zhou, Kaijun Liu, Riku Jarvinen, Esa Kallio, Kun Cheng, Shuai Zhang, Qi Liu, Yuqi Liu, Yan Wang, Ruohan Wang, Xinye Wang, Xuanyu Shang, Zhongyuan Xu, Yi Yuan
Figure caption: The three-dimensional surface of the neutral sheet in Run A1 to illustrate the overall magnetotail twist.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Investigating the nature of streaming instability in our shock simulations. The left and right panels correspond to two different shock simulations, ﹩{{ \mathcal M }}_{{\rm{A}}}=20﹩ (the run ﹩{ \mathcal B }1﹩) and ﹩{{ \mathcal M }}_{{\rm{A}}}=10﹩ (the run ﹩{ \mathcal B }3﹩), respectively at ﹩t\approx 95\,{\omega }_{\mathrm{ci}}^{-1}﹩, where all other parameters v pt/c = 0.1, ﹩{{ \mathcal M }}_{{\rm{s}}}=40﹩, and m i/m e = 100 are identical. Panel (a) shows the current density (black) and anisotropic momentum flux (magenta) of NT protons in the upstream, panel (b) shows the profiles of the magnetic fields, and panel (c) represents the Fourier mode analyses of the magnetic fields for the thick blue/red region of the panel (b). In panel (c), the vertical dashed black line marks the resonant wavenumber, ﹩k=2\pi /{R}_{{\rm{L}}}\equiv \pi /{{ \mathcal M }}_{{\rm{A}}}\,{d}_{{\rm{i}}}^{-1}﹩, for particles propagating at twice the shock speed. The panels on the left suggest that ﹩{{ \mathcal P }}_{\mathrm{nt},{\rm{i}}}/{P}_{{\rm{B}},0}\gtrsim 20﹩ for the ﹩{{ \mathcal M }}_{{\rm{A}}}=20﹩ shock, resulting in predominantly right-handed (nonresonant) magnetic fluctuations, ﹩{\tilde{B}}_{{\rm{R}}}﹩. In contrast, for the ﹩{{ \mathcal M }}_{{\rm{A}}}=10﹩ shock in the right panels, the upstream fluctuations are mostly left-handed ﹩{\tilde{B}}_{{\rm{R}}}﹩, indicating that they are resonant with the current-driving protons. Note that this analysis applies to the linear growth stage of the instability. At later times, both resonant and nonresonant waves may exhibit equal power in the shock precursor (where NT particles diffuse), and the linear growth shifts to regions further upstream where NT particles stream.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Energy budget for the downstream thermal and NT populations, and the magnetic fields. The red and blue curves represent the fraction of total postshock energy density in NT protons and electrons with momentum p ≥ p 0,α  (as described by Equations (3) and (8)). ϵ th,i and ϵ th,e represent the energy density fractions for thermal protons (brown) and electrons (cyan), obtained for p < p 0,α , and ϵ B is the magnetic energy density.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Panel (a): diagnostics showing the beam plasma parameters in our benchmark shock run ﹩{ \mathcal B }1﹩ in Table 1. Panel (b): the time evolution of B ⊥/B 0 for the three controlled simulations using the parameters found in the shock run of the panel (a). Thick lines in panel (a) show the time-averaged (between ﹩100\mbox{--}150\,{\omega }_{\mathrm{ci}}^{-1}﹩) profile of thermal and NT proton number densities (normalized to far-upstream thermal proton density n 0), and the drift velocity of NT protons (v nt,i) in the background plasma rest frame. Note in panel (b) how the growth is delayed for larger m R, though eventually the same saturation is achieved.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: Injection efficiency of energetic particles as a function of v pt ≡ 3v sh/4 (panel (a)), ﹩{{ \mathcal M }}_{{\rm{A}}}﹩ (panel (b)), ﹩{{ \mathcal M }}_{{\rm{s}}}﹩ (panel (c)), and m i/m e (panel (d)). Red and blue lines represent the fraction of energetic particles with momentum p ≥ p 0,α  (Equation (3)), calculated at late times over a region of 1000 d i immediately downstream of the shock. Unless otherwise specified, v pt = 0.1c, ﹩{{ \mathcal M }}_{{\rm{A}}}=20﹩, ﹩{{ \mathcal M }}_{{\rm{s}}}=40﹩, and m R = 100.
Paper: Electron Acceleration at Quasi-parallel Nonrelativistic Shocks: A 1D Kinetic Survey
Authors: Siddhartha Gupta, Damiano Caprioli, Anatoly Spitkovsky
Figure caption: The temperature of downstream thermal plasma for different shock parameters (Table 1). The brown and cyan lines show the temperature of protons and electrons normalized to ﹩0.5{m}_{{\rm{i}}}{v}_{\mathrm{sh}}^{2}﹩ and the orange lines represent the electron-to-proton temperature ratio (T e/T i). The default parameters in all four panels are ﹩{v}_{\mathrm{pt}}=0.1c\equiv 3{v}_{\mathrm{sh}}/4﹩, ﹩{{ \mathcal M }}_{{\rm{A}}}=20﹩, ﹩{{ \mathcal M }}_{{\rm{s}}}=40﹩, and ﹩{m}_{{\rm{R}}}=100﹩, similar to Figures 7 and 8.