adsabs/AstroCLIMB huggingface dataset:
Paper: Understanding the Duration of Solar and Stellar Flares at Various Wavelengths
Authors: Jeffrey W. Reep, Vladimir S. Airapetian
Figure caption: The cooling behavior of a 100 Mm loop with an expanding cross section (factor of 11 from footpoint to apex) heated by a strong electron beam. Similar to Figure 1. The density remains constant through the radiative cooling phase, so the intensities track the change in ionization fractions.
Paper: Understanding the Duration of Solar and Stellar Flares at Various Wavelengths
Authors: Jeffrey W. Reep, Vladimir S. Airapetian
Figure caption: The evolution of X-ray emission in the four loop simulations described in Figures 1 through 4, from top to bottom, respectively. The left-hand column shows the X-ray spectrum at the time of peak heating (50 s), as the heating decays (75 s), and at the onset of the cooling phase (125 s). The right-hand column shows the irradiance time series in the energy ranges observed by NICER, XMM-Newton, or GOES/XRS (assuming a distance of 1 au).
Paper: Understanding the Duration of Solar and Stellar Flares at Various Wavelengths
Authors: Jeffrey W. Reep, Vladimir S. Airapetian
Figure caption: The cooling behavior of a uniform 100 Mm loop heated by a strong electron beam, with strong turbulent suppression of thermal conduction. Similar to Figure 1. The loop becomes much hotter and less dense than the laminar case, which causes the cooling and draining times to be significantly longer.
Paper: Understanding the Duration of Solar and Stellar Flares at Various Wavelengths
Authors: Jeffrey W. Reep, Vladimir S. Airapetian
Figure caption: Irradiance time series for uniform, laminar loops of total lengths between 25 and 200 Mm. The duration depends strongly on loop length as well as the formation temperature of each spectral line. The intensity spike during the heating period is relatively stronger in longer loops.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: Three-color images of 9″ × 9″ regions around (a) 850.1 and (b) 850.2 constructed from JWST NIRCam imaging, with F090W+F150W as blue, F200W+F277W as green, and F356W+F444W as red. Panels (c) and (e) show ﹩5^{\prime\prime} \times ﹩ 5″ regions using F277W, F356W, and F444W as blue, green, and red and the same filter combination is used in panels (d) and (f), which show views of 850.1 and 850.2 “de-sheared” to correct for the lensing magnification (the scale bar indicates 1 kpc). Panels (a) and (b) also show the SMA 880 μm contours (starting from 2σ in 7σ increments), these unambiguously identify the two submillimeter sources. Note that 850.1 corresponds to an extremely red, highly structured source lying close to a bright, foreground disk galaxy with several fainter sources in close proximity. In contrast, 850.2 is more isolated and appears to be a bluer, disk-like system. The various sources and features discussed in the text are identified on each panel: distinct sources have labels starting with “A,” “B” for potential subcomponents, and “C” for likely emission-line features. The colors and photometric redshifts suggest that “knot” B1 near 850.1 is likely to lie at z < 4.26, while B2 is probably a close/interacting companion seen in projection to 850.1 or a less-obscured component within the galaxy. The photometric-redshift analysis also suggests that A1, A4, and A5 are likely to be cluster members at z ∼ 0.35, while A2 and A3 are probably behind the cluster, but foreground to 850.1 and 850.2.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: The NOEMA 3 mm spectra for 850.1 (left) and 850.2 (right), showing the CO(4–3), [C I](1–0), and CO(5–4) emission lines. The panels are centered on the expected frequencies of the lines at the adopted redshifts for each source from Table 2 and a model fit comprising a Gaussian and a constant continuum level is shown for each line. Both sources have relatively weak [C I] emission compared to their CO(4–3) and CO(5–4). A single Gaussian provided an adequate description of the emission for the lines in 850.1, but all three lines in 850.2 display a dip at the systemic velocity, suggesting a double-peaked profile, with the higher-frequency CO peak close to the redshift derived from the rest-frame UV spectroscopic features. The spectra for 850.2 have been rebinned to 40 MHz per channel, except for the [C I] line, which has been rebinned to 100 MHz per channel (and as a result is shown over a slightly wider frequency window to illustrate the off-line noise).
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: A three-color JWST NIRCam image of a 100″ × 100″ region (north at the top, east to the left) around the z = 0.35 cluster A 1489 (where F090W+F150W is shown as blue, F200W+F277W is green, and F356W+F444W is red). Signal-to-noise contours are shown, representing the SCUBA-2 850 μm emission (starting at 5σ, in 5σ increments, 14.″5 FWHM beam), the SCUBA-2 450 μm emission (3σ and 4σ, 7.″5 FWHM beam), and the NOEMA 3 mm continuum emission (10σ, ∼5″ FWHM beam). Note that 850.1 and 850.2 are the two bright sources visible at 450 μm, 850 μm, and 3 mm to the northeast of the cluster core, which is identified by several bright elliptical galaxies, as well as associated strong lensing features. The counterparts to these sources are unambiguously identified using the higher-resolution SMA 880 μm observations shown in Figure 2.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: The different profiles of the Alfvén speeds used in the analysis are shown by curves of different colors. The constant Alfvén speed profile (shown here by the blue horizontal line) will serve as a comparison basis. Speeds and lengths are given in dimensionless units. The two tanh profiles are symmetric about the midpoint of the inhomogeneity in order to apply periodic boundary conditions to our numerical solver, hence removing the effects of fixed boundaries.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: Left: the variation of the damping length of phase-mixed Alfvén waves in a partially ionized plasma, L  d   P , in terms of the wavelength of the Alfvén waves. Here, and throughout the figures for Section 3, unless otherwise stated, the Alfvén speed profile is given by the sinusoidal profile in Equation (16). Right: the ratio of the damping length of phase-mixed Alfvén waves in fully ionized, L  d   F , and partially ionized, L  d   P , plasmas. The curves obtained for different ionization degrees are shown by different colors.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: The variation of the ionization degree with height based on the AL c7 atmospheric model (Avrett & Loeser 2008; black line) together with the variation of the Spitzer resistivity (green line), Cowling resistivity (red line), and shear viscosity (blue line). These transport coefficients were calculated taking into account the values of the physical parameters given by the AL c7 model.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: An envelope is fitted to the normalized maxima of Alfvén waves in the case of the four Alfvén speed profiles. The particular wavelength used in this figure corresponds to λ ∥ ≈ 400 km and the ionization degree is set to μ = 0.7852.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: The percentage reduction in the wave amplitude after a propagating length of 1 Mm is plotted for various ionization degrees; the Alfvén speed profiles are labeled in the legend. The steepest of the four profiles gives rise to the most effective wave damping, while all waves are damped effectively for ionization degrees close to μ = 0.6381, where the values of viscosity, resistivity, and ambipolar diffusion are at their effective combined maximum. For this figure, we study waves with approximate wavelength λ ∥ ≈ 400 km.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: The variation of the damping length with height above the solar surface ranging from 1000 to 2500 km in the case of the four Alfvén speed profiles (P 1 − P 4) given by Equation (16). The particular wavelength used here corresponds to λ ∥ = 400 km. The overplotted red line shows the ionization degree based on the AL c7 model.
Paper: Coronal Magnetic Field Extrapolation and Topological Analysis of Fine-scale Structures during Solar Flare Precursors
Authors: Wen He, Ju Jing, Haimin Wang, Sushree S. Nayak, Avijeet Prasad
Figure caption: Topological analysis of the field lines corresponding to brightenings P1 and P2 near the vertical slice S1 (location marked in Figures 5 and 6). Panel (a) The distribution of ∣ J ∣/∣ B ∣ in slice S1. The identified field lines corresponding to precursor P1a (magenta), P1b (yellow), P2a (green), and P2b (cyan) are also shown and marked. Panel (b) The same distribution on S1 as in panel (a), but with the corresponding magnetic field line intercepting points in the same colors as the field lines overplotted on the vertical slice S1 and the bottom layer. The intercepting points are also drawn in panels (c) and (d). Panels (c) and (d) show the distributions of the twist number T  w  and the squashing degree Q in slice S1, as indicated by the color bars. For all panels, the B  z  map with the PIL highlighted in white contours is drawn on the bottom layer.
Paper: Coronal Magnetic Field Extrapolation and Topological Analysis of Fine-scale Structures during Solar Flare Precursors
Authors: Wen He, Ju Jing, Haimin Wang, Sushree S. Nayak, Avijeet Prasad
Figure caption: Similar analysis as shown in Figure 9, with the distributions of the corresponding topological parameters on the vertical slice S2. The format is the same as in Figure 9. The same sets of the magnetic field lines and the intersection points with corresponding colors are shown.
Paper: Coronal Magnetic Field Extrapolation and Topological Analysis of Fine-scale Structures during Solar Flare Precursors
Authors: Wen He, Ju Jing, Haimin Wang, Sushree S. Nayak, Avijeet Prasad
Figure caption: The top views of the distributions of (a) the twist number T  w  and (b) the squashing degree Q (in base-10 logarithmic scale) on the bottom boundary. The footpoints for the four groups of field lines illustrated in Figures 5 and 6 are overlaid in different colors: precursor P1a in magenta, P1b in yellow, P2a in green, and P2b in cyan.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: S/Ns for the SFD redshift tomography (cross-correlating with the SDSS references) for different spatial weight maps parameterized by γ shown in different color lines. These analyses repeat what is in the upper (B) panel in Figure 1 while seeking to optimize the bootstrapping-based S/Ns. The main plot shows the per-redshift-bin S/Ns, and the inset shows the total S/Ns summed over redshift for each γ. Since the noise is related to the foreground, we use Galactic H I to set the family of weight maps ﹩\omega (\phi )\propto {N}_{{\rm{H}}\,{\rm\small{I}}}^{\gamma }(\phi )﹩. The case of γ = 0 (yellow line) corresponds to no spatial weighting. An optimal S/N is reached around γ = − 1.5 (thick red line in the main plot), which down-weights regions with a strong foreground. The inset shows that this optimization leads to a factor of 1.8 higher total S/N than that in the no-weighting, γ = 0 case.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: The best-fit weights, or the linear coefficients C  i , for each of the 180 LSS templates (30 bases along the x-axis times six augmented beam sizes along the y-axis). These weights are obtained by requiring the linearly combined map to reproduce all of the detectable tomographic statistics of the CIB in SFD. The top panel sums over the weights for each base set, showing that all of our WISE galaxy samples contribute. The side panel on the right shows the total weight per beam, indicating that those with a beam slightly larger (factor of ﹩\sqrt{2};﹩ third row from the bottom) than SFD contribute the most. The errors in the top and side panels are from end-to-end bootstrapping.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Time evolution of the bar strength A 2 for different indicated Q.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Top panel: rotation curve of the Maclaurin disk in spherical halo potential with mass and scale radius specified in the text. The total rotation curve is represented by the solid line that is decomposed into the contributions from disk potential (dotted line) and halo potential (dotted–dashed line). Bottom panel: rotational frequency in units of Ω0 of the same disk, decomposed into the contributions from both components as in the top panel.
Paper: Dynamical Analysis of the Maclaurin Disk with Velocity Dispersion and Its Influence on the Formation of the Bar
Authors: T. Worrakitpoonpon
Figure caption: Surface density maps in units of Σ0 for Q = 1 (top row) and 1.5 (bottom row) at different indicated times. The progression of time in each row is from left to right.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Comparison between two estimators of angular two-point cross-correlation functions between SFD and the SDSS references in several redshift bins. The left panel uses the usual annulus binning (Equation (5)), while the right uses the differential compensated filter (Equation (12)). The gray dashed line in each panel shows the response to a pure Gaussian kernel of the ﹩6\buildrel{\,\prime}\over{.} 1﹩ SFD beam. This figure shows that the compensated filter (right) leads to cross-amplitudes with a smoother progression from low to high redshifts (no blue lines in the middle of reds) as it is more stable against fluctuating local zero-points due to the strong foreground.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Correlation coefficient matrix for the weights C  i  of the 30 base templates. Anticorrelations (blue) appear when two templates overlap significantly in redshift. Therefore, when one such template is picked in a bootstrap realization, the other one is not needed (e.g., templates ID 2 and 20; see Figure 12 for their redshift distributions). These covariances are fully propagated into the final reconstructed LSS/CIB and the associated error maps.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Pixel value correlation between SFD and the Galactic H I column density map (left panel), the original SFD map (upper right), and the residual SFD map after regressing out the H I–correlated foreground (lower right). As the H I–cleaned SFD, by construction, has a mean close to zero, we add a small offset such that both maps on the right can be plotted over the same logarithmic dynamic range. This plot shows that the H I cleaning is effective in reducing large-scale foreground gradients.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Distance R  f (t  f  = 17.24 ms) from the system center of mass for the surviving tracer particles plotted against their initial distance R  i  from the center of their home NS. Red circles distinguish unbound particles.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Schematic presentation of the different stages and outcomes of BNS mergers: from left to right, inspiral, merger, postmerger remnant plus debris disk, and, possibly, a stable NS. The timescales for each stage are shown below the corresponding sketches. The bottom line lists the GW frequency and the principal physical mechanisms of each stage.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Top: position in the x–y plane of the surviving particles at t = 14.506 ms (blue dots) and at t = 14.705 ms (yellow crosses). The line labeled “l  x ” is fit to the line-like feature in the middle of the “S-”shape at t = 14.50 ms. The red arrows illustrate the x–y velocities of a random sample of surviving particles at t = 14.50 ms; the arrows’ lengths are proportional to the speeds of the particles’ orbital plane motion. Bottom: positions in the l  x  –z plane of the surviving particles in the line-like feature at t = 14.50 ms.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Evolution of the electron fraction, x–y plane mass density, and x–z plane mass density. Y e is shown on a linear color scale (x–y plane), the mass densities on a logarithmic scale. Each quantity is presented at times 14.66 ms, 15.29 ms, and 16.31 ms; the last is shortly after the collapse to a BH. Note that the color scale for Y e at t = 14.66 ms is different from the color scale at the other times.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Motion in (x, y) of three surviving particles (blue, green, and red dotted paths) from t = 12 ms to t = 16.6 ms, when the star collapses to a BH. The black circle shows the outline of their parent star at t = 12 ms. Cusps are the signature of shock deflection.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: The evolution of the separation between six surviving particles and their initial close neighbors. The top panel shows how their y-coordinates evolve, the bottom panel shows the evolution of their x-coordinates. Each pair’s starting location (x, y) is shifted by an arbitrary amount relative to the other pairs so that they can be visually distinguished. In some cases (e.g., the bottom two), the members of the pair start out so close together that their curves are superposed. To contrast the differing trajectories within a pair, it is best to follow the two curves beginning from t = 13 ms; designation of which survives and which does not is made by the arrows near t = 17 ms.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Time dependence of the angular momentum u  ϕ  for our sample of six pairs of particles. Survivors are shown with solid lines, and captured particles with dashed lines; matching colors identify the pairs. The time of collapse to a BH, 16.6 ms is marked with a gray dashed vertical line; for captured particles after that time, the physical significance of u  ϕ  is unclear.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Evolution of the pressure P in the x–y and x–z planes, shown on a logarithmic scale at times 14.50 ms, 14.66 ms, 15.37 ms, and 16.39 ms.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: The x–y locations of the same six surviving particles shown in Figure 4 superposed on the t = 14.50 ms density map. Their z-coordinates are z = 2.558, −2.225, −3.097, 2.182, 1.738, and 3.504 km for the particles shown as a plus sign, a square, a circle, a dot, an “X,” and a caret, respectively.
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Upper panel: the probability that a particle with initial radius R  i  survives BH collapse. M sur and M tot are the masses associated with the surviving and all the tracer particles, respectively. Lower panel: the probability density (in arbitrary units) that a surviving particle had initial radius R  i .
Paper: Bound Debris Expulsion from Neutron Star Merger Remnants
Authors: Yossef Zenati, Julian H. Krolik, Leonardo R. Werneck, Ariadna Murguia-Berthier, Zachariah B. Etienne, Scott C. Noble, Tsvi Piran
Figure caption: Evolution of u  ϕ , the conserved angular momentum component in an axisymmetric spacetime, for a large sample of the survivor tracer particles: 220 particles selected at random. The small number of surviving particles with higher u  ϕ  and noisy u  ϕ  histories during the premerger inspiral (blue, yellow, and purple lines) were initially located very close to the surface of one or the other of the NSs.