adsabs/AstroCLIMB huggingface dataset:
Paper: Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System
Authors: Rogerio Deienno, André Izidoro, Alessandro Morbidelli, David Nesvorný, William F. Bottke
Figure caption: Panel (a) shows the cumulative SFD of the population of C-type planetesimals implanted into the MAB from Figure 3. Two end-members for the SFD are labeled in black. The intermediate implanted SFDs are shown in gray. They all have the same slope of N(>D) ∝ D −5 (red oblique line) of the initial planetesimal population for D > 100 km. The current MAB SFD (Bottke et al. 2005) is shown in green. Asteroids 1-Ceres and 4-Vesta are also shown for reference (red). Panel (b) reports the results from two experiments where we followed the evolution of the implanted SFDs during depletion by the giant planet instability while still accounting for collisional grinding (see main text for details). The current MAB SFD (green) is repeated for reference.
Paper: Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System
Authors: Rogerio Deienno, André Izidoro, Alessandro Morbidelli, David Nesvorný, William F. Bottke
Figure caption: Panel (a): total mass of CC dust produced during Jupiter’s migration plus the total amount of mass generated in CC pebble-sized fragments that reached 1 au for the different planetary growth tracks considered in Figure 1. Panel (a) is the sum of the contribution shown in panel (b), the total mass of CC dust produced during Jupiter’s migration, and panel (c), the total mass generated in CC pebble-sized fragments that reached 1 au due to fast orbital decay. Green and red shaded areas demarcate the range of the maximum mass budget contribution that both Earth and Mars (respectively) could receive from outer solar system material based on analysis from meteorite collection, where 4% (dotted–dashed lines) represents the more probable amount (Burkhardt et al. 2021).
Paper: Plasma Heating and Nanoflare Caused by Slow-mode Wave in a Coronal Loop
Authors: Fanxiaoyu Xia, Tongjiang Wang, Yang Su, Jie Zhao, Qingmin Zhang, Astrid M. Veronig, Weiqun Gan
Figure caption: (a) The evolution of plasma density n and temperature T derived from the observations at position 3 at the loop are shown in blue and green, the fitted light curves of Δn and ΔT plus the background trends are shown in red, and the mean of the plasma density n mean and temperature T mean are shown in black. The error bars of n mean and T mean are shown in gray. (c) The ratio of the damping time (τ) to the wave period (P) as a function of the loop equilibrium temperature calculated based on the linear wave theory with thermal conduction alone (red), compressive viscosity alone (green), considering both (black), and the case with the viscosity enhanced by a factor of 3 (pink). The vertical dashed line marks the mean temperature (T 0 = 4.2 MK) of the observed loop, and the horizontal dotted line marks the observed τ/P = 0.58. (d) Time–distance map of the perturbed density (n 1/n 0) along the loop simulated using a 1D nonlinear MHD model with the classical thermal conduction and the 3-times enhanced viscosity (see in text for detail). (e) Time profiles of the perturbed density at the location x = 165 Mm for the one case when both the thermal conduction and viscosity coefficients take the classical values (green) and for the other case with the classical thermal conduction but the 3-times enhanced viscosity (red). The dashed lines are their exponential decay time fits. The measured wave period and damping time are marked on the plot.
Paper: Plasma Heating and Nanoflare Caused by Slow-mode Wave in a Coronal Loop
Authors: Fanxiaoyu Xia, Tongjiang Wang, Yang Su, Jie Zhao, Qingmin Zhang, Astrid M. Veronig, Weiqun Gan
Figure caption: Overview of the observations from SDO/AIA and the temperature derived from DEM analysis. (a) AIA 94 Å image of the loop region. The yellow and red dashed curves show the manually traced loop and the fitted loop, respectively. The yellow and red boxes mark the regions of the flare and the RB, respectively. (b) AIA 211 Å image of the loop region. Zoom-in at the right bottom corner shows the base-difference image of the region of interest. The red contour corresponds to the 80% level of the maximum value of the AIA 211 Å image. (c) Light curves derived by summing over the yellow box for the different AIA filters (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, 335 Å, and 1600 Å) normalized to the pre-event values at 17:37 UT. GOES 1.0–8.0 Å light curve is shown in gray. (d) Evolution of the plasma temperature averaged over the flare region. (e) AIA light curves derived by summing over the red box. The dashed vertical lines in panels (c)–(e) indicate the start and end times of the oscillation.
Paper: Plasma Heating and Nanoflare Caused by Slow-mode Wave in a Coronal Loop
Authors: Fanxiaoyu Xia, Tongjiang Wang, Yang Su, Jie Zhao, Qingmin Zhang, Astrid M. Veronig, Weiqun Gan
Figure caption: (a) Time–distance map of the intensity from the base-difference images along the traced loop in Figure 1(a). The red lines indicate the sound speeds calculated from the mean temperatures, and the fitted propagating speeds are shown in black. (b) Time–distance map of the temperature along the loop. The horizontal lines in panels (a) and (b) mark the selected positions 1–3 along the loop. (c) Time–distance map of intensity modelled with the best-fit parameters of the oscillation. (d)–(f) The detrended and normalized light curves (black) along with the best-fit light curves (red) for positions 1–3. (g) The electron density (blue) and the temperature (green) for the oscillation (solid line) and background trend (dashed line) at position 3.
Paper: Plasma Heating and Nanoflare Caused by Slow-mode Wave in a Coronal Loop
Authors: Fanxiaoyu Xia, Tongjiang Wang, Yang Su, Jie Zhao, Qingmin Zhang, Astrid M. Veronig, Weiqun Gan
Figure caption: DEM analysis for the loop region. (a) and (b) DEM maps in different temperature ranges. (c) The background-subtracted EM(T) profile (black) and the background EM(T) profile (blue) for the perturbation region marked in panel (b). The error bars derived from the Monte Carlo method provided by the revised sparse DEM code are shown in pink and green. The vertical dashed line indicates the lower boundary to separate the spike-shaped hot component above logT = 6.5 K from the warm background.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Slice maps through the center of the computational domain for different galaxy models, indicated by the panel titles. All snapshots are taken when 〈[Fe/H]〉 = −2.2. The number of SNe, N SNe, required to reach this mean abundance is 5600, 1300, and 14,000, respectively. The top row shows an edge-on view, while the bottom row shows a face-on view of the disk. In each panel, the left-hand side (blue–green color map) is the number density of H (﹩{\mathrm{log}}_{10}{n}_{{\rm{H}}}﹩) while the right-hand side (purple–yellow) is the local gas abundance of [Fe/H]. Each panel is 6z eff along each axis, while the scale bars indicate the relative sizes between panels. The time since the beginning of the simulation is shown. These times correspond to 1.89t  r , 3.87t  r , and 1.41t  r , respectively. In all models, individual SNR are clearly resolved, and the increased homogeneity of the lower SFR models at the same 〈[Fe/H]〉 can be easily observed.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Evolution of the velocity dispersion, σ  v  (blue) and the mean [Fe/H] abundance (〈[Fe/H]〉; purple line) as well as 1σ and 3σ spreads (shaded regions) as a function of time. The relaxation time, t  r , for each model is marked by the vertical gray line in each panel. The panel titles indicate the simulation. Models with lower SFR have a more slowly evolving 〈[Fe/H]〉 but tend to have smaller spread at the same mean abundance as models with higher SFR.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Mass-weighted distributions of [Mg/Fe] in the cold, dense gas as a function of 〈[Fe/H]〉 for SN injection sites with intrinsic yield variations. The solid white contours indicate the 99% extent of the distributions while the dashed lines indicate the 68% extent. The black shaded regions indicate the [Fe/H] bins used to bin the abundances measured by Roederer et al. (2014), the solid black lines indicate the 99% span of the sample in the bin, and the black dashed lines indicate the 68% span. From left to right, the surface density of gas in the modeled galaxy decreases.
Paper: Supernova-driven Turbulent Metal Mixing in High-redshift Galactic Disks: Metallicity Fluctuations in the Interstellar Medium and its Imprints on Metal-poor Stars in the Milky Way
Authors: Anne Noer Kolborg, Davide Martizzi, Enrico Ramirez-Ruiz, Hugo Pfister, Charli Sakari, Risa H. Wechsler, Melinda Soares-Furtado
Figure caption: Top panel: Median (solid lines), 25th, and 75th percentile (shaded region) of the mass of Fe (Mg) enclosed within R cool around all SN injection sites (average over 15 Myr intervals) in the MW progenitor with low SFR (purple) and the one with high SFR (yellow). The solid black line marks the mass of Fe per injected SN and thus provides a measurement of the degree of overlap between adjacent mass injection events. Both models are marginally consistent with a single enrichment model at low 〈[Fe/H]〉. Bottom panel: cumulative distribution functions (CDF) of the mixing masses derived for all injected SNe in the two MW progenitor models (colors are the same as in the top panel). The shaded region denotes the IQR for both distributions. The patchy distribution of elements in the higher SFR model translates to a wider distribution of mixing masses for the SNe.
Paper: Plasma Heating and Nanoflare Caused by Slow-mode Wave in a Coronal Loop
Authors: Fanxiaoyu Xia, Tongjiang Wang, Yang Su, Jie Zhao, Qingmin Zhang, Astrid M. Veronig, Weiqun Gan
Figure caption: (a)–(e) Base-difference images for the region of the RB. (f) Time profiles for EM(T) integrated over different temperature intervals. The peak time of the thermal energy is marked by the vertical line. (g) For the region of the RB, EM(T) profiles at the peak time of thermal energy (black) and the time before RB (blue) derived with the Monte Carlo method.
Paper: Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System
Authors: Rogerio Deienno, André Izidoro, Alessandro Morbidelli, David Nesvorný, William F. Bottke
Figure caption: Total mass in C-type planetesimals implanted in the MAB associated with the different planetary growth tracks and disk masses adopted in Figure 1, i.e., for Jupiter growing and migrating from 10, 15, 20, and 25 au all the way to 5.2 au. Symbols are the same as in Figure 1(b). The figure also shows, for reference, (i) the current mass of the MAB (green dotted–dashed line; ≈5 × 10−4 M ⊕) and (ii) the maximum implanted amount of mass (shaded yellow; 1.5 × 10−3 M ⊕ ≤ M implanted ≤ 0.75 M ⊕) of C-type planetesimals that could be depleted by models of the giant planet instability followed by depletion due to subsequent chaotic diffusion. Note that the results related to the case 2.0 MMSN, fpl = 0.5 when Jupiter starts at 25 au were suppressed because the very massive disk interior to Jupiter induced planetesimal-driven migration that caused Jupiter’s growth track to diverge from its analytical path (see Section 2). Therefore, we did not evaluate this case.
Paper: Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System
Authors: Rogerio Deienno, André Izidoro, Alessandro Morbidelli, David Nesvorný, William F. Bottke
Figure caption: Representation of the implantation mechanism via MMR transport during Jupiter’s inward gas-driven migration (case 2.0 MMSN, fpl = 0.5, ﹩{a}_{\mathrm{Jup}}^{\mathrm{init}}=﹩ 15 au). The evolution of the eccentricity, inclination, and planetesimal radii (top, middle, and bottom panels in each plot) as a function of semimajor axis is provided. The planetesimal sizes are colored to improve visualization. Time evolves from left to right and top to bottom, as Jupiter (black filled circle), in this example, moves from ﹩{a}_{\mathrm{Jup}}^{\mathrm{init}}=﹩ 15 au to ﹩{a}_{\mathrm{Jup}}^{\mathrm{final}}=﹩ 5.2 au. Planetesimals are more efficiently transported via 2:1 and 3:2 MMR shepherding (vertical dashed lines). The figure also shows that collisional evolution happens mainly once planetesimals are in MMRs (see Section 4 for discussion). The MAB space (gray shaded area) is defined as in Deienno et al. (2016, 2018; region limited within 1.8 au ≤ a ≤ 3.6 au). The horizontal lines in the bottom panels are shown for reference sizes of r = 10−5, 10−3, 10−1, 101, 103, and 105 km (bottom to top).
Paper: Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System
Authors: Rogerio Deienno, André Izidoro, Alessandro Morbidelli, David Nesvorný, William F. Bottke
Figure caption: (a) Planetary growth tracks for Jupiter starting at 10,  15,  20,  and 25 au as a Moon-sized object (M                   ﹩{}_{{\rm{J}}{\rm{u}}{\rm{p}}}^{{\rm{i}}{\rm{n}}{\rm{i}}{\rm{t}}}﹩ = 0.01 M ⊕) and migrating all the way to 5.2 au (current position with its current mass, M Jup ≈ 330 M ⊕; gray circle). (b) Total mass in the disk interior to Jupiter’s initial orbit and outside 5 au (see main text). Symbols in the bottom right corner represent the many cases studied (radial mass distributions, MMSN, and the initial fraction of the total solid MMSN mass transformed into planetesimals in each given disk, fpl, when assuming a 1% stellar metallicity).
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Top row: magnification difference in log-scale for three pairs of lens configurations indicated in the subpanel titles. q = 10−3 for all cases. Color bar to the right shows the difference scale in log10. The oval-shaped contours are the loci of equal magnification (null). Three null-crossing source trajectories with α = 15°, 45°, and 90° are shown with the two-segment solid lines, with the direction going from the upper right to the lower left. The green central caustics are for the changing s  B . Second row: magnifications (μ) for null-crossing trajectories in the same color coding as the top row. Solid lines are for s  A  and dashed lines for s  B . The x-axis (time) is centered on the lens-axis null and scaled to ∣ξ null∣. Bottom three rows: planetary perturbation shown as the difference to a single-lens model in units of magnitudes. The maximum deviation is indicated in the second-to-last row.
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Deviation of ξ null,0 from the exact null location, normalized to ∣(s  A  − 1/s  A ) − (s  B  − 1/s  B )∣, where the exact null location is derived numerically with q = 10−4. Three solid curves show this relative error for changing s  A  against three values of fixed s  B  ≃ (1/1.3, 1/1.8, 1/2.5). The two dashed lines with darker colors show the alternative expression ξ null,hm which is exact for ξ null ≪ 1 (see Section 2.2), or equivalently s A ∼ 1/s B, shown only for ∣ξ null∣ < 0.5 and ∣s A − s B∣ > 1.
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Example of the offset degeneracy generalized to triple-lens systems. Top: magnification difference between triple-lens configurations of (s 1, s 2, ϕ) = (1.2, 1.25, 60°), referred to as the wide–wide configuration whose central caustic is shown in blue, and the close–close configuration of (0.8189, 0.7938, 60°) whose central caustic is shown in green. ϕ is the angle between the two lens axes (dashed lines), with the horizontal one corresponding to s 1. The two resulting lens-axis nulls are marked with cyan dots, which coincide with the source trajectory (solid line). Bottom: light curves for the null-crossing trajectory. In the legend, s ↔ 1/s refers to the (1/1.2, 1/1.25, 60°) configuration expected from the central caustic degeneracy. The designations “close” and “wide” refer to the caustic topology rather than the close–wide degeneracy. The bottom panels show light-curve residuals of the degenerate configurations to the wide–wide configuration in units of magnitudes. Light curves resulting from the central caustic degeneracy (green curves) are shown to have greater residual than that from the offset degeneracy (red curves). The horizontal axis is the source location projected to the x-axis, and the cyan dots indicate the nulls allowing for a straightforward comparison to the top panel.
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Same as Figure 3, but for three different configurations.
Paper: A Mathematical Treatment of the Offset Microlensing Degeneracy
Authors: Keming Zhang, 可名 张, B. Scott Gaudi
Figure caption: Error on the ﹩{s}^{\dagger }=\sqrt{{s}_{{\rm{A}}}\cdot {s}_{{\rm{B}}}}﹩ heuristic, defined as the difference between the predicted value of u anom = s † − 1/s † from s A,B, and the exact location of equal magnification on the lens axis. Solid curves are for the s † heuristic, and dashed curves are for the offset degeneracy (u anom = ξ null,0) for comparison. Quantities are defined similarly to Figure 2.
Paper: Bridging the Bondi and Event Horizon Scales: 3D GRMHD Simulations Reveal X-shaped Radio Galaxy Morphology
Authors: Aretaios Lalakos, Ore Gottlieb, Nicholas Kaaz, Koushik Chatterjee, Matthew Liska, Ian M. Christie, Alexander Tchekhovskoy, Irina Zhuravleva, Elena Nokhrina
Figure caption: To survive the onslaught of infalling gas, jets deflect toward the equatorial plane (﹩{ \mathcal T }\sim 90^\circ ﹩, panel e), before aligning with the z-axis (﹩{ \mathcal T }\lesssim 10^\circ ﹩). This jet reorientation naturally results in an X-shaped jet morphology (Figure 2). The early period, t ≤ 5 × 104 R g/c, of high mass accretion rate ﹩\dot{M}/{\dot{M}}_{{\rm{B}}}\gtrsim 0.06﹩ (panel a) features low values of the dimensionless BH magnetic flux ϕ BH ≲ 20 (panel b), total-EM to BZ jet-power ratio L/L BZ ≲ 0.25 (panel c), and jet energy efficiency η ≲ 10% (panel d). The infalling dense gas easily deflects the weak jets sideways, toward the equatorial plane, resulting in high jet-tilt angle ﹩{ \mathcal T }\sim 90^\circ ﹩ (panel e) and large variations, ∼180°, in precession ﹩{ \mathcal P }﹩ angle (panel f). At later times, t ≳ 105 R g/c, the accumulation of large-scale vertical magnetic flux on the BH leads to strong ϕ BH ∼ 50 (panel b) and a MAD state (highlighted in green; steady-state averages shown with horizontal dashed orange lines): The powerful jets, L/L BZ ∼ 1 (panel c) and η ∼ 150% (panel d), suppress ﹩\dot{M}﹩ (panel a) and stably propagate along the z-axis (﹩{ \mathcal T }\lesssim 10^\circ ﹩, panel e), about which both the BH and the ambient gas rotate, out to large distances (Figures 2 and 4). When jets are nearly aligned, the value of the precession angle is not well defined, resulting in noisy values. During the MAD state, ﹩\dot{M}﹩ saturates at 2% of ﹩{\dot{M}}_{{\rm{B}}}﹩ (panel a), implying that only 2% of the Bondi accretion rate reaches the BH and the rest, 98%, leaves as outflows.
Paper: Bridging the Bondi and Event Horizon Scales: 3D GRMHD Simulations Reveal X-shaped Radio Galaxy Morphology
Authors: Aretaios Lalakos, Ore Gottlieb, Nicholas Kaaz, Koushik Chatterjee, Matthew Liska, Ian M. Christie, Alexander Tchekhovskoy, Irina Zhuravleva, Elena Nokhrina
Figure caption: The first demonstration that X-shaped radio galaxy morphology naturally emerges from initially axisymmetric conditions: BH and ambient gas initially rotate around the vertical z-axis, with the gas threaded by a vertical magnetic field. Panels (a)–(i) show a time sequence of vertical slices through the simulated density (see color bar). The times and lengths shown in each panel have been scaled to M87*: 0.15 kpc = R B = 103 R g, 475 yr = R B/c = 103 R g/c. The early-time t ≲ 105 R  g /c ∼ 0.05 Myr evolution results in intermittent low-density jets (seen in yellow-green) that are frequently disrupted due to the onslaught of infalling gas and transient reductions in jet power (see also Figure 1). In spite of this, the jets and cavities they inflate manage to reach outside the Bondi radius, which is shown with a black circle. Throughout the simulation, jets and remnant cavities point in different directions and resemble the X-shaped jet morphology in XRGs. The jets stabilize around t ∼ 105 R  g /c ∼ 0.05 Myr, once the BH saturates with the vertical magnetic flux and the disk enters the MAD state: The jets become strong enough to avoid getting deflected by the infalling gas and propagate along the vertical z direction. This ends the short-lived intermittent jet state, whose transient nature can account for the rarity of XRGs.
Paper: First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O III]/Hα Emitter at z = 6.11
Authors: Fengwu Sun, Eiichi Egami, Nor Pirzkal, Marcia Rieke, Martha Boyer, Matteo Correnti, Mario Gennaro, Julien Girard, Thomas P. Greene, Doug Kelly, Anton M. Koekemoer, Jarron Leisenring, Karl Misselt, Nikolay Nikolov, Thomas L. Roellig, John Stansberry, Christina C. Williams, Christopher N. A. Willmer
Figure caption: JWST/NIRCam F322W2 image (top-left; size: 1.″9 × 1.″9), 2D, and 1D spectra (top/bottom-middle/right) of NRCJ1631+3008-z6.1 in the F322W2 and F444W band. Image and 1D spectra were smoothed with a Gaussian kernel of σ = 1 pix (0.″063 or 1 nm) and 2D spectra were smoothed with σ = 2 pix. All spectra were flux-calibrated and background-subtracted. 1D spectra were extracted within D = 7 pix (0.″44) box with aperture correction factors applied (modeled from the profiles of the [O III] λ5007 and Hα  line). Six identified lines (He II λ4686, Hβ, [O III] λλ4959/5007, Hα,  and [N II] λ6583) at z  =  6.112 ± 0.001 are labeled with dark blue lines and highlighted with shallow red shades. 1D error spectra are shown as the gray-shaded regions.