adsabs/AstroCLIMB huggingface dataset:
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Upper: the extragalactic RM map of Hutschenreuter et al. (2022) in orthographic projection, centered on the Galactic poles. The left panel shows the northern hemisphere, the right panel shows the south, with circles of constant latitude at b = ±30° and ±60°. Lower: the spherical harmonic expansion of the Hutschenreuter et al. (2022) RM distribution with ﹩{l}_{\max }=3﹩. We overlay the positions of nearby radio continuum loops (Vidal et al. 2015) and label the Galactic quadrants by Roman numerals on both panels. As these are images of the sky, parity is reversed compared with the ordinary face-on view of the Galactic plane seen from above the northern hemisphere.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Scatter plots between rotation measures (RM) of Galactic pulsars with 10° < ∣b∣ < 50° taken from the ATNF catalog and RMs of extragalactic sources from Hutschenreuter et al. (2022). The scatter plots are organized by distance (D, left panel) and height above and below the Galactic plane (∣z∣, right panel). On the right panel, there is a tight correlation for pulsars with ∣z∣ > 0.6 kpc, as indicated by the Pearson coefficients, R, shown along with the number of pulsars in each sample, N, and the slope of the best-fit line, which approaches 1 as z increases. These numbers are summarized in Table 4. The pulsar RMs are very precisely measured; in most cases, the error bars are smaller than the symbols. The errors in the extragalactic RMs are the standard deviations in the Hutschenreuter et al. (2022) map at the positions of the pulsars.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Simulated RM maps showing the M = 0 and M = 1 modes, each with ± dipolar and quadrupolar symmetry. The two top rows show these modes individually. The lower rows show all 16 combinations thereof. The case of −M0 dipolar added to −M1 quadrupolar, in the fourth row and rightmost column, is reproduced in Figure 19.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Correlation between the average LoS magnetic field, 〈B ∥〉, and ∣z∣ for our selected 54 pulsars. Four analytical trends of the form ﹩\langle {B}_{\parallel }\rangle =\langle {B}_{\parallel },0\rangle {e}^{(-| z| /{h}_{B})}﹩ are overlaid as functions of the magnetic field scale height, h  B . As in Figure 11, the points are scattered over a wide range, but they are mostly consistent with h  B  < ∼ 0.5 kpc.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: The upper panels show Stokes I emission at 408 MHz (destriped; Haslam et al. 1982; Remazeilles et al. 2015). The lower panels show the Hα emission from SHASSA, VTSS, and WHAM (Finkbeiner 2003). Alignment and overlays are the same as Figure 15.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Dispersion measure (DM) as a function of ∣z∣ for our selected 54 pulsars. Estimated trends from the literature are listed in the legend with corresponding values of the scale height of the ionized gas in the Milky Way h  e . Although the points show large scatter, the data are consistent with estimates for h  e  in the range 1.0–1.8 kpc.
Paper: Structure in the Magnetic Field of the Milky Way Disk and Halo Traced by Faraday Rotation
Authors: John M. Dickey, Jennifer West, Alec J. M. Thomson, T. L. Landecker, A. Bracco, E. Carretti, J. L. Han, A. S. Hill, Y. K. Ma, S. A. Mao, A. Ordog, Jo-Anne C. Brown, K. A. Douglas, A. Erceg, V. Jelić, R. Kothes, M. Wolleben
Figure caption: Rotation measure vs. longitude for pulsars with latitudes +25° ≤ b ≤ + 45° and z > 0.3 kpc (upper panel) or − 25° ≥ b ≥ − 45° and z < − 0.3 kpc (lower panel). For comparison, the Equation (1) predictions using the extragalactic fit parameters (Table 1) are indicated by the dashed curves. Many of the pulsars have such precisely measured RMs that the error bars are smaller than the symbols. In both hemispheres, the agreement between the extragalactic RMs and the pulsar RMs is very good, particularly for pulsars with ∣z∣ > 0.6 kpc.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: (a) Comparison of average initial 60Fe/56Fe ratios calculated from our CC (left panel), and NC (center panel) data, as well as the entire data set (right panel). Weighted linear regressions [1]–[5] were performed for each data set (indicated above or below each panel) similarly. [1] Regression based on all data of the given data set (Table 5), without consideration of correlations between uncertainties. [2] Regression based on data of the given data set minus the anomalous outliers discussed in Section 5.3, without considering correlations between uncertainties. [3] Regression of all data of the given data set after normalization of 60Ni/62Ni ratios to the average 60Ni/62Ni ratios of nickel-rich targets (56Fe/62Ni ratios <20,000) from the entire data set (i.e., not only from the data set for which the linear regression result is displayed). Correlations of uncertainties are again disregarded. [4] Regression based on all data of the given data set, with the effect of correlated uncertainties removed. [5] Regression based on data of the given data set minus the anomalous outliers discussed in Section 5.3, with the effect of correlated uncertainties removed. Thin black line with a light yellow band: initial 60Fe/56Fe of IVB iron meteorite precursors (CC isotope reservoir) according to Steele et al. (2012), with 1σ uncertainty. Thick blue line: 60Fe/56FeCCAI ratio estimated by Tang & Dauphas (2015) (mostly) from quenched angrites, eucrites, and UOC chondrules (NC isotope reservoir). Line thickness was adjusted to cover ±1σ uncertainty. Gray band: uncertainty of the initial 60Fe/56Fe estimate of Kodolányi et al. (2022) calculated from CC and NC troilite compositions. The displayed initial 60Fe/56Fe estimates of Tang & Dauphas (2015) and Kodolányi et al. (2022) overlap. (b) The same as (a) but with an additional data point in each panel (colored and black symbols), which correspond to the average 60Fe/56Fe ratios of the given isotope reservoir at the formation of CCAIs (60Fe/56FeCCAI ratios). These ratios were calculated from the results of regressions [5], using the average age of chondrules in the given isotope reservoir. The average age for the right panel was calculated by mixing the weighted average 26Al/27Al ratios calculated for CC and NC chondrules (see Section 5.6) in a 56:30 ratio (i.e., in the ratio of our nickel isotope data in Table 5 after the removal of the anomalous 60Ni/62Ni ratios discussed in Section 5.3), and using this average to derive an average age relative to CCAI formation (2.10 ± 0.01 Myr).
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption:  56Fe/62Ni and 60Ni/62Ni ratios of chondrule silicates from the present study and the literature (Mishra & Goswami 2014 Mishra & Chaussidon 2014; Mishra et al. 2016; Telus et al. 2018). (a) The entire compositional range. (b) Data with 56Fe/62Ni ≤ 340,000. Green arrows point at data points that are discussed in detail in Section 5.3 For data from the present study, 56Fe/62Ni ratios were calculated from 54Fe/62Ni ratios, assuming terrestrial iron isotope ratios, and error bars represent ±1σ. 56Fe/62Ni ratios from the literature were either reported as such in the original publications, or were recalculated from reported 56Fe/61Ni ratios (again under the assumption that iron isotope ratios were terrestrial), and error bars were omitted for legibility. Solid black lines (labeled “M&G14 Ch8” and/or “1”) show the relationship between the 56Fe/62Ni and 60Ni/62Ni ratios expected for objects having the same initial 60Fe/56Fe ratios as that inferred for chondrule “8” from Semarkona by Mishra & Goswami (2014), 11.2 × 10−7. Gray dotted lines (labeled “M16 Ch 5” and/or “2”) show the same when calculated from the initial 60Fe/56Fe ratio of chondrule “Ch 5” from QUE 97008 (6.6 × 10−7) inferred by Mishra et al. (2016). Finally, black short-dashed lines (labeled “T18 BM80 Ch13” and/or “3”) correspond to 60Ni/62Ni versus 56Fe/62Ni ratios expected for objects having an initial 60Fe/56Fe ratio of 4.9 × 10−7, inferred by Telus et al. (2018) for Bishunpur chondrule “BM80 Ch13”. “Chond”. in the legend stands for chondrule.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: Texture and phase assemblage of chondrule b9 from QUE 97008. Abbreviations are the same as in Figure 1, with the following additions: M = iron-nickel metal, MI = melt inclusion. (a) BSE image of the entire chondrule with the areas shown in (b) and (c) indicated by yellow dotted rectangles. White arrows point at the boundary between areas with nonporous and porous textures (see also (b)). (b) BSE image of a detail of the chondrule, with the red line indicating the location of the FIB slice lifted out from the boundary between material with nonporous and porous textures (the boundary is again marked with white arrows). (c) BSE image of another detail of the chondrule, that shows the analysis points of the present study (10 sample and two dynamic background measurements, all marked with white arrowheads) and one from the study by Telus et al. (2018 large circular pit). All of the points are in the nonporous part of the chondrule. (d) HAADF image of the FIB slice from the boundary between nonporous and porous chondrule parts. White dotted curve is the approximate trace of the actual boundary. The thin section’s surface was toward the right. (e) HAADF image and composite element maps of a detail of the FIB slice shown in (d). Nonporous texture. (f) HAADF image and composite element maps of a detail of the FIB slice shown in (d). Porous texture.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: Texture and phase assemblage of chondrule b49 from DOM 08006. Abbreviations are the same as in Figure 1, with the following additions: Ap = apatite, Chr = chromite. (a) BSE image of the entire chondrule fragment with the area shown in (b) indicated by a yellow dotted rectangle. (b) BSE image of a chondrule detail. The location where the FIB slice shown in (d–h) was lifted out is indicated by a red line. Yellow dotted rectangle shows the area displayed in (c). (c) Composite iron-sulfur–silicon element map of the area indicated in (b). Notice the association of ∼1 μm bright yellow iron-sulfide (Fe-sul) grains with red iron-oxide (Fe-ox) grains of about the same or smaller size. (d) Brightfield image of the FIB slice lifted out of the chondrule (see (b) for the exact location). Yellow and red dotted rectangles indicate the areas depicted in (e) and (f)–(h), respectively. (e) Brightfield image of a detail of the FIB slice, with the SAED pattern of the silicate mesostasis in the inset. (f) Composite iron-sulfur–oxygen element map of the area shown in (e). (g) Composite calcium–phosphorous–chromium–silicon element map of the area shown in (e). Cyan arrows indicate what are presumably melt inclusions. (h) HAADF image of the area shown in (e). Again, cyan arrows indicate what are presumably melt inclusions.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: Chemical and mineral zoning in chondrules. Abbreviations are the same as in Figure 1, and as follows: Tro = troilite, Pn = pentlandite. (a) BSE image of chondrule b47 from DOM 08006. The chondrule outline is marked with a white stippled curve (b). Magnesium element map of the chondrule displayed in (a). Brightness scales with magnesium concentration. Diffuse magnesium zoning characterizes all olivine crystals, with crystal cores being richer in magnesium than rims, but due to differences in the position of the thin section’s plane relative to the true cores of the crosscut olivine crystals, only a few show magnesium zoning strong enough to be clearly visible in the map (white arrows). (c) BSE image of chondrule b1 from NWA 8276. Chondrule outline is marked with a white stippled curve. (d) Composite aluminum–magnesium–silicon element map of the chondrule displayed in (c). Olivine forms large masses which are surrounded by enstatite. (e) Calcium-aluminum-silicon element map of a detail of the chondrule displayed in (c) and (d). Olivine is surrounded by enstatite. Calcium-rich pyroxene lines the boundary between enstatite and the mesostasis, and occurs in the mesostasis as well.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: Veins in chondrule b1 of MET 00526. Abbreviations are the same as in Figure 1. (a) Aluminum–magnesium–silicon element map of the entire chondrule. (b)–(d) and (e)–(g) show element maps of two different areas within the chondrule displayed in (a). Both areas have a dense network of iron-rich veins, while their nickel distributions are markedly different. (h) BSE image of a third detail of the chondrule, with NanoSIMS analysis pits (see also Figure 1). Yellow line shows the trace of the FIB slice shown in (i) and (j). Red arrow points at the vein also highlighted by red arrows in (i). (i) HAADF image of the FIB slice cut along the yellow line in (h). The high-Z material filling the NanoSIMS pit is platinum from the FIB sample preparation. (j) Nickel–sodium–iron element map combined with the HAADF image of a detail of the FIB slice shown in (i). Notice the partial decoupling of nickel and iron in the major, thick vein on the left-hand side of the image, and the sodium-rich satellite veinlets.
Paper: Topological Modes in Stellar Oscillations
Authors: Armand Leclerc, Guillaume Laibe, Pierre Delplace, Antoine Venaille, Nicolas Perez
Figure caption: Profiles of S for four different typical stellar objects. N is plotted for comparison. Solid orange line indicates the region where the topological mode is trapped, as measured by the trapping length ﹩{ \mathcal L }﹩ defined by Equation (25). Stellar interiors are computed with MESA. The high-mass star is an M = 100 M ⊙ main-sequence star. The white dwarf mass is 0.6 M ⊙, during its cooling phase. The Jupiter model has a solid core of 10 Earth masses. S cancels always at least once, whether in the radiative or convective region. Light gray area indicates the convective zone.
Paper: The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: János Kodolányi, Peter Hoppe, Christian Vollmer, Jasper Berndt, Maren Müller
Figure caption: Comparison of EDX and EPMA data (with 1σ measurement uncertainties) in an olivine from DOM 08006 (BSE image; white dots represent the analysis spots). Ol = olivine. FeOtotal = all iron reported as FeO.
Paper: H1821+643: The Most X-Ray and Infrared Luminous Active Galactic Nucleus (AGN) in the Swift/BAT Survey in the Process of Rapid Stellar and Supermassive Black Hole Mass Assembly
Authors: Hikaru Fukuchi, Kohei Ichikawa, Masayuki Akiyama, Claudio Ricci, Sunmyon Chon, Mitsuru Kokubo, Ang Liu, Takuya Hashimoto, Takuma Izumi
Figure caption: (Left) Luminosity of the 70 month Swift/BAT AGN sample as a function of redshift at z < 0.4. H1821+643 is shown with the star (orange). The 14–150 keV luminosity is taken from Ricci et al. (2017a). (Right) 14–150 keV luminosity and the total infrared luminosities (1–1000 μm) taken from Ichikawa et al. (2019).
Paper: H1821+643: The Most X-Ray and Infrared Luminous Active Galactic Nucleus (AGN) in the Swift/BAT Survey in the Process of Rapid Stellar and Supermassive Black Hole Mass Assembly
Authors: Hikaru Fukuchi, Kohei Ichikawa, Masayuki Akiyama, Claudio Ricci, Sunmyon Chon, Mitsuru Kokubo, Ang Liu, Takuya Hashimoto, Takuma Izumi
Figure caption: SED-fitting result of H1821. The filled points are the photometric data, and the symbols are same as in Figure 2. The red dotted line represents the AGN direct and dust emission. The blue solid line represents the dust emission from the host galaxy. The yellow line represents the stellar emission from the host galaxy, and the green dashed line represents the intrinsic stellar emission. The black solid line is the combined one of dust, stellar, nebular, and AGN.
Paper: H1821+643: The Most X-Ray and Infrared Luminous Active Galactic Nucleus (AGN) in the Swift/BAT Survey in the Process of Rapid Stellar and Supermassive Black Hole Mass Assembly
Authors: Hikaru Fukuchi, Kohei Ichikawa, Masayuki Akiyama, Claudio Ricci, Sunmyon Chon, Mitsuru Kokubo, Ang Liu, Takuya Hashimoto, Takuma Izumi
Figure caption: UV, optical, and IR SED of H1821+643 with the Spitzer/IRS spectrum at 9–35 μm. The different symbol represents the photometric data taken from different satellites or instruments.
Paper: Mode Mixing and Rotational Splittings. I. Near-degeneracy Effects Revisited
Authors: J. M. Joel Ong, 加冕 王, Lisa Bugnet, Sarbani Basu
Figure caption: Mixed-mode rotational splittings as a function of Ω, for quadrupole modes in the same red giant model used for Figure 3. Retrograde sectoral modes are shown in blue, prograde sectoral modes in orange, and zonal modes in gray. Mixed modes are shown with solid lines, while the uncoupled p- and g-modes (and their splittings) are shown with the dashed and dotted lines in the background, respectively. Note the avoided crossings in the solid lines near where dotted and dashed lines of the same color cross.
Paper: Mode Mixing and Rotational Splittings. I. Near-degeneracy Effects Revisited
Authors: J. M. Joel Ong, 加冕 王, Lisa Bugnet, Sarbani Basu
Figure caption: Scaled off-diagonal elements of the matrix elements R  ij  with respect to two different sets of basis functions for dipole modes. Matrix elements in the natural basis of mixed modes are shown in the left panel, and those in the isolated basis of π- and γ-modes are shown in the right panel. Note that both panels use the same color scale, which is significantly saturated in the left panel in order to show structure in the right panel.
Paper: Mode Mixing and Rotational Splittings. I. Near-degeneracy Effects Revisited
Authors: J. M. Joel Ong, 加冕 王, Lisa Bugnet, Sarbani Basu
Figure caption: Diagonal-dominance discriminant for the mixed, π, and γ dipole-mode rotational matrices (including cross-coupling terms) shown in Figure 3. Modes for which this discriminant exceeds unity, shown with the horizontal dashed line, are most poorly approximated by a diagonal rotation matrix. The π-mode frequencies are shown with the vertical dashed lines.
Paper: Mode Mixing and Rotational Splittings. I. Near-degeneracy Effects Revisited
Authors: J. M. Joel Ong, 加冕 王, Lisa Bugnet, Sarbani Basu
Figure caption: Asymmetry parameters ψ ± as a function of ω  γ /ω  π  for a dipole mixed-mode pair, using parameters supplied from a MESA evolutionary model (Model 1, described later). Values derived using the quadratic approximation of Deheuvels et al. (2017) are shown with the dashed lines, and are in very good agreement with the solutions to the quartic equations.
Paper: Mode Mixing and Rotational Splittings. I. Near-degeneracy Effects Revisited
Authors: J. M. Joel Ong, 加冕 王, Lisa Bugnet, Sarbani Basu
Figure caption: Mixing functions ζ for different azimuthal indices m (solid curves of different colors), computed using inertia ratios with respect to a red giant evolutionary model (Model 2 of the next section) with nontrivial envelope rotation. The dashed lines show the locations of the rotationally split π-modes. The dotted lines connect the inertia ratios of all modes in increasing order of frequency; the resulting curve does not describe a mixing function ζ of the kind used by the construction of Mosser et al. (2015) and subsequent works.
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: Statistical distributions of the stress tensor component, where the values are in units of u 2. Rows: [τ  xx , τ  xy , τ  xz ] components; columns: simulation times at [5.62, 7.55, 9.48] ms. Blue lines: target τ distribution; orange lines: CNN prediction; gray dotted lines: gradient turbulence subgrid model of the form τ  ij  = 1/12Δ2 δ u  ik  δ u  jk , using the Einstein notation, where Δ is the filter width and u is the velocity.
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: Slices presenting the spatial distribution of the 3D stress tensor component at t = 7.55 ms, sampled down to 1163. Left: target τ  xx ; right: PIML prediction of τ  xx . The statistical distribution of the above slices can be found in Figure 6 (first row, second column).
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: The plot presents an unnormalized distribution of P turb as time evolves. P turb is in units of u 2. We compare the performance of our PIML model with the gradient turbulence subgrid model.
Paper: Physics-informed Machine Learning for Modeling Turbulence in Supernovae
Authors: Platon I. Karpov, Chengkun Huang, Iskandar Sitdikov, Chris L. Fryer, Stan Woosley, Ghanshyam Pilania
Figure caption: Prediction of x components of τ at t = 1000 of the JHTDB MHD data set in normalized numerical units. Blue shows the original target data, orange shows the predictions of the CNN or PIML models, for off-diagonal and diagonal terms, respectively, and gray shows the result of the gradient subgrid model, as per Section 3.1.