adsabs/AstroCLIMB huggingface dataset:
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Trajectories of dust cells seen in the a3vf10BR run. Color represents the dust surface density at each dust cell. As mentioned in Figure 4, the dust surface density is larger at a radius where more dust cells gather since our numerical method is based on the Lagrangian cells. There are multiple rings, and the dust surface density of the ring monotonically increases as the ring moves inward. It is important to note that the rings start growing in outer regions that are far from the inner boundary. Therefore, the ring formation near the inner boundary in Figure 9 is not due to a boundary effect.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Dust surface density profiles obtained in the six runs. The color of the markers represents whether secular GI is unstable or not at each radius. As found in Paper I, secular GI operates more easily in the outer region where Toomre’s Q is relatively low.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: The resulting ring structure in the a5vf30BR run. (Top panel) The radial profiles of dust surface density (dark blue line) and dust size a (red line) are shown. (Bottom panel) The radial profiles of the mean drift velocity ﹩\left\langle {v}_{r}\right\rangle ﹩ (black line), the total velocity v  r  (blue dashed line), and the diffusion velocity (gray line) are shown.
Paper: Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks. II. Dust-ring Formation Mediated by Backreaction and Fragmentation
Authors: Ryosuke T. Tominaga, Hidekazu Tanaka, Hiroshi Kobayashi, Shu-ichiro Inutsuka
Figure caption: Cumulative probability distribution of the ring mass in six runs. We conduct another five runs for each parameter set with different initial perturbations to plot these distributions. In most runs, we find that a ring mass of ≃0.5 M ⊕–1.5 M ⊕ is the most frequent.
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: Gas consumption rate of the central galaxy as a function of the cooling rate of ICM, for 104 galaxies, groups, and clusters from McDonald et al. (2018) for comparison with H1821. The cooling rate of H1821 is obtained from Russell et al. (2010, blue filled star) and McDonald et al. (2018, black open star), respectively. The gas consumption rate of ﹩{\dot{M}}_{\mathrm{con}}={\dot{M}}_{\mathrm{BH}}+\mathrm{SFR}﹩ is obtained from our SED-fitting results for H1821. For the other sources, we treat ﹩{\dot{M}}_{\mathrm{con}}=\mathrm{SFR}﹩ (McDonald et al. 2018) because ﹩{\dot{M}}_{\mathrm{con}}﹩ is dominated by SFR, and the availability of ﹩{\dot{M}}_{\mathrm{BH}}﹩ is not complete. Red circles show systems that were found AGN activity based on WISE color, and orange circles indicate systems defined as AGN by SDSS spectra. Note that some systems do not have SDSS spectra, and BCG without AGN means systems that do not show red WISE color and are not defined as AGN based on SDSS spectra or do not have SDSS spectra. Green arrows show upper limits of gas consumption rate by AGN contamination and detection limit. Typical gas consumption rate is 1%–10%, but H1821 consumes ≳100% gas.
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: The relation between SFR and stellar mass (M ⋆) of H1821, plotted as blue star, and the star formation main sequence (MS) at z ∼ 0.3 (Pearson et al. 2018). The lowest SFR of H1821 is estimated using AKARI data for FIR photometry, and the highest stellar mass is the value obtained from HST PSF subtraction method. The shaded area is the expected MS region at z = 0.3 with the scatter of 0.35 dex. Empty circles are the local ULIRGs and one HyLIRG obtained from Kilerci Eser et al. (2014) with redshift 0.050 < z < 0.487 (median is 0.181). The dotted line represents the 10 times above the MS at z = 0.3.
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: Best-SED-fitting results of H1821 for the case of changing the error size with using IRAS and ISO fluxes for FIR data. The filled points are the photometric data, and the symbols are the same as in Figure 2.
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: Same with Figure 7 but using AKARI flux for FIR data.
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) ISO spectra before calibration with S/N > 3. (Right) ISO spectra after calibration using detector 5, whose flux is consistent with the IRAS/PSC 100 μm band flux. The average spectra of the four bins are overplotted with black circles.
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 for (a) dipole and (b) quadrupole modes, for a MESA evolutionary model near the base of the red giant branch (see text for complete description). Markers and lines connecting them show the asymmetry in the mode splitting computed using Equation (16), both with respect to the actual multiplets (orange open circles and lines), as well as for multiplets comprised of the two nearest sectoral modes for each zonal mode (blue markers and lines). Other curves show various estimates for asymmetric multiplet splitting: we show predictions from only second-order Coriolis effects (dotted–dashed black lines), from second-order rotational effects including the centrifugal force (dotted lines), and the upper bound on asymmetric splitting from near-degeneracy effects (Equation (29), black dashed lines). A modified expression for near-degeneracy effects accounting for the dense g-mode spectrum, Equation (44), is shown with the red dashed lines. The locations of the π-modes are shown with vertical dashed lines, to guide the eye.
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: Systematic asymmetry (a) and relative errors (b) induced into pure rotational splitting from multimode coupling, over the course of post-main-sequence evolution, for MESA models with angular momentum transport (see text for description). All quantities are evaluated at ﹩{\nu }_{\max }﹩. Both are shown with respect to ﹩{{ \mathcal N }}_{1}﹩, the number of dipole g-modes per p-mode. Colors show different stellar masses, with different initial conditions (see text for complete description). The shaded regions in (a) show upper limits on the magnetic asymmetry in pure g-mode multiplets in the presence of a fossil magnetic field. We show these limits with respective field strengths of 1 MG (blue zone), 0.3 MG (gray zone), and 0.1 MG (green zone) at Model 1 (﹩{ \mathcal N }\sim 5﹩). (b) shows the relative statistical error associated with an absolute measurement uncertainty of 10 nHz (as in Gehan et al. 2018).
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: Magnetic asymmetries induced on the mixed-mode dipolar multiplets for Model 1 when considering a field of amplitude 1MG, as done in Bugnet et al. (2021). Blue line and points indicate the magnetic perturbation computed on mixed-mode frequencies in the presence of mode coupling, and the orange circle shows the result when mode coupling is not taken into account. The locations of the π-modes are marked out with the vertical dashed lines in both panels. (a) Comparison of multiplet asymmetries computed with only the first-order expressions, vs. those emerging from the full mode-coupling calculations. (b) Differences in ζ between modes with and without accounting for the magnetic field perturbation—these differences are ignored in the first-order construction.
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: Cumulative integrals of different families of rotational inversion kernels associated with dipole modes, all in the same evolved stellar model. (a) Standard inversion kernels computed using Equation (9) with respect to mixed-mode eigenfunctions, as typically used in the literature. These exhibit sensitivity to both the radiative core and to the convective exterior, to differing extents depending on the mixing fraction ζ of the modes under consideration. (b) Rotational kernels from π-mode eigenfunctions. Because dipole π-modes have an interior turning point at ﹩{\nu }_{\max }﹩ exterior to the radiative core, these inversion kernels are essentially insensitive to the core, unlike the mixed-mode kernels. (c) Rotational kernels from γ-mode eigenfunctions. The localization of these kernel functions is such that they decay exponentially outside of the compact radiative core.
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: Relative error ϵ in the rotational width δ ω rot for dipole modes of MESA evolutionary models near (a) the base of the red giant branch and (b) the luminosity bump (see text for complete description). Blue markers show the relative systematic errors in the rotational width compared to predictions using the first-order expressions, which are given in the two-zone model by Equation (3). We also show expressions for this error owing to near-degeneracy effects as predicted from two-mode coupling alone (black dashed lines, Equation (31)), and accounting for the dense forest of g-modes (red dotted lines, Equation (46)). Note that the g-dominated modes have errors with signs opposite to those of the p-dominated modes.
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: Differences between the mixing fraction ζ  m  of multiplet components of different azimuthal orders m versus that of the m = 0 multiplet component, ζ 0, shown as a function of the nonrotating mode frequency for the dipole modes of model 1 (see Figure 6(a)). Vertical dashed lines indicate the locations of the underlying π-modes.
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: The same quantities as shown in Figure 6, computed with respect to dipole modes in a more evolved red giant model (see text for a complete description).
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: Same quantities as Figure 10, but with a magnetic field strength of 0.3 MG.
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: Training loss evolution: the top panel shows the actual loss of the model consisting of combined L 1 and KS loss components; the middle panel shows the L 1 loss component, and the bottom panel shows the KSstat loss component.
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: Evolution of the statistical distribution of the stress tensor component (τ  xy ) in the first half of the simulation (t < 5 ms). These exact checkpoints, nine in total, were used as a target for training the CNN network.
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: Graph of the CNN encoder used in all models for tensor component prediction. The activation function is either LogSigmoid or ShrinkTanh, depending on the tensor component type. Further information can be found in Section 3.3.1
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Hydrogen mass fraction (X), propagation diagrams, and rotational kernels as a function of fractional radius for a 5 M ⊙ SPB star at two different stages of the main-sequence evolution (left = zero-age main sequence, right = mid main sequence). Top: during the main-sequence evolution, the core hydrogen mass fraction has decreased and a chemical gradient been developed that gives rise to the spike in the Brunt–Vaisala frequency shown in blue in the middle right panel. Middle: the blue curve shows the Brunt–Vaisala frequency N, while the Lamb frequency for a dipole mode S  ℓ=1 is shown by the orange curve. The blue and orange shaded regions correspond to the propagation cavity of the g- and dipole p-modes, respectively. Bottom: rotational kernel K  n ℓ (r) for a dipole prograde g-mode of radial order n = −22 (blue), and a (ℓ, m, n) = (1, 1, 5) p-mode (orange) calculated using Equation (3.356) in Aerts et al. (2010). The rotational kernel is made dimensionless by scaling with the stellar radius R. The kernels show that the g-modes mainly probe the rotation profile near the convective core, while the p-modes mainly provide information about the rotation near the stellar surface.
Paper: Saturation Level of Turbulence in Collapsing Gas Clouds
Authors: Sho Higashi, Hajime Susa, Gen Chiaki
Figure caption: The saturation Mach number ﹩{{ \mathcal M }}_{\mathrm{sat}}﹩ vs. γ eff (upper panel), and the ratio of the eddy turnover frequency ω and the absolute value of the Hubble parameter ∣H∣ vs. γ eff (lower panel). The red square, blue cross, and green inverse triangle symbols denote the numerical results for ﹩{{ \mathcal M }}_{0}=0.1﹩, with the seeds A, B, and C, respectively. The blue, orange, and green solid lines in the upper panel are the saturation Mach numbers estimated using Equation (18), which assumes turbulence driving scales a ℓ ∼ L J/2, L J/3, and L J/4, respectively. The black dashed line in the lower panel is obtained from Equation (14).
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Spin parameter as a function of oscillation frequency in the corotating frame of reference. Stars for which inferences were made based on space photometry are shown in the left panel, while stars with ground-based data are shown on the right. For stars with period spacing patterns, the lowest (circle) and highest (triangle) frequency in the period spacing pattern are connected by lines. Open symbols correspond to stars without period spacing patterns. The colors indicate the derived rotation frequencies of the stars. The superinertial regime is indicated by the hatched region, while the light-gray shaded region shows part of the subinertial regime.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: SPB instability strip and the locations of the sample of SPB stars studied in this work for which derived luminosities are available. The shaded region indicates the number of radial orders of degree ℓ = 1, 2 that are expected to be excited in a given region of the HR diagram (Moravveji 2016). Example evolutionary tracks for five initial stellar masses are shown in gray. The dotted–dashed lines indicate the boundaries of the main sequence, and the dashed black line shows the beginning of the β Cephei instability strip. The colors of the data points indicate if the rotational frequency was derived based on space photometry (pink) or ground-based data (gray).
Paper: Saturation Level of Turbulence in Collapsing Gas Clouds
Authors: Sho Higashi, Hajime Susa, Gen Chiaki
Figure caption: The evolutions of the core mean densities as a function of time −t. The solid lines show the numerical results. The dashed lines, which have corresponding colors, denote ρ mean = (α(0)/4π G)t −2, where α(0) are given in Table 2. Note: these values, except for that “with cooling,” γ eff = 1.09, and γ eff = 1.1, are multiplied by factors of x for ease of viewing.
Paper: Saturation Level of Turbulence in Collapsing Gas Clouds
Authors: Sho Higashi, Hajime Susa, Gen Chiaki
Figure caption: The same as Figure 3, but for barotropic models and the model with primordial cooling. The solid curves denote the numerical results for γ eff = 1.09 (red), γ eff = 1.1 (cyan), and the model with radiative cooling (green). The black dashed line is obtained by an analytic estimate (Equation (14) of HSC21).
Paper: Saturation Level of Turbulence in Collapsing Gas Clouds
Authors: Sho Higashi, Hajime Susa, Gen Chiaki
Figure caption: Scatter plot of the energy dissipation rate (﹩={\dot{E}}_{\mathrm{in}}﹩) vs. ﹩{{kv}}_{\mathrm{rms}}^{3}﹩. The different colors correspond to the different γ eff. The solid blue line is obtained by the least squares method. Note: there are no differences of the values among the different γ eff, so the points almost degenerate to a single point for each energy dissipation rate.
Paper: Saturation Level of Turbulence in Collapsing Gas Clouds
Authors: Sho Higashi, Hajime Susa, Gen Chiaki
Figure caption: The temporal evolution of the turbulent velocity in the case with the kinetic energy input rate ﹩{\dot{E}}_{\mathrm{in}}=1﹩. The colors of the curves correspond to each γ eff indicated in the box to the bottom right of the figure. We can see no γ eff dependence.
Paper: Internal Rotation and Inclinations of Slowly Pulsating B Stars: Evidence of Interior Angular Momentum Transport
Authors: May G. Pedersen
Figure caption: Amplitude conversion factors derived using Equation (C2) as a function of effective temperature.
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Upper panel: The DTW of the northern hemispheric sunspot number (quarry data, black color) and the southern hemispheric sunspot number (reference data, red color) are mapped to find the minimum distance between these two sets of data sequences. This mapping is shown more clearly for the first 200 sequences of the data (depicted in the lower panel).
Paper: Temporal Evolutions and Quasiperiodic Variations Present in the Sunspot Number and Group Sunspot Area Data Measured at Kodaikanal Observatory for Solar Cycles 14–24
Authors: Belur Ravindra, Partha Chowdhury, Pratap Chandra Ray, Kumaravel Pichamani
Figure caption: Upper panel: The DTW of the northern hemispheric sunspot area (quarry data, black color) and the southern hemispheric sunspot area (reference data, red color) are mapped to find the minimum distance between these two sets of data sequences. This mapping is shown more clearly for the first 200 sequences of the data (depicted in the lower panel).
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: SNR surface densities from Method 2. Top: GD (blue solid curve) and GD μ=0 profile (red dashed curve). Bottom: MGF (orange solid line), CB98e15 (green dashed–dotted curve), and Sérsic (purple dashed curve). All surface densities are for the case of an exponential correction function. The shaded regions are the lower and upper limits of the similarly colored profiles.
Paper: Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Total number of SNRs estimated using Method 1 (pink bar and red error) and Method 2 (light-blue bars and blue errors). The Method 2 numbers correspond to the model numbers in Table 3. All numbers are calculated over the region 0 kpc < R ≤ 11.5 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 the Wolleben et al. (2021) map of the GMIMS RMs in orthographic projection. The lower panels show the spherical harmonic expansion, as in Figure 15. The radio continuum loops discussed in the text are indicated as in Figure 15. The gray patches are areas where the signal-to-noise is too low to allow calculation of the first moment of the Faraday spectrum.
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: Models for the contribution of the disk to the RMs observed at intermediate latitudes. The left panel shows north latitudes (b = + 40°) and the right panel shows the corresponding south latitudes (b = − 40°). These are computed following the method described in Ma et al. (2020, Section 2.2). The blue and orange curves result from the model of Sun et al. (2008) for the disk component and disk plus halo, respectively. The green curve is the disk component of the Van Eck et al. (2011) model, and the red is the disk component of the model by Jansson & Farrar (2012). The recent model of the halo contribution to RMs of pulsars Xu & Han (2019) is shown in purple for b = ±30° (copied from their Figure 17). For comparison the Equation (1) fits to the extragalactic RMs for similar latitude ranges are shown by the dashed curves. The Xu & Han (2019) halo model matches the models for the GMIMS and extragalactic RMs quite well in both hemispheres, as does the Sun et al. (2008) disk-plus-halo model, but the disk-only models do not fit the RM pattern in the northern hemisphere.