adsabs/AstroCLIMB huggingface dataset:
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 5-1
Authors: V. P. Shyam Prakash, Vivek K. Agrawal
Figure caption: PDS in the HB and NB segments showing QPO features. The PDS is modeled using power-law and multiple Lorentzian functions.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 5-1
Authors: V. P. Shyam Prakash, Vivek K. Agrawal
Figure caption: GX 5-1 spectrum in HB and NB fitted using the model tbabs*(diskbb+nthComp) in the 3–20 keV energy band. Residuals are also plotted along with the fit.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Case R = 1:2, θ = 10° and starting jet activity after 50 Myr and 1 Gyr (upper panels), and 2 Gyr and 5 Gyr (lower panels). Note that τ = t − t jet,0 and that the times shown are different for the 5 Gyr case.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Density and CR pressure projection maps in the z-direction. Case R = 1:2, θ = 20° and starting jet activity after 50 Myr and 1 Gyr (upper panels), and 2 Gyr and 5 Gyr (lower panels). Note that τ = t − t jet,0 and that the times shown are different for the 5 Gyr case.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Case R = 1:5, θ = 20° and starting jet activity after 50 Myr and 1 Gyr (upper panels), and 2 Gyr and 5 Gyr (lower panels). Note that τ = t − t jet,0 and that the times shown are different for the 5 Gyr case.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Volume weighted δ v 3/L 0 distributions at 2.9 Gyr for the R = 1:5, θ = 20° run. We show the distributions corresponding to the solenoidal (solid lines) and compressive (dashed lines) turbulent velocities as computed by the two methods described in Section 4.3. The first method (taking into account the AREPO output) is shown in gray color and the second method (using the vortex-p code) is shown in dark cyan color. We multiplied by a factor of 1030 for purposes of better visualization.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Case R = 1:5, θ = 10° and starting jet activity after 50 Myr and 1 Gyr (upper panels), and 2 Gyr and 5 Gyr (lower panels). Note that τ = t − t jet,0 and that the times shown are different for the 5 Gyr case.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Volume-averaged velocity divergence (left-hand panel) and magnetic field strength (right-hand panel) of the CR jet material as a function of time for the case R = 1:5, θ = 20° and t jet,0 = 50 Myr. We show the corresponding evolution for different thresholds described in Appendix B.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Same as Figure 3 for the R = 1:5 cases. We overplot in orange the results of the higher resolution simulations.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: The magnification-corrected, rest-frame Lyα profiles, ordered from left to right, then top to bottom, first by increasing central Lyα peak strength relative to the redshifted Lyα peak in the non-LyC-leaking apertures, then the LyC-leaking apertures by the numeric order of their slit identifier. Those in red (top row) are non-LyC-leaking apertures (slits M5, M4, and M6), in pink (slit M3) is a non-LyC-leaking aperture targeting a highly magnified, exotic object (see Section 5.1 for more details), and in blue are the LyC-leaking apertures (slits M0, M2, M7, M8, and M9). The dashed black lines represent the overall fits, and dotted black lines represent the individual Lyα peak fits, based on the median best-fit parameters from the fitting described in Section 3.5.4. The shaded region represents the 2σ uncertainties of the flux densities. The observations clearly show a significant variety of Lyα profiles in the Sunburst Arc. Slit M0 has a much larger flux density scale due to poor observing conditions that prevented an accurate fluxing (see Table 1 for more details about the observation).
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: HST/WFC3 F606W imaging of the Sunburst Arc from GO-15377 (PI: M. Bayliss). Black dashed rectangles on the main image mark the main arc segments, labeled as in K. Sharon et al. (2022). The inset panels enlarge the two largest arcs, which are the focus of spectroscopic MagE data presented in this work (Table 1). The MagE apertures appear as magenta rectangles, where solid apertures cover images of the LyC-leaking region, and dashed apertures do not. In the inset panels, circles (except for squares for the LyC-leaking region) mark images of different source-plane regions of the Sunburst Arc, as labeled and colored in the lens model of K. Sharon et al. (2022).
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: The fluctuations in B  x  are produced by subtracting the long-term background trends (red-dashed curves) from the original profiles measured by taking an average of 3 pixels at locations I, II, and III denoted in Figure 3(a) (see panels (a), (c), (e)). The top panels (b), (d), and (e) repeat the bottom panels of (a), (c), and (e) and are placed above the corresponding wavelet distributions for comparison. Note that 0 s in these figures corresponds to 1587 s, i.e., the starting time of the figures in the left panels. The wavelet distributions exhibit dominant periods of 59.06, 70.23, and 91.08 s at locations I, II, and III, respectively, as in Figure 5.
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: The spatial distribution of the total magnetic field at (a1) 962 s when the CS has been formed (see the right panel of Figure 1(a)) and at (a2) 2224 s during propagation of the waves (the same time as in Figure 3(a)). The color map scales for these plots are different due to the magnetic evolution. Magenta streamlines indicate the magnetic fields at 962 and 2224 s in (a1) and (a2), respectively. Panels (b), (c), and (d) show distance–time diagrams of the magnetic field magnitude along slits s1, s2, and s3, respectively.
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: The upper panels of (a), (c), and (e) show the density variations (black solid curve) measured at locations I, II, and III, respectively. The red-dashed curves in those panels denote the long-term background trends, which are subtracted in order to produce the detrended small-scale density fluctuations shown in the bottom panels of (a), (c), and (e), which are a signature of wave propagation. Panels (b), (d), and (f) show the corresponding results for v  y .
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: Panels (a), (b), and (c) give the spatiotemporal variations of temperature along slits s1, s2, and s3, respectively. The black dotted horizontal lines are the same as those in Figures 3 and 9. Panels (d), (e), and (f) represent the in-phase relation between perturbations in thermal pressure and temperature. Since these two quantities have different dimensions physically, we plot them in dimensionless form for consistency. Red- and blue-dotted curves are the background trends, which are subtracted to extract the perturbed quantities using the same time windows as described in Appendix C.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: Same as Figure 2 but for the X1.6 flare on 2023 August 5. The GOES X1.6 flare onset (∼21:46 UT), peak (∼22:21 UT), and end (∼22:40 UT) explain the duration of the flare rise and decay phase.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: White-light image from SOHO/LASCO-C2 combined with the white-light image from SDO/AIA 193 Å displayed with the GOES SXR flare component and solar radio dynamic spectra from Wind/WAVES over the M1.6 impulsive phase (a)–(b) and over the decay phase (c)–(d) for the M1.6 flare on 2023 August 5. The GOES M1.6 flare onset (∼06:16 UT), peak (∼07:23 UT), and end (∼08:10 UT) explain the duration of the flare's rise and decay phase.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: SDO/AIA 94 Å images (a) for flare M1.6 at 07:22 UT from N07W63 of the active region AR 3386 and (b) for flare X1.6 at 22:21 UT from N11W77 of the same AR 3386 of the Sun.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: Temporal profiles of 5 minute resolution data plotted for the time period of 01:00 UT 2023 August 5 to 17:55 UT 2023 August 6. (a)–(c) Solar proton fluxes (cm−2 sr−1 s−1) of 12–25, 25–40, 40–80, 83–99, 99–118, and 118–150 MeV overplotted with the respective smoothed data, and (d) background-subtracted data of the smoothed proton fluxes (cm−2 sr−1 s−1) of 12–25, 25–40, 40–80, and 83–99 MeV.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Morlet wavelet power spectra for the AIA slit time series, δ I(t), in Interval 2, (left) 193 Å, and (right) 304 Å. Increasing spectral power is denoted by increasing darkness. Significant power lies within the 95% confidence level contours and outside the hatched cone-of-influence region. Vertical lines at relative time t = 300 and 328 hr respectively mark the approximate eruption onset and eruption time. In each panel, the global wavelet power spectrum is also shown, with the spectral power normalized with respect to its variance. A dashed line denotes the global confidence level of the spectrum in each case. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Investigating the relationship between period increases in the EUV filament channel and height increase in the prominence, comparing results from the (a) Quiescent and (b) Precursor stages. Values for P  b /P  a  (from Table 2) are plotted with their respective error bars. Labels LS, F, and GW are used to denote Lomb–Scargle, Fourier, and Global Wavelet, respectively, with subscript numbers denoting whether the periods correspond to P 1 or P 2 in the table. The shaded region spans the possible values for ﹩\sqrt{{r}_{b}/{r}_{a}}﹩ (﹩\sqrt{120/101}﹩ - ﹩\sqrt{120/94};﹩ Table 1). Extended hatched regions include errors.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: (Left) Cross-correlation coefficient vs. lag time between the 193 and 304 Å time series (Interval 2). These are computed using smoothed versions of the time series for time t = 240–300 hr (red curve) and t = 255–270 hr (black curve). (Right) Cross-wavelet between the 193 and 304 Å wavelet power spectra. Time is expressed in hours from 2011 March 14 00:00 UT. Vertical lines are as in Figure 18. A global wavelet power spectrum is also shown on the right, normalized using its variance.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Morlet wavelet power spectra for the AIA ROI time series in Interval 3, (left) 193 Å and (right) 304 Å. In both panels, the time is expressed in hours from 2011 March 14 00:00 UT. Increasing spectral power is denoted by increasing color level. Significant power lies within the 95% confidence level contours and outside the hatched cone-of-influence region. Vertical lines are as in Figure 19. Normalized global wavelet power spectra are also shown, with the global significance level marked using dashed lines.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Filament intensity in SDO/AIA 193 Å (Interval 3) for the ROI shown in Figure 15 with a blue box. (Top) Averaged ROI intensity, I, and a smoothed profile, I 0. (Bottom) The profile δ I = (I − I 0)/I 0 is obtained using I and I 0 in the top panel. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Lomb–Scargle periodogram (blue) and Fourier power spectrum (red) for the 193 Å time series, δ I(t), in Interval 3. The Fourier spectrum is shown using a histogram mode. The spectra are normalized with respect to the variance of a global wavelet power spectrum, and the global significance level is shown as a dashed line.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Investigating the period increase in the 193 Å sequence (Interval 3), for the shorter-period behavior. The average period in a rolling window is calculated from the wavelet power spectrum, weighted with spectral power. Line thickness is increased where spectral power is greater. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: The Decline and Fall of ROME. V. A Preliminary Search for Star-disrupted Planet Interactions and Coronal Activity at 5 GHz among White Dwarfs within 25 pc
Authors: Matthew Route
Figure caption: White dwarf survey ν L  ν  radio luminosity detection limits compared to known stellar flare luminosities. The spectral type(s) of each system are given in parentheses. The flare radio luminosity of the interacting binary BY Dra AB is calculated from its X-ray flare luminosity ranges via the Güdel–Benz relationship, which relates the X-ray luminosity to radio luminosity of incoherent gyrosynchrotron stellar flares (A. O. Benz & M. Güdel 2010). Beamed flares observed at AD Leo are created by the coherent ECM process (A. V. Stepanov et al. 2001). The peak radio emission from AR Sco at 5 GHz is generated by the interaction of the white dwarf's magnetic field with the M dwarf companion's stellar wind and its radio luminosity determined using the Gaia measured parallax (E. R. Stanway et al. 2018, 2021). The luminosity for the planet-hosting pulsar system PSR1257+12 is calculated from its 430 MHz flux density, with distance obtained from Very Long Baseline Interferometry (A. Wolszczan & D. A. Frail 1992; Z. Yan et al. 2013). The dashed (dotted) lines mark the detection thresholds of our most (least) sensitive observations, those of WD 1334+039 in circular (WD 1632+177 in linear) polarization, relative to these flare energies.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Top:  Chandra ACIS-S images of NGC 5728 in the specified energy bands. These are binned at 1/8 of the native ACIS-S pixel and are adaptively smoothed with a 2–15 pixel scale, 9 counts under kernel, and 30 iterations. Regions of enhanced X-ray emission are indicated in each band. We show the background-subtracted number of counts (calculated from the raw data) in each region of interest (black circles, with 1σ errors), and compare them to those in equally sized (same area) nearby regions (pink circles and annuli). All images are shown in the ASINH scale, for easy comparison between the emission in different bands. Bottom: RGB composite images of NGC 5728 shown in different color scales to emphasize different features, linear, square root, and log scale, respectively. Red is the 0.3–1.5 keV image, green is the 1.5–3 keV, and blue is the 3–5 keV emission.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Left: 0.3–3 keV Chandra adaptively smoothed (9 counts under kernel, 0.5–5 pixel scale, 30 iterations) image of NGC 5728. The different X-ray structures analyzed in the current paper are highlighted in different colors: the innermost soft X-ray bicone (in green), and the circumnuclear star-forming ring (in red). Center: ALMA CO (2–1) observations of NGC 5728 show prominent spiral arms of cold molecular gas surrounding the nucleus, and a double-peaked morphology that straddles the center. Right: MUSE Hα+[N II] map of the central region of NGC 5728 illustrating the prominent star-forming ring observed at ∼1 kpc from the central source in the optical. The central and right panels show the location of the Chandra X-ray centroid as a white cross.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: Left: ratio map showing the 1.5–3 keV/0.3–1.5 keV emission ratio in NGC 5728 (“soft ratio map”). Right: ratio map showing the 3–5 keV/0.3–3 keV emission ratio in NGC 5728 (“hard ratio map”). These maps are derived from 1/4 subpixel data and are shown in log scale. The color scale shows the ratio value per 1/4 ACIS pixel.
Paper: The Decline and Fall of ROME. V. A Preliminary Search for Star-disrupted Planet Interactions and Coronal Activity at 5 GHz among White Dwarfs within 25 pc
Authors: Matthew Route
Figure caption: Sample Stokes V dynamic spectra and bandpass-integrated time series from this survey (left) and our previous survey of UCDs (right) at AO. The left panels exemplify the null detection of circularly polarized radio emission from WD 1344+106. This data set is the least corrupted by RFI and instrumental artifacts obtained during our survey. For comparison, the right panels depict a highly circularly polarized ECM radio flare from the T6 dwarf, WISEPC J112254.73+255021.5 (M. Route & A. Wolszczan 2016a, 2016b). Light (dark) gray denotes left (right) circularly polarized emission. Solid horizontal gray bars near 4.5 and 4.85 GHz mark where strong RFI was excised. The time series graphs have been smoothed over 3.6 s for clarity.
Paper: Deep Chandra Observations of NGC 5728. III. Probing the High-resolution X-Ray Morphology and Multiphase Interstellar Medium Interactions in the Circumnuclear Region
Authors: Anna Trindade Falcão, G. Fabbiano, M. Elvis, A. Paggi, W. P. Maksym
Figure caption: X-ray spectra obtained for the three regions defined in Figure 3. The spectra are binned with 15 counts per bin and fit with an absorbed soft thermal component and a soft power law. For R2, we also include a hard power-law component and a Gaussian for fitting the hard emission. Best-fit models and residuals are shown in each panel.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The evolution of Z atm/Z bulk for different equilibrium temperatures for a 1 M J planet of ﹩10\,{{k}}_{{\rm{B}}}{{m}}_{{\rm{u}}}^{-1}﹩.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: Final heavy-element mass fraction profiles for four different initial setups sorted by their convective stability. The figures in the low-entropy column started with a primordial entropy of ﹩8\,{{k}}_{{\rm{B}}}{{m}}_{{\rm{u}}}^{-1}﹩ and the figures in the high-entropy column with ﹩10\,{{k}}_{{\rm{B}}}{{m}}_{{\rm{u}}}^{-1}﹩ (for details of the entropy profiles, see Section 2.2).
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: Entropy assuming a homogeneous composition and the associated heavy-element mass fraction for the model from Appendix C at the beginning and after reaching steady state.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: Radius evolution of the models presented in Section 4.1.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The location of the RCB vs. time for a linear primordial entropy gradient from ﹩7\,\mathrm{to}\,10\,{k}_{{\rm{B}}}{m}_{{\rm{u}}}^{-1}﹩ and the model “extended” composition gradient. The black line shows the result using MESA. The teal line represents our analytical solution assuming Δs  X,Z  = 0. The red line is computed in a similar fashion but assuming the initial Δs  X,Z . Lastly, the orange line considers only the primordial entropy, i.e., it ignores any contribution from the composition gradient.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: A sketch of the idealized mixing process for a positive mixing entropy. The solid black line represents the entropy profiles, and the dashed lines the associated heavy-element mass fraction profile. The light blue region indicates the change in Z that leads to an increase in entropy due to mixing.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The heavy-element distribution for the various models we consider at the beginning (solid lines) and end (dashed lines) of the simulations (see Section 4.1 for further details).
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The time evolution of Z atm/Z bulk for a range of primordial entropies.