adsabs/AstroCLIMB huggingface dataset:
Paper: A Comparison of Global Magnetofrictional Simulations of the 2015 March 20 Solar Eclipse
Authors: Duncan H. Mackay, L. A. Upton
Figure caption: The PFSS initial condition used for all of the simulations determined from the AFT map at 12 noon on 2014 September 1. The grayscale image shows the radial field at the photosphere, where white/black represents positive/negative flux, where the values saturate at ±50 G. The black lines denote the field lines extending up to the source surface at 2.5R ⊙.
Paper: Turbulent Regimes in Collisions of 3D Alfvén-wave Packets
Authors: S. S. Cerri, T. Passot, D. Laveder, P.-L. Sulem, M. W. Kunz
Figure caption: Left: time-averaged energy spectrum of δ B ⊥ fluctuations and its local slope vs. k ⊥ ℓ 0 for different Lundquist numbers and/or resolutions, at χ 0 ∼ 0.5 (upper spectra, in blue shades and different line styles) and at χ 0 ∼ 0.1 (lower spectra, green/yellow/orange/black colors and different line styles). The Lundquist number S = L 0 v A/η has been varied by changing L 0 at fixed resolution. Two examples of different resolutions at fixed χ 0 ∼ 0.1 exhibit the same behavior (L 0 ≃ 1244ρ i and S ≃ 1.4 × 106, yellow dashed and black dotted lines; L 0 ≃ 1493ρ i and S ≃ 1.7 × 106, green solid and black dashed lines), demonstrating numerical convergence for the chosen dissipation parameters. Right: time-averaged δ B ⊥ spectrum and its local slope vs. k ⊥ ρ i at χ 0 ∼ 0.5 for different combinations of dissipation operators, viz., only Laplacian dissipation (∝k 2, orange dashed line), only eighth-order dissipation ( ∝ k 8, light-blue dashed–three-dotted line), and a combination of both Laplacian and eighth-order dissipation (blue solid line; this corresponds to the purple dashed line in the left panel, i.e., S ≃ 2.8 × 105). This shows that, when a combination of the two operators is employed, our choice of dissipation parameters is such that the tearing-mediated range ﹩\propto {k}_{\perp }^{-11/5}﹩ is due to the usual (i.e., Laplacian) resistivity.
Paper: Turbulent Regimes in Collisions of 3D Alfvén-wave Packets
Authors: S. S. Cerri, T. Passot, D. Laveder, P.-L. Sulem, M. W. Kunz
Figure caption: Left: time evolution of the root-mean-square (rms) current density, J rms (normalized to J 0 = J rms(t = 0); time is normalized to the time of peak activity τ *). The inset reports the (measured) number of collisions ﹩{N}_{\mathrm{int}}^{* }={\tau }_{* }/{\tau }_{\mathrm{int}}=3{\tau }_{* }/{\tau }_{{\rm{A}}}﹩ required to reach the peak of turbulent activity as a function of the initial nonlinearity parameter χ 0, showing that a fully developed turbulent state is achieved on a timescale shorter than the one associated with the usual weak scaling (using the estimate τ * ∼ 3τ nl, dotted line is 9/χ 0; a dashed line ﹩9/{\chi }_{0}^{2}﹩ based on the estimate τ * ∼ 3τ casc is also given for reference). Right: time evolution of the rms Elsässer fields, ﹩{z}_{\mathrm{rms}}^{\pm }﹩ (normalized to ﹩{z}_{0}^{\pm }={z}_{\mathrm{rms}}^{\pm }(t=0)﹩). The inset shows the time evolution of the rms nonlinearity parameter χ rms.
Paper: Turbulent Regimes in Collisions of 3D Alfvén-wave Packets
Authors: S. S. Cerri, T. Passot, D. Laveder, P.-L. Sulem, M. W. Kunz
Figure caption: Isocontours of δ B ⊥/B rms in the x–z plane at y = L 0/2 (left column) and in the x-–y plane at z = L 0/2 (right column), at t/τ * ≃ 1.35 (in the developed turbulent regime) for initial nonlinearity parameter χ 0 ∼ 0.1, ∼ 0.5, and ∼ 1 (from top to bottom). Recall that  B  0 is along z. Insets: isocontours of δ B ⊥/B rms averaged over z (see lagrange.oca.eu/fr/silvio-cerri/3794-animations for animations).
Paper: Turbulent Regimes in Collisions of 3D Alfvén-wave Packets
Authors: S. S. Cerri, T. Passot, D. Laveder, P.-L. Sulem, M. W. Kunz
Figure caption: Variation of the alignment angle with scale for different initial values of the nonlinearity parameter χ 0 and at different times within developed turbulence (0.9 ≲ t/τ * ≲ 1.7): ﹩\sin (\theta )﹩ vs. k ⊥ ρ i at times when AW packets spatially overlap (top row) and when they are far apart (bottom row). Scale-dependent alignment is computed using Equation (4). Relevant power laws are provided for reference.
Paper: Turbulent Regimes in Collisions of 3D Alfvén-wave Packets
Authors: S. S. Cerri, T. Passot, D. Laveder, P.-L. Sulem, M. W. Kunz
Figure caption: Left: δ B ⊥ energy spectrum and its local slope vs. k ⊥ ρ i. Spectra are time-averaged over 0.9 ≲ t/τ * ≲ 1.7. Right: spectral anisotropy k ∥/k ⊥ averaged over the same time interval (k ∥(k ⊥) is obtained using the method presented in Cho et al. (2002)). Relevant power laws are provided for reference.
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Metallicity effect (γ; top left panel), PL scatter (top right panel), and PL intercept (bottom panel) in the W  JK  band as a function of the radius of the SMC region considered. The values are based on the data set and method adopted by Wielgórski et al. (2017). Blue points are the values found in the same conditions as Wielgórski et al. (2017), and green points represent the values obtained after correcting for the SMC geometry (Graczyk et al. 2020).
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Evolution of the metallicity term γ in different filters over time. Open squares indicate the studies in which we identified issues that likely affect the accuracy of the corresponding γ values. The open star in the bottom panel indicates that the present work in W  H  does not include HST photometry for the SMC sample. References: (Ke98) Kennicutt & Stetson (1998), (Sa04) Sakai et al. (2004), (Ma06) Macri et al. (2006), (Sc09) Scowcroft et al. (2009), (R09) Riess et al. (2009), (FM11) Freedman & Madore (2011), (St11) Storm et al. (2011a), (R11) Riess et al. (2011), (Gr13) Groenewegen (2013), (R16) Riess et al. (2016), (Wi17) Wielgórski et al. (2017), (Gi18) Gieren et al. (2018), (Gr18) Groenewegen (2018), (R19) Riess et al. (2019), (Ri20) Ripepi et al. (2020), (Ri21) Ripepi et al. (2021), (R22) Riess et al. (2022), (Br21) Breuval et al. (2021), (Br22) present work. The dashed colored line represents the prediction of γ from Anderson et al. (2016) using Geneva evolution models including the effects of rotation.
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Metallicity effect predicted by Anderson et al. (2016) using the Geneva evolution models including rotation.
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Metallicity effect (γ) as a function of the inverse of wavelength (1/λ) in the hypothesis of a more metal-poor SMC sample of −0.90 ± 0.05 dex (see discussion in Section 5.4).
Paper: An Improved Calibration of the Wavelength Dependence of Metallicity on the Cepheid Leavitt Law
Authors: Louise Breuval, Adam G. Riess, Pierre Kervella, Richard I. Anderson, Martino Romaniello
Figure caption: Metallicity effect (γ) as a function of the inverse of wavelength (1/λ).
Paper: Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants
Authors: Ben Margalit, Adam S. Jermyn, Brian D. Metzger, Luke F. Roberts, Eliot Quataert
Figure caption: Evolution in the space of mass and angular momentum of the (assumed solid-body rotating) core of a BNS merger remnant under the action of accretion from a surrounding Keplerian envelope–disk. Solid black curves bound the parameter space in which solid-body rotating equilibrium neutron star solutions are viable, as set by the maximum mass supported against gravitational collapse ﹩{M}_{\max }(J)﹩ (top curve) and the mass-shedding limit M Kep(J) (right curve), for an SLy EOS (where M TOV = 2.04M ⊙). A black triangle denotes the total remnant mass M tot and angular momentum J tot in an illustrative case residing in the traditionally considered SMNS regime (M TOV < M tot ≲ 1.2M TOV). Stars show three examples of the initial post-merger core properties that exhibit qualitatively distinct evolution. Over disk viscous timescales, mass and angular momentum are accreted onto the core, causing it to move up the trajectory illustrated by the appropriately colored solid curves. Case (B) accretes until reaching M = M tot, while case (A) first hits the mass-shedding curve and hence is rotating near breakup when reaching M = M tot. In both cases (A) and (B), the remnant will only collapse to a black hole once disk accretion has ceased and angular momentum is lost at roughly fixed mass over longer timescales, e.g., via magnetic spindown (left along the dotted lines). By contrast, in case (C), collapse occurs during the core accretion process itself, bypassing the spindown process and resulting in very little rotational energy deposited into the remnant environment. Such an accretion-induced collapse outcome occurs for initial core properties ﹩\{{M}_{\mathrm{core}},{J}_{\mathrm{core}}\}﹩ above the critical curve M AIC(J) (dotted–dashed black curve; approximately given by Equation (21)). A similar curve, M break(J) (dashed-black curve) separates between cores that are spinning at breakup at the end of viscous evolution and those whose rotation rates are lower (as in cases (A), (B), respectively). See text for further details.
Paper: Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants
Authors: Ben Margalit, Adam S. Jermyn, Brian D. Metzger, Luke F. Roberts, Eliot Quataert
Figure caption: Merger remnant outcomes as a function of the total remnant mass M tot normalized to the TOV mass and the fractional initial mass ﹩{M}_{\mathrm{core}}﹩ in the comparatively slowly rotating core. Each panel corresponds to different assumptions about the initial core angular momentum (e.g., ﹩{J}_{\mathrm{core}}=0﹩ and ﹩{J}_{\mathrm{core}}=50 \% ﹩ breakup) and the effective lever arm for adding specific angular momentum to the core (ζ ≡ R acc/R = {1, 2}; Equation (17)) as marked. The three qualitatively different outcomes illustrated by the tracks (A), (B), (C) in Figure 4 are denoted by yellow, blue, and red regions. Remnants formed from massive mergers (large M tot/M TOV) with a large fraction of their mass in a slowly rotating core (large ﹩{M}_{\mathrm{core}}/{M}_{\mathrm{tot}}﹩) collapse as a result of accretion from the envelope–disk (region (C); accretion-induced collapse). By contrast, lower-mass remnants and/or those with smaller cores remain as stable neutron stars even after the entire envelope has been accreted (spindown), whether the core is at that point rotating at breakup (region (A)) or subcritically (region (B)). Solid black contours indicate the extractable rotational energy that can be removed from the remnant into the environment, T ext (e.g., via magnetic spindown; Equation (25)). The black region in the upper right corner is forbidden because cores of mass >﹩{M}_{\max }({J}_{\mathrm{core}})﹩ are dynamically unstable. Black stars denote estimates of ﹩\{{M}_{\mathrm{core}},{M}_{\mathrm{tot}}\}﹩ based on individual numerical relativity BNS merger simulations for several different EOS (SHT, APR4, MS1, and SFHo; from Kastaun et al. 2016; Ciolfi et al. 2017; Kastaun & Ohme 2021, respectively). The calculations in this figure assume ξ = 1.2, η = 0.4, M TOV = 2.1M ⊙, and R = 12 km.
Paper: Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants
Authors: Ben Margalit, Adam S. Jermyn, Brian D. Metzger, Luke F. Roberts, Eliot Quataert
Figure caption: Timescale for angular-momentum transport t visc (Equation (3)) within a PNS remnant formed from the core collapse of a rotating massive star as a function of radius at several snapshots in time measured from core bounce, as marked above each plot. The imposed angular-velocity profile Ω(r) is shown as a solid black curve in the top panel of each snapshot, and can be compared to the Keplerian angular velocity ΩK (dotted black). We assume that ﹩{\rm{\Omega }}(r)=(2\pi /2\,{\rm{s}})/\left[1+(r/1000\,\mathrm{km})\right]﹩ in the iron core prior to collapse and that specific angular momentum is conserved on mass shells during collapse. We show viscous times separately for each of the angular-momentum transport processes we consider in Section 2.2: neutrino viscosity (blue; limited to optically thick regions), MRI (yellow), convection (red), and the TS dynamo (green; solid—nominal case adopting the Fuller et al. 2019 saturation condition; dotted—using the Spruit 2002 saturation prescription instead). The total viscous time arising from the sum of the viscosities is shown with the solid gray curve. The total viscous time is shorter than the PNS’s thermal timescale ≳ its age ∼t (horizontal dashed gray curve), suggesting that the object quickly comes into solid-body rotation.
Paper: Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants
Authors: Ben Margalit, Adam S. Jermyn, Brian D. Metzger, Luke F. Roberts, Eliot Quataert
Figure caption: Schematic of BNS merger remnants as considered in this work. The rotational profile of post-merger remnants has been found by numerical relativity simulations to be qualitatively similar to that shown above. Black dashed curves show the profile reported by Kastaun & Ohme (2021; after removing the frame-dragging effect), and the solid-red curve shows the analytic approximation employed in generating Figure 3 (Equation (2)). The system can be thought of as composed of an initially slowly rotating core at small radii that is surrounded by a ∼centrifugally supported envelope–disk at larger distances. The mass contained within the core, ﹩{M}_{\mathrm{core}}﹩, is typically a large fraction of the total merger remnant mass M tot (with current numerical relativity merger simulations suggesting ﹩{M}_{\mathrm{core}}/{M}_{\mathrm{tot}}\sim 0.8﹩).
Paper: Angular-momentum Transport in Proto-neutron Stars and the Fate of Neutron Star Merger Remnants
Authors: Ben Margalit, Adam S. Jermyn, Brian D. Metzger, Luke F. Roberts, Eliot Quataert
Figure caption: Same as Figure 3, but calculated for an imposed angular-velocity profile appropriate to a BNS merger remnant (Equation (2)).
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: uKLD measures the action-space clustering for streams in the simulations m12i (left) and m12f (right) from 6.8–13.8 Gyr. The two semi-TI models (orange and green) have systematically higher uKLD (a few nats) than the time-evolving model (blue) until all the stellar streams have formed. While the completely TI model (red) has the lowest uKLD. Discrete jumps in the uKLD are due to the formation of each new stream by tidal disruption; individual formation times are marked with gray vertical lines. While all the models produce a highly clustered action space around the present day, a drop in uKLD, indicating less action-space clustering, can be clearly seen for m12f during both the mergers (purple line and purple shaded region). The prolonged merger in m12f is marked using a vertical purple band with the shading reflecting the proximity of the satellite to the Galactic Center (darker shades indicate smaller pericenter distance). The degree of clustering, and hence the accuracy of the potential model, decreases as the merging halo approaches the main halo. Figure 3 shows the exact pericenter distances for the two mergers in this simulation.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Absolute value of amplitude ∣Φ ℓ,m ∣ as defined in Equation (5) (color bar) at all radii as a function of time for the TEMP model for all the simulations. The TMR of these halos can be found in Table 1. The pericenter positions of the merging satellites are shown in red and purple in m12f (middle) and m12w (bottom). Due to axisymmetry, only the even poles exist with m = 0 components. Amplitude decreases as a function power law of radius with index ∼−0.5 for the zeroth pole, which has all the information of the total mass of the halo. Higher poles have relatively low and uniformly distributed amplitude for m12i (top). In m12f and m12w, the pericenter position of the merging satellites (red and purple) strongly coincides with the radial locations with higher amplitude in the spectrum for the duration of the mergers for ℓ = 2, 4. This strongly suggests that even with axisymmetry constraints, the TEMP model with higher poles does well in modeling a dual COM system such as merging satellites.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Action-space (J  r  vs. J  z ) of stellar streams present in m12i for all the models (labeled on the top left) at two time steps, 13.8 and 8 Gyr, respectively. The complete time-evolving action-space videos are posted for all the models and simulations. The actions stay relatively consistent and clustered at both time steps for all the models. Although the semi-TI model produces higher clustering at 8 Gyr, which is due to the (mass ratio <1) scaling at earlier time steps.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Action space (J  r  vs. J  z ) of stellar streams present in m12i (row 1) and m12f (row 2) found using the TEMP model. The three columns represent the time before the merger, during the merger, and after the merger in m12f at 10.52, 10.82, and 12.64 Gyr, respectively. During the merger, the clustering of actions decreases in m12f (middle column). After the merger, the actions have been modified after the interaction (in m12f) and never retain their original values. While m12i has no such loss of clustering and instability in action space throughout different time frames. Note that a new stream forms in the third frame for both m12i and m12f. The complete time-evolving action-space videos are posted at https://drive.google.com/drive/folders/1t2dLAQx4X5H7WOrUhX9nyrf2_pdgD2ga?usp=sharing for all the models and simulations.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: nKLD measures the stability of action space as a function of time for the simulations m12i (left) and m12f (right). For the TI models we compare the action-space distribution at each snapshot to the present-day action-space distribution, while for the TEMP model we compare the action-space distributions of neighboring snapshots in time. For the TI models, the action space is completely decoherent (the nKLD is saturated) before 2.8 Gyr. For comparison, the shaded horizontal bands show the 95% range of MI computed for individual streams using the TEMP model (blue) and TI model (green), respectively. The time where our KLD value first exceeds the MI range, corresponding to an information loss equivalent to an entire stellar stream, is shown with a red dashed vertical line.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Known stellar streams in action space (J  r –J  ϕ  and J  z –J  ϕ ) for m12i (left), m12f (center), and m12w (right) at the present day computed using an order 4 multipole potential expansion assuming axisymmetry (TEMP). The top right corner in the first row plots the positions (Z–X) for these streams. Note the clustering of streams in the action space as compared to their position space. The color bar at the bottom lists the mass of each stream in solar masses starting from lowest to highest. A higher mass order in the streams leads to less clustering in the action space. Also, the different number of streams in each simulation, m12i and m12f, have nine and eight streams, respectively, and m12w only has two.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Fraction of stars in the three simulations with defined actions, as a function of time in the TEMP model. The fraction is described by the total number of stars that have defined actions calculated using the TEMP model over the total number of stars bound to the main halo (E ≤ 0). Note that for m12i (top) and m12f (middle), almost all of the stars have well-defined actions. While for m12w (bottom), about 20% of stars do not have well-defined actions around the merger at 7.95 Gyr.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: Spatial distribution of stars in the Z–X plane at 7.95 Gyr for m12w. Stars with undefined actions belonging to the main halo are shown in magenta and those belonging to the perturber are shown in yellow. All of these stars are in bound orbits around the main halo with E ≤ 0 and in close proximity to the perturbing satellite.
Paper: On the Stability of Tidal Streams in Action Space
Authors: Arpit Arora, Robyn E. Sanderson, Nondh Panithanpaisal, Emily C. Cunningham, Andrew Wetzel, Nicolás Garavito-Camargo
Figure caption: The three Cartesian accelerations (green) of the COM position along with the spline accelerations (black) calculated using the smooth cubic spline fits for each coordinate axis for m12i. The actual acceleration is jittery, highly oscillatory, and large while the spline values are significantly smooth and lower in comparison. The spline fit COM positions do not adversely affect the action space with fictitious forces arising due to jittery COM and only depend on the potential model.
Paper: Exploring Stellar and Ionized Gas Noncircular Motions in Barred Galaxies with MUSE
Authors: Carlos López-Cobá, Sebastián F. Sánchez, Lihwai Lin, Joseph P. Anderson, Kai-Yang Lin, Irene Cruz-González, L. Galbany, Jorge K. Barrera-Ballesteros
Figure caption: Top panel: ESO476-16 DES-z image. The yellow contours represent the isophotes. Bottom panel: radial variation of the disk position angle and ellipticity of the isophotes. The vertical red line shows the approximate length and position angle of the bar, estimated to ﹩r{{\prime} }_{\mathrm{bar}}\sim 9\buildrel{\prime\prime}\over{.} 5\pm 1\buildrel{\prime\prime}\over{.} 5﹩ and ϕ = 114° ± 3°, respectively. The red shadow region represents the bar length standard deviation. The green line on top of the continuum image represents these values. The galaxy is oriented north–east with north pointing up and east to the left.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: Moment 1 and moment 2 maps for 13CO. The MSX sources, two in S112 and another in Clump B, are overlaid with cross symbols.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: Moment 1 and moment 2 maps for C18O.
Paper: Star and Cluster Formation in the Sh2-112 Filamentary Cloud Complex
Authors: Alik Panja, Yan Sun, Wen Ping Chen, Soumen Mondal
Figure caption: (a) Excitation temperature map for 12CO; optical depths for (b) 13CO and for (c) C18O.