adsabs/AstroCLIMB huggingface dataset:
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The heavy-element mass fraction profiles at 4.55 Gyr when using different EoSs 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: The heavy-element distribution for the “Helled 2023” model at the beginning and end of the simulation for different primordial entropies.
Paper: Convective Mixing in Gas Giant Planets with Primordial Composition Gradients
Authors: Henrik Knierim, Ravit Helled
Figure caption: The heavy-element mass fraction profiles at the end of the simulations for different planetary masses. The dashed line shows the initial heavy-element mass fraction profile.
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 planetary masses between 0.3 and 2.0 M J.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: For G = 0.5, growth rate contours for m = 1 modes are displayed in the field-strength space, in which the x-axis denotes the strength of the high-latitude band, denoted by H band in the x-axis label, and the y-axis that of the low-latitude band, denoted by L band in that label. Left-hand and right-hand panels are, respectively, for antisymmetric (m = 1, A) and symmetric (m = 1, S) modes. As the band system migrates from high latitudes toward the equator, the four rows from top to the bottom show how the instability features change, respectively, for bands at 60°–20° (aa, ab), 55°–15° (ba, bb), 50°–10° (ca, cb), and 45°–5° (da, db).
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: ESC reveals that the separation between high- and low-latitude branches in each hemisphere may not be constant but may vary with the progress of the cycle. Adapting Figure 7(d) from S. W. McIntosh et al. (2021; the extended cycle in NGDC green line), the double-arrows are overlaid on the extended cycle. This reveals that the high- and low-latitude branches are more than 30° separated at the beginning of a solar cycle but their separation decreases as the cycle progresses.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Growth rates (left-hand panels) and phase velocities (right-hand panels) are displayed for a double-band system, for which the low-latitude band (i.e., the active-cycle’s band) is placed at 10° and the high-latitude band is placed at five different latitudes, namely at 20°, 30°, 40°, 50°, and 60°. Panels (a) and (c) display growth rates and phase velocities for m = 1 antisymmetric modes, and panels (b) and (d) for m = 1 symmetric modes. The purpose of keeping the field strength of high-latitude band fixed at 10 kG and varying the strength of low-latitude band is to show how the instability intensity varies with Alfvén speed provided by the low-latitude band’s peak-field strength. Furthermore, the choice of placing the low-latitude band at 10° is to demonstrate that the presence of a high-latitude band interacts to make the double-band system unstable when a low-latitude band is not unstable by itself at such a low-latitude. Note that there are two modes with comparable growth rates in two cases, namely when the bands are at 10° and 30°, and are at 10° and 40°. We distinguish these two cases by a dashed–triple–dotted curves as opposed to dashed curves in the antisymmetric case, and by a dotted curves as opposed to solid curves in the symmetric case.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Snapshots of flows (white arrow vectors) and magnetic fields (black arrow vectors) overlaid on the top-surface of the shell (color-map) in latitude–longitude planform for the antisymmetric and symmetric m = 1 modes, respectively, in left-hand and right-hand columns, for toroidal bands separated by 20°. For all panels, the high-latitude band’s peak is 10 kG and the low-latitude band’s peak is 30 kG. Red-yellow denotes bulging of the tachocline top surface, and green-blue the depressions. Panels from top to bottom display how the eigenfunctions for double-band system always connect between them in each hemisphere, and then eventually allow cross-equatorial communication as the high- and low-latitude bands migrate toward the equator.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Snapshots of flows (white arrow vectors) and magnetic fields (black arrow vectors) overlaid on top-surface of the shell (color-map) in latitude–longitude planform for the antisymmetric and symmetric m = 1 modes, respectively, in left-hand and right-hand columns, for toroidal field bands separated by 40°. For all panels, the high-latitude band’s peak is 10 kG and the low-latitude band’s peak is 30 kG. Red-yellow denotes bulging of the tachocline top surface, and green-blue the depression. Panels from top to bottom show how the eigenfunctions evolve as the band system migrates equatorward, keeping the same band separation and band amplitude.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Equatorial region enlarged to display cross-equatorial communication via flows (top panels) and fields (bottom panels) for the case of the bands at 5° and 25° in each hemisphere, i.e., for the cases presented in Figures 5(c) and (f). Again, left-hand and right-hand panels, respectively, display m = 2, A and m = 1, S. Note that the velocity vectors are also plotted in black arrows instead of white arrows for better visibility. Note that in this enlargement green is the prominent color in the right-hand panels because green implies no bulges or depressions, which is the case near the equator for the symmetric mode. We see this near the equator for all symmetric modes, such as in Figure 5 right-hand panels.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: The same as in Figure 2, but for 20° band separation.
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Same as in Figures 4 and 5, but for variable band separation during the band system’s equatorward migration; separation between high- and low-latitude bands in each hemisphere decreases from 35° to 20° by the time low-latitude band reaches 5°-latitude. The field-strength of both bands also changes with the frames, as labeled, roughly according to the progress of solar cycle. Note that unstable antisymmetric modes with highest growth rate change wavenumber from m = 1 to 2 (bottom two panels in the left-hand column).
Paper: Magnetohydrodynamic Instabilities of Double Magnetic Bands in a Shallow-water Tachocline Model. II. Teleconnection Between High- and Low-latitude Bands and Across Equator
Authors: Mausumi Dikpati, Bernadett Belucz, Robertus Erdélyi, Peter A. Gilman, Scott W. McIntosh, Breno Raphaldini
Figure caption: Eigenfunctions displayed in latitude–longitude space for two distinct modes of similar growth rates for the double-band system when a high-latitude band is at 40° and the low-latitude one is at 10° latitudes. The low-latitude band’s field-strength is 0.3 in dimensionless unit, or 30 kG dimensional; as in earlier Figures, the high-latitude band’s field-strength is 10 kG. Eigenfunctions in top and bottom panels respectively correspond to the cases with solid and dotted black curves in panels (c), (d) of Figure 8. Note that these solid and dotted curves in panel (d) of Figure 8 respectively display lower and higher phase speeds. Latitude–longitude structures look quite different for these two modes.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Left: comparison of CO column density radial profiles for three different models of the HD 163296 disk: MAPS model from K. Zhang et al. (2021a; blue), model with a CO depletion factor of 5 from C. Qi et al. (2015; orange), and model presented in this paper with a CO depletion factor of 320 (green). Reference CO column density values corresponding to τ = 1 for different CO isotopologue transitions based on RADEX calculations (see text) are marked in gray: 2 × 1020 cm−2 for C17O 1–0, 7 × 1019 cm−2 for C17O 2–1, 5.5 × 1019 cm−2 for C18O 1–0, and 1.9 × 1019 cm−2 for C18O 2–1, assuming ISM ratios of CO/C17O = 2005 and CO/C18O = 557. Right: radial profiles of the normalized integrated flux of C17O 1–0 (blue) and C18O 1–0 (orange) emission observed with ALMA toward the disk of HD 163296. The profiles are normalized to their respective values at a radius of 70 au to facilitate comparison of the relative flux changes. Error bars indicate the observational uncertainties. The relative flux of C18O 1–0 remains consistently higher than that of C17O 1–0, suggesting that C18O 1–0 is optically thicker than C17O 1–0 across the CO snow line.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Comparison of two disk models with different VIRaM layer thicknesses and disk masses. The left panel shows the CO column density profiles for Model 1 (thin VIRaM layer, 0.01 M ⊙, blue) and Model 2 (thick VIRaM layer, 0.04 M ⊙, orange). Model 2 exhibits a sharp drop in the CO column density across the CO snow line, while Model 1 shows a more gradual decline. The right panel shows C17O 1–0 emission spectra for both models. The integrated flux of Model 1 is consistently higher than Model 2, despite Model 2 having higher CO column density inside the snow line, as emission from beyond the CO snow line, where the gas is optically thin, dominates at this (low) angular resolution.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Radial profiles of integrated intensity (top) and their derivatives (bottom) for simulated C17O 1–0, C18O 1–0 C17O 2–1, C18O 2–1 emission (from left to right) in models with thick (blue) and thin (orange) VIRaM layers. The gray dashed line in each panel indicates the location of the CO snow line. For the optically thin lines, the derivative profiles for the thick VIRaM model show a minimum near the CO snow line resulting from the significant change in the CO column density with the radius. The minimum in the derivative is less prominent in C18O 1–0 than in C17O 1–0 due to increasing optical depth, and it becomes undetectable in C18O 2–1, which is optically thick.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Disk densities and temperatures for two models: (left) thick VIRaM layer with an isothermal vertical temperature structure, (center) thin VIRaM layer with a conventional vertical temperature gradient. The temperature contours (red) are at 20, 24, and 28 K, and the density contours (blue) are at 108, 109, and 1010 cm−3. (right) CO column density distributions for the two models. The disk with a thick VIRaM layer shows a sharp radial drop across the CO snow line.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Simulated integrated intensity images of C17O 1–0 and C18O 1–0 (ngVLA, top) and C17O 2–1 and C18O 2–1 (ALMA, bottom) for models with thin and thick VIRaM layers (as labeled). The light blue dashed line indicates the location of the CO snow line in the models. These images reveal a much sharper drop in C17O emission beyond the CO snow line for the thick VIRaM layer model than for the thin VIRaM layer model. A similar, less pronounced, effect is visible in C18O 1–0 but not C18O 2–1 emission, as the latter is optically thick.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Normalized flux profiles of HD 163296 C17O 1–0, 2–1 and C18O 1–0, 2–1 emissions for the ALMA observations (blue) and for disk models with CO depletion factors of 320 (orange) and 5 (green). The model with a depletion factor of 320 matches the data better. The C18O 2–1 emission is not sensitive to the CO depletion factor.
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Radial profiles and derivatives of C18O 1–0 emission observed by ALMA toward MAPS sources GM Aur, AS 209, IM Lup, and MWC 480. The gray dashed line in the panel of GM Aur indicates the location of the CO snow line determined in C. Qi et al. (2019).
Paper: Evidence for a Sharp CO Snow Line Transition in a Protoplanetary Disk and Implications for Millimeter-wave Observations of CO Isotopologues
Authors: Chunhua Qi, David J. Wilner
Figure caption: Radial profiles and derivatives of C17O and C18O 1–0 and 2–1 emission observed by ALMA toward HD 163296. The gray dashed line in each panel indicates the location of the CO snow line. The local minima in the derivatives for the optically thin tracers align closely with the CO snow line location.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Parameterized models describing the possible density structure and geometry of the pre-SN nebula surrounding the progenitor star of SN 2014C. The isosurfaces delineate material with a particle number density n > 104 cm−3; color indicates the density value (color legend provided on the right). The star at the center indicates the position of the SN explosion. Both models presented successfully replicate the X-ray lightcurve of SN 2014C. The model on the left (TOY_T50_D6.8) is tailored to match the temperature evolution inferred by D. Brethauer et al. (2022), while the one on the right (TOY_T150_D7) is needed to reproduce the temperature evolution observed by B. P. Thomas et al. (2022).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Mass flow rate at the progenitor star’s collapse vs. radial distance, obtained from the TOY models outlined in Section 3 (dotted and dashed lines), along with the two reference models characterizing the remnant’s expansion: one through the asymmetric outflow of a RSG progenitor with variable mass-loss rate (model RSG_A1_B1; red line), and the other through the nebula of a massive episodic eruption (model MEE_A8; blue line).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Upper panels: X-ray lightcurve in the [0.5, 100] keV band (red line) synthesized from runs TOY_T50_D6.8 (on the left) and TOY_T150_D7 (on the right) compared with the observed lightcurve of SN 2014C obtained with Chandra and NuSTAR (blue and green symbols; D. Brethauer et al. 2022 and B. P. Thomas et al. 2022, respectively). Dashed and dotted lines mark the contributions to emission from the shocked plasma from the nebula and the shocked ejecta, respectively. Lower panels: corresponding to the upper panels, the plots show the evolution of average X-ray emission-weighted electron temperature. Dashed and dotted lines indicate the average electron temperature of shocked plasma from the nebula and the shocked ejecta, respectively.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: 2D cross sections in the (x, z) plane show the spatial density distribution (in logarithmic scale) at the labeled times for models TOY_T50_D6.8 (left half panels) and TOY_T150_D7 (right half panels). Each image is normalized to its maximum, ﹩\max (\mathrm{log}{n}_{{\rm{e}}})﹩, for enhanced visibility. The symmetry axis of the disk aligns with the z-axis.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Bolometric lightcurve derived from our SN model compared with the actual one of SN 2014C (R. Margutti et al. 2017).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Left panels: the 2D cross sections in the (x, z) plane show the spatial density distribution (in logarithmic scale) of the CSM at core collapse from RSG (upper panel) and MEE (lower panel) models; each quadrant in the panels displays the result for each of the models listed in Table 2. The symmetry axis of the nebula aligns with the z-axis. The dashed and dotted contours show the cross section of the torus in runs TOY_T50_D6.8 and TOY_T150_D7, respectively. Right panels: density profiles along the red lines shown in the left panels are presented for the RSG (upper panel) and MEE (lower panel) models in comparison with the analogous profiles derived from the two TOY models (dashed and dotted lines).
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Upper panels: distributions of emission measure (EM) vs. electron temperature kT e and ionization timescale τ = n e t at the labeled times for model MEE_A2. Middle panels: corresponding three-color composite images of the EM distributions. The colors show the contribution to EM from the different shocked plasma components, namely the ejecta (green) and the nebula (red). Lower panels: maps of the continuum-subtracted Fe Kα line flux at the same times. The white contours identify the regions where 25%, 50%, and 90% of the Fe Kα line flux originates.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: Upper panel: mass-loss history used in model MEE_A8 (see Table 2), resulting in X-ray lightcurve and temperature evolution of the SNR consistent with those inferred from the analysis of X-ray observations of SN 2014C (e.g., D. Brethauer et al. 2022; B. P. Thomas et al. 2022). Lower panel: corresponding amount of mass released by the progenitor star in the millennia leading up to its core collapse.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: X-ray lightcurve in the [0.5, 100] keV band (upper panels) and evolution of the average X-ray emission-weighted electron temperature (lower panels) synthesized from models MEE_A2 (left panels) and MEE_A8 (right panels). These are compared with the luminosity and temperature derived at various epochs from the fitting of joint Chandra and NuSTAR spectra of SN 2014C using the spectral model 2VAPEC (cyan and magenta symbols) or VAPEC+VNEI (blue and red symbols). Dashed, dotted, and dotted–dashed lines show the contribution from shocked CSM, shocked ejecta, and shocked Fe, respectively, synthesized from the MEE models.
Paper: Constraining the Circumstellar Medium Structure and Progenitor Mass-loss History of Interacting Supernovae Through 3D Hydrodynamic Modeling: The Case of SN 2014C
Authors: Salvatore Orlando, Emanuele Greco, Ryosuke Hirai, Tomoki Matsuoka, Marco Miceli, Shigheiro Nagataki, Masaomi Ono, Ke-Jung Chen, Dan Milisavljevic, Daniel Patnaude, Fabrizio Bocchino, Nancy Elias-Rosa
Figure caption: As in Figure 12 but for model MEE_A8.