adsabs/AstroCLIMB huggingface dataset:
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The image of the KN BH surrounded by a prograde and retrograde thin accretion disk at 86 GHz. Top panel: observation angle θ 0 = 17 deg for the prograde disk. Middle top panel: observation angle θ 0 = 75 deg for the prograde disk. Middle bottom panel: observation angle θ 0 = 17 deg for the retrograde disk. Bottom panel: observation angle θ 0 = 75 deg for the retrograde disk. From left to right, the spin of the KN BH is a = 0.8, a = 0.8, and a = 0.94, with corresponding charge of Q = 0.3, Q = 0.5, and Q = 0.3. The mass of the BH is set to M = 1.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The influence of BH spin, BH charge, and observation inclination angle on the intensity. Left panel: the BH charge varies from 0 to 0.5 with a step size of 0.05, while the spin is fixed at a = 0.5 and the observation angle at θ 0 = 75 deg. Middle panel: the BH spin varies from 0 to 0.98 with a step size of 0.05, while the charge is fixed at a = 0.3 and the observation angle at θ 0 = 75 deg. Right panel: The observation angle varies from 0 to 180 deg with a step size of 15 deg, while the BH charge is set to 0.2 and the spin is set to 0.8.
Paper: Image of the Kerr–Newman Black Hole Surrounded by a Thin Accretion Disk
Authors: Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin
Figure caption: The intensity distribution of a KN BH surrounded by a prograde and retrograde thin accretion disk at 86 GHz. Top panel: intensity distribution along the x-axis for the prograde disk. Middle top panel: intensity distribution along the y-axis scenario for the prograde disk. Middle bottom panel: intensity distribution along the x-axis for the retrograde disk. Bottom panel: intensity distribution along the y-axis for the retrograde disk.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Colors show observed-frame [O II] SB for the galaxies in our sample and the galaxy Makani (J2118) as a comparison. On each panel, we show the area with a signal detected above an SNR threshold of four. The axes are labeled in kpc from the brightest spaxel. Note we use the same logarithm color scale for the whole sample to ease comparison.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Kinematics of the [O II] emission for the galaxy J1613. The axes are labeled in kpc from the brightest spaxel. Left-hand panels: The four panels show the [O II] velocity (v 50, v 02, and v 98) and velocity dispersion (σ) maps for the galaxy J1613. The magenta box, shown in the remaining right-hand panels, traces the central 6″ × 6″. Right-hand panels: These four panels show the v 50 and σ maps of the [O II] emission for the first (top panels) and second (bottom panels) [O II] kinematic components.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: The panels with a black background show a continuum image illustrating stellar emission at observed-frame 4000–5500 Å for the galaxies in our sample and the galaxy Makani (J2118). On each panel, the white contour represents the 4σ [O II] emission as presented in Figure 1. We use a logarithm color scale. The panels with a white background show HST/WFC3 F814W (rest frame V-band at these redshifts) observations of eight galaxies in our sample and the galaxy Makani (J2118). The axes are labeled in kpc from the brightest spaxel. North is up and east is left.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: [O II] kinematics for three of the galaxies in our sample with the highest values of velocity dispersion, σ, J1107 (top left-hand four panels), J1341 (top right-hand four panels), and J1500 (bottom four panels). In each set of four panels, we show in the top left-hand panel the [O II] central velocity (v 50); in the top right-hand panel the [O II] velocity dispersion (σ), in the bottom left-hand panel the [O II] maximum redshifted velocity (v 02); in the bottom right-hand panel [O II] maximum blueshifted velocity (v 98). All velocities of the ionized gas are relative to the systemic redshift of the source. The color bars show the velocity in km s−1. The axes are labeled in kpc from the brightest spaxel.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: [O II] kinematics for four galaxies in our sample with moderately high-velocity dispersion, σ, J0944, J1205, J1622, and J1506. In each quadrant, we show in the top left-hand panel the [O II] central velocity (v 50); in the top right-hand panel the [O II] velocity dispersion (σ), in the bottom left-hand panel the [O II] maximum redshifted velocity (v 02); in the bottom right-hand panel [O II] maximum blueshifted velocity (v 98). All velocities of the ionized gas are relative to the systemic redshift of the source. The color bars show the velocity in km s−1. The axes are labeled in kpc from the brightest spaxel.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Colors show observed-frame Mg II SB for the galaxies in our sample. On each panel, we show the area with a signal that looks real above a threshold defined after an eye inspection of the extracted spectra. The dashed white contour denotes 1σ Mg II emission, while the solid white one shows the 4σ [O II] emission as presented in Figure 1. The axes are labeled in kpc from the brightest spaxel. The Mg II signal per spaxel in J1713 is too faint to produce a reliable Mg II SB map.
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Radial SB profile of the [O II] emission. For each galaxy, the zero-point is set to be the brightest spaxel in the SB map, i.e., the origin of each panel in Figure 1. The red line shows the azimuthally averaged [O II] radial SB profile and the gray diamonds are the [O II] SB data at every spaxel. The purple line shows the radial profile of the stellar continuum, normalized to the peak of the [O II] profile, and the cyan line shows the extent of the ground-based seeing, also normalized to the [O II]. Errors are the standard deviation from the mean.
Paper: Has the Palomar 14 Globular Cluster Been Captured by the Milky Way?
Authors: Akram Hasani Zonoozi, Maliheh Rabiee, Hosein Haghi, Pavel Kroupa
Figure caption: Evolution of the half-mass radius (top), the total mass (middle), and α 2 (bottom) of different model clusters without PMS (S = 0). All models start with the same 3D half-mass radius of 5 pc but different numbers of particles: N = 5 × 104 (green solid lines, Model 2), N = 7.5 × 104 (blue dotted lines, Model 7), and N = 105 (red dashed lines, Model 9). In all models, first the clusters evolve around a point mass dwarf galaxy with M dw = 109  M ⊙ at an orbital distance of 2 kpc, and at the switching time, they are placed on a circular orbit in the MW at the Galactocentric distance of 71 kpc. The α 2 parameter is calculated for stars in the mass range of 0.5 < M/M ⊙ < 0.8 and inside the half-mass radius. Vertical lines show the corresponding t sw to each model (Table 1). The solid horizontal lines represent the observed values, and the dashed horizontal lines indicate the 1σ errors. The observed value of r h =  35.6 ± 0.6 pc is not shown in the top panel due to its large value. The very early drop of the mass and increase of the half-mass radius is due to the stellar evolution.
Paper: Has the Palomar 14 Globular Cluster Been Captured by the Milky Way?
Authors: Akram Hasani Zonoozi, Maliheh Rabiee, Hosein Haghi, Pavel Kroupa
Figure caption: Evolution of the half-mass radius (top), the total mass (middle), and α 2 (bottom) of the cluster with N = 1.75 × 105 particles and an initial 3D post-gas expulsion half-mass radius of 7 pc. In this model, the degree of mass segregation was chosen as S = 0.9. The cluster evolves around a point mass dwarf galaxy, with M = 1.0 × 109  M ⊙ at an orbital distance R {g,dw} = 2 kpc (green solid lines), entirely on a circular orbit around the MW at R {g,MW} = 71 kpc (black dotted lines), and has been switched from the dwarf galaxy potential to the MW potential in four different models: on a circular orbit at t = 1.6 Gyr (red dashed lines); on a circular orbit at t = 2.3 Gyr (orange dashed lines); on a circular orbit at t = 2.5 Gyr (blue dashed–dotted lines), and on an eccentric orbit with e ≈ 0.6 and R  a  = 71 kpc, at t = 2.3 Gyr (purple dashed–dotted lines). Vertical lines show the corresponding t  α  to each model (Table 1). The horizontal lines show the observed values.
Paper: Has the Palomar 14 Globular Cluster Been Captured by the Milky Way?
Authors: Akram Hasani Zonoozi, Maliheh Rabiee, Hosein Haghi, Pavel Kroupa
Figure caption: Evolution of the half-mass radius (top), the total mass (middle), and α 2 (bottom) of the cluster with N = 1.40 × 105 particles and the initial 3D post-gas expulsion half-mass radius of 7 pc. In this model, the degree of mass segregation was chosen as S = 0.9. The cluster evolves around a point mass dwarf galaxy, with M = 1.0 × 109 M ⊙ in an orbital distance R {g,dw} = 2 kpc (green solid lines), and has been switched from dwarf galaxy potential to the MW potential in two different models: place into the MW, in a circular orbit at t = 1.6 Gyr (red dashed lines) and in an eccentric orbit with e ≈ 0.6 and R  a  = 71 kpc, at t = 1.6 Gyr (purple dashed–dotted lines). The vertical line shows the corresponding t  α  (Table 1). The horizontal lines show the observed values.
Paper: Has the Palomar 14 Globular Cluster Been Captured by the Milky Way?
Authors: Akram Hasani Zonoozi, Maliheh Rabiee, Hosein Haghi, Pavel Kroupa
Figure caption: Evolution of the half-mass radius (top), the total mass (middle), and α 2 (bottom) of the clusters without PMS and with N = 1.75 × 105 particles and an initial 3D post-gas expulsion half-mass radius of 7 pc. The cluster evolves around a point mass dwarf galaxy, with M = 109 M ⊙ in an orbital distance R {g,dw} = 2 kpc (green solid lines), and has been switched from dwarf galaxy potential to the MW potential in an eccentric orbit with e ≈ 0.95 at three different times of t sw = 4, 9, 10 Gyr. The horizontal lines show the observed values. Vertical lines show the corresponding t sw to each model (Table 1).
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: –Same as in Figure A1
Paper: The Outflowing [O II] Nebulae of Compact Starburst Galaxies at z ∼ 0.5
Authors: Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti
Figure caption: Velocity dispersion σ map of the [O II] emission for six galaxies in our sample, i.e., J0944, J1205, J1500, J1558, J1713, and J1506. Velocity profiles of representative spaxels are shown in the insets, highlighting areas with high and low velocity dispersion. In the velocity profiles and spectra, the black line is the continuum-subtracted spectrum, the red-solid line is the total emission-line model, and the blue-dashed lines are the [O II] emission-line models for the individual [O II] doublet components.
Paper: Has the Palomar 14 Globular Cluster Been Captured by the Milky Way?
Authors: Akram Hasani Zonoozi, Maliheh Rabiee, Hosein Haghi, Pavel Kroupa
Figure caption: The same as Figure 1, but for clusters with N = 7.5 × 104 particles and different degree of PMS: S = 0 (dark and light blue dashed lines); S=0.7 (purple solid lines), and S = 0.9 (brown dashed lines). On each curve, the dark-colored part corresponds to the evolution period in the dwarf galaxy and the lighter part corresponds to the cluster evolution in the MW.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: Time–distance maps along the slits of 1×–6× in Figure 1. The blue plus symbols trace to each individual thread point with a local maximum intensity. The magenta solid lines show the sinusoidal fitting curve. In total, 35 individual threads are marked. Threads 22 and 23 in the red boxes are plotted in Figure 3 to show the width determination. Threads 9, 13, 15, and 24 in the cyan boxes are plotted in Figure 4 to show the increasing oscillation amplitude.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: Illustration of the toy model of radial phase mixing presented in Section 3.2.2. The left panel maps the distribution of particles in the Ω R –θ  R  and the R−V  ϕ  space, both color coded by 〈V  R 〉 at the time of 400 Myr. The right panel illustrates the L  Z −〈V  R 〉 wave signal of the dynamically cold (J  Z  < 8 km s−1 kpc, blue) and hot (J  Z  > 23 km s−1 kpc, red) populations at the time of 250 and 400 Myr. As phase mixing proceeds, the characteristic wavelength of the L  Z −〈V  R 〉 decreases. The wave of the dynamically hot population displays a systematic phase shift toward lower L  Z  compared to the cold one. The phase shift amplitude (ΔL  Z , lighter blue points corresponding to the right axis) increases with decreasing L  Z , as predicted by our toy model.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: Phase shift amplitude (ΔL  Z ) variation trend vs. L  Z  after the satellite pericenter passage. The plots in the upper and lower panels are from the simulation data at 1400, 1600, 2000, and 3400 Myr. The dashed lines in the upper row illustrate the ﹩{\rm{\Delta }}{L}_{Z}-\bar{{L}_{Z}}﹩ plot in eight different azimuthal ranges. In the lower row, the red and blue solid lines display the L  Z −〈V  R 〉 wave signal for the dynamically hot (J  Z  > 23 km s−1 kpc) and cold (J  Z  < 8 km s−1 kpc) subpopulations. Within the lower L  Z  range, we see a monotonic decreasing trend of ΔL  Z  with increasing L  Z  in most azimuthal ranges for all snapshots, consistent with the prediction of our toy model developed in Section 3.2.2.
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: (a), (c) Zoom out the red boxes in Figure 2 to show the displacement oscillations of threads No.22 and No.23. The blue pluses trace the thread with the local maximum intensity, and the magenta solid lines give the sinusoidal function fitting. The purple dashed lines represent the drifting motion or the oscillation equilibrium. The amplitudes of the oscillations at each peak are marked by lines with arrows, and the values are also given. The red arrow shows the drifting motion with drifting velocity. (b) Intensity distribution along the slit direction at three times as marked by blue, black, and red vertical lines in (a). (d) Similar to (b), but the intensity distribution is plotted only at one time marked by red vertical lines in (c).
Paper: Thread Displacement and Intensity Oscillations in a Quiescent Prominence
Authors: Yuxiang Song, Zongjun Ning, Dong Li, Fanpeng Shi, Jun Xu, Yuzhi Yang
Figure caption: NVST Hα image of the quiescent prominence on the solar southwest limb on 2019 October 31 at 07:41:54 UT. The bright solar disk is visible on the left edge of the image. The red solid lines indicate six slits marked by 1×, 2×, 3×, 4×, 5×, and 6× parallel to the solar surface. The distance between the two slits is about 6000 km (50 pixels). The cyan box shows the thread used to be sliced at different positions in Figure 5.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: The phase shift (ΔL  Z ) variation trend is shown in the same manner as Figure 4. The four snapshots are from simulation data at 800 (represents the bar-only case for comparison), 1200, 1500, and 1800 Myr. The vertical dashed lines mark the locations of corotation resonance (brown) and the 2:1 OLR (blue) of the bar.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: The temporal evolution of the modeled Galactic disk under the joint perturbation of transient spirals and a steadily rotating bar demonstrated in the same manner as Figure 3. The transient spiral potential reaches its maximal amplitude at 1200 Myr.
Paper: Radial Wave in the Galactic Disk: New Clues to Discriminate Different Perturbations
Authors: Chengye Cao, Zhao-Yu Li, Ralph Schönrich, Teresa Antoja
Figure caption: The temporal evolution of the modeled Galactic disk under the perturbation of two-armed transient spirals in the same manner as Figure 4. The times are at 200 and 300 Myr.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: Tachocline properties estimated using data sets obtained with a 5 × 72-day-long time series plotted as a function of time, using the time at the midpoint of the observational window. The panels on the left were obtained for data with symmetric fits to the mode profile, while those on the right with asymmetric profiles. The different colors and symbols correspond to data sets corresponding to GONG, MDI, or HMI observations using either the MDI or HMI projects’ pipelines or the SGK pipeline, as shown in the legend. The gray curve shows the monthly smoothed sunspot numbers from the Royal Observatory of Belgium, Brussels, whose scale can be read on the right-hand axes. The vertical solid lines mark the times of solar maximum, while the vertical dashed lines mark the times of solar minimum determined from smoothed values of activity proxies.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The position (left panels) and the width (right panels) of the tachocline plotted as a function of time for data sets of different time series length, i.e., 8×, 10×, 16×, and 32 × 72 days (top to bottom) and the SGK pipeline. Like in Figure 3, the black dots correspond to the GONG results, purple circles correspond to MDI results, and magenta circles correspond to HMI results. The vertical solid and dashed lines mark epochs of solar maxima and minima, respectively. The horizontal line in the panels on the left mark the position of the CZ base. The horizontal lines in the panels on the right are an average of all the points in each panel.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The upper and lower boundaries of the tachocline, i.e., r  d  + w  d  and r  d  − w  d , plotted as a function of time for data sets obtained with different time series lengths, i.e., 8×, 10×, 16×, and 32 × 72 days (top to bottom) and the SGK pipeline. Like in Figure 3, the black dots correspond to the GONG results, purple circles correspond to MDI results, and magenta circles correspond to HMI results. The vertical solid and dashed lines mark epochs of solar maxima and minima, respectively. The horizontal line marks the position of the CZ base.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The jump across the tachocline derived from the 72 day-long time series data sets using GONG, MDI, or HMI observations and the SGK pipeline (black dots, purple circles, and magenta circles respectively). The solid and dashed vertical lines mark, respectively, the positions of solar maxima and solar minima.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: Odd-order splitting coefficients, c 1–c 5, derived from a 16 × 72-day long time series plotted as a function of the lower turning points of the modes. The cyan points are the individual values, while the red points show values averaged over r  t  bins of width 0.015R ⊙. The error bars on the red points are not visible because they are similar to the size of the symbols.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The jump in the rotation rate across the tachocline for data sets corresponding to the approximately 1.5-yr, 2-yr, 3-yr, and 6-yr long time series data sets for GONG, MDI or HMI and the SGK pipeline. Like in Figure 3, the black dots correspond to the GONG results, purple circles to MDI results and magenta circles to HMI results. The vertical solid and dashed lines mark epochs of solar maxima and minima, respectively.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The difference between the exact and estimated values of tachocline properties plotted as a function of the exact value of the parameters. The differences are in the sense (exact value–estimated value). The left-hand panels ((a), (b), and (c)) show results for the grid-based method; the right-hand panels ((d), (e), and (f)) show results from simulated annealing.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: The distribution of tachocline parameters in the grid of 15,000 models.