adsabs/AstroCLIMB huggingface dataset:
Paper: Impacts of Extreme Ultraviolet Late Phase of the Solar Flare on Ionospheric Electrodynamics
Authors: Xuanqing Liu, Jing Liu, Junjie Chen, Liying Qian, Phillip C. Chamberlin, Yao Chen, Xiangliang Kong, Shuhan Li
Figure caption: Solar flare-induced  E  ×  B  WI (upward positive) at 2.°5E longitude (UT ≈ LT) on the pressure level -4 (∼120 km). First row: WI for the entire flare, no flare, and their differences. Second row: WI for the entire flare, only the ELP, and the differences. Third row: WI with the complete flare impact, only the MP, and their differences. Dashed lines denote the flare onset (11:53 UT) and ELP peak (13:53 UT).
Paper: Impacts of Extreme Ultraviolet Late Phase of the Solar Flare on Ionospheric Electrodynamics
Authors: Xuanqing Liu, Jing Liu, Junjie Chen, Liying Qian, Phillip C. Chamberlin, Yao Chen, Xiangliang Kong, Shuhan Li
Figure caption: Latitude and UT variations of simulated ΔWI under MP (first row) or ELP (second row) effects at local noon. (b)–(c)/(e)–(f): the contributions of MP/ELP response of the conductivity or neutral wind to WI.
Paper: Temporally Resolved Type III Solar Radio Bursts in the Frequency Range 3–13 MHz
Authors: Antonio Vecchio, Milan Maksimovic, Nicolina Chrysaphi, Eduard P. Kontar, Vratislav Krupar
Figure caption: Synthetic light curves at 5 MHz derived as a power-law function between the maximum and the background values from Figure 4 of V. Krupar et al. (2020) with a random noise with a 0.5 dB standard deviation superimposed. The black dashed line corresponds to a power-law fit on these data.
Paper: Temporally Resolved Type III Solar Radio Bursts in the Frequency Range 3–13 MHz
Authors: Antonio Vecchio, Milan Maksimovic, Nicolina Chrysaphi, Eduard P. Kontar, Vratislav Krupar
Figure caption: Histograms of the decay times obtained from the visually selected type III burst subset at the five considered frequencies when the time resolution has been reduced to 3.5 s. Red full lines represent the empirical probability density function estimated using the KDE approach and constructed from the histogram.
Paper: The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST
Authors: Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith, Kelsey E. Johnson
Figure caption: Left: the age and mass for our final sample of 97 Class 0a and 0b clusters. The solid red line represents the F555W 90% completeness limit derived using the LEGUS Cluster Completeness Tool (M  V  = −6.24; S. T. Linden et al. 2022). The goal of this study is to evaluate the population of clusters in M83 with ages less than 10 Myr. Therefore to achieve a mass-limited sample over this entire age range (see F. Renaud 2020) we impose a cut of M > 102.8 M ⊙, which removes an additional 44 sources from the final analysis. Middle: the extinction vs. age for our 53 most massive clusters in M83. The lower-mass sources removed to maintain a mass-complete sample over the first 10 Myr are shown in gray. The solid green curve represents the running mean of the distribution. Our Paβ selection has increased the number of young (t ≤ 3 yr) and dusty (E(B − V) > 0.5) sources by 14 relative to previous studies of M83 (N. Bastian et al. 2012; R. Chandar et al. 2014). Right: the CI vs. age for our 53 most massive clusters in M83. The lower-mass sources removed to maintain a mass-complete sample over the first 10 Myr are again shown in gray. The solid green curve represents the running mean of the distribution. We do not see a significant size evolution over the age range studied here. This result is broadly consistent with J. E. Ryon et al. 2015, who show modest to little evolution of cluster size in the first 10 Myr.
Paper: The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST
Authors: Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith, Kelsey E. Johnson
Figure caption: The three YSCs in our final cluster catalog with the highest SED-derived E(B – V) values. The leftmost panel shows an older source—ID 364—who has age ≥4 Myr, M * ≥ 104.7 M ⊙, and E(B – V) ≥1.4. Although rare within our WFC3 footprint, this source may represent an important population of clusters requiring SN feedback to fully disperse their surrounding gas and dust across the full disk of M83. The middle and right panels show the younger two sources with ages ∼1 Myr, M * ∼ 103.4 M ⊙, and E(B – V) ≥1.4. These very young and heavily extincted sources are the signposts for active feedback into the surrounding ISM.
Paper: The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST
Authors: Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith, Kelsey E. Johnson
Figure caption: The F336W–F435W vs. F555W–F814W color–color diagram for all visually classified Class 0a and 0b clusters (N  = 270—light gray). Overlaid in light blue are the Yggdrasil SSP models adopted here (f cov = 0.5, Kroupa IMF, z = 0.02) to fit cluster ages, masses, and extinctions. The cluster catalog after applying all selection cuts described in Section 2.2 is show in black (97 sources). In red we show the magnitude of an A  V  = 2 extinction vector, demonstrating that our selection method can identify sources with F555W–F814W up to ∼1.5, which are likely heavily dust-enshrouded and missed in previous UV/optical surveys of the star cluster populations in M83.
Paper: JWST Reveals Bulge-dominated Star-forming Galaxies at Cosmic Noon
Authors: Chloë E. Benton, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Justus Gibson, Abigail I Hartley, Marco Martorano, Sedona H. Price, Katherine A. Suess, Arjen van der Wel, Pieter van Dokkum, John R. Weaver, Katherine E. Whitaker
Figure caption: A comparison of the central flux of galaxies in F150W (rest-frame V band; left) vs. F444W (rest-frame J band; right). Σ1 is the flux contained within the central kiloparsec. Here, Σ1 represents central flux surface density instead of stellar mass density. We find that galaxies measured in F444W overall have higher central flux than in F150W.
Paper: The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST
Authors: Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith, Kelsey E. Johnson
Figure caption: False-color red green blue (F814W/F435W/F336W) and F336W/Hα/Paβ images of the central region (bottom) and inner spiral arm (top) in M83. The left panels show UV/optical emission, highlighting the relatively bright, dust-free, and intermediate-age stellar populations in the disk. The right panels focus on optical and NIR hydrogen recombination line emission (Hα and Paβ), highlighting the youngest and most heavily dust-enshrouded stellar clusters. The combination of both broadband and narrowband imaging allow us to robustly identify and characterize these very young sources across M83 for the first time.
Paper: JWST Reveals Bulge-dominated Star-forming Galaxies at Cosmic Noon
Authors: Chloë E. Benton, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Justus Gibson, Abigail I Hartley, Marco Martorano, Sedona H. Price, Katherine A. Suess, Arjen van der Wel, Pieter van Dokkum, John R. Weaver, Katherine E. Whitaker
Figure caption: The average radial brightness profile for star-forming galaxies and quiescent galaxies at filters F150W and F444W. Right: we note that both galaxies have dense cores, with the peaks being at relative magnitudes. Left: at shorter wavelengths, the peak of the star-forming galaxies is a magnitude lower than the quiescent galaxies. This offset is to be expected since we assume the F150W filter to be an inconsistent tracer of stellar mass.
Paper: JWST Reveals Bulge-dominated Star-forming Galaxies at Cosmic Noon
Authors: Chloë E. Benton, Erica J. Nelson, Tim B. Miller, Rachel Bezanson, Justus Gibson, Abigail I Hartley, Marco Martorano, Sedona H. Price, Katherine A. Suess, Arjen van der Wel, Pieter van Dokkum, John R. Weaver, Katherine E. Whitaker
Figure caption: The left panel shows the radial surface brightness profiles of our SFGs given in F150W and F444W. The light colored lines show the surface brightness profiles of individual galaxies of each filter, the dark their median. Overall, F444W has a much steeper surface brightness profile than the F150W. For the right panel, the shaded region represents the uncertainty in the ratio of the averaged profiles. The light colored lines represent the ratio of the filters (F444W/F150W) for each individual profile. As we expect, there is more variation at the outskirts of these galaxies.
Paper: The Clearing Timescale for Infrared-selected Star Clusters in M83 with HST
Authors: Suyash Deshmukh, Sean T. Linden, Daniela Calzetti, Angela Adamo, Matteo Messa, Kathryn Grasha, Elena Sabbi, Linda Smith, Kelsey E. Johnson
Figure caption: Three-color images of representative YSC candidates for each of our four defined classes: 0a, 0b, 1 and 2. All 454 sources were manually classified based on the criteria mentioned in Section 2.2.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The same as Figure A1 but for the central source in Band 7. Since the emission is spatially resolved, the peak intensity and size are not degenerate as in Band 3.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The same as Figure A1 but for the central source in Band 3. Since the emission is smaller than the beam size, the peak intensity and size are degenerate.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The same as Figure 3 but for the radial profiles in the northwest peak direction (left column) and the azimuthally averaged radial profiles in the directions other than the peak (right column). The upper column shows the radial intensity profiles, while the lower column shows the spectral index profiles. The Gaussian in the upper right corner of the upper left panel represents the beam size in the northwest peak direction, and the Gaussian in the upper right corner of the upper right panel shows the major and minor axes of the deprojected beam.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The corner plot of MCMC fitting for the ring of PDS 70 in Band 3. The dashed lines in the uppermost panels of each column show the 16th, 50th, and 84th percentiles of the marginal distributions. The blue lines show the parameters that maximize the joint probability.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The corner plot of the difference in the center position between the ring and the central source in Band 3. It shows that the center of the ring and the central source are consistent.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The same as Figure A5 but in Band 7.
Paper: Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations
Authors: Kiyoaki Doi, 聖明 土井, Akimasa Kataoka, 章雅 片岡, Hauyu Baobab Liu, 浩宇 呂, Tomohiro C. Yoshida, 有宏 吉田, Myriam Benisty, Ruobing Dong, 若冰 董, Yoshihide Yamato, 義英 大和, Jun Hashimoto, 淳 橋本
Figure caption: The same as Figure A1 but in Band 7.
Paper: On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity
Authors: Mason Dorseth, Sofiane Bourouaine, Jean C. Perez
Figure caption: Top left: normalized magnetic PSD ensemble averages of slow wind intervals—imbalanced Alfvénic slow wind (orange), balanced Alfvénic slow wind (blue), and compressible slow wind (green). The black dashed, dashed–dotted, and dotted guidelines are for comparison to a −5/3, −3/2, and −1 power law, respectively. The vertical gray dashed lines show the approximate location of the spectral break at 2 × 10−4 Hz. Top right: normalized velocity PSD for the same ensemble averages. Bottom left: average residual energy and cross helicity of each of the intervals. The dashed circle is the boundary of mathematically possible pairs of values. Bottom right: average compressibility and magnetic compressibility of each of the intervals. The crosses on the bottom two panels correspond to the spectra in Figure 4.
Paper: On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity
Authors: Mason Dorseth, Sofiane Bourouaine, Jean C. Perez
Figure caption: Top left: example of a typical (compressible) slow wind. The interval is 3 days long, starting 2019 May 24, 00:00:00. The top, middle, and bottom panels show the wind speed in the spacecraft frame, the magnetic field components and magnitude, and the number density, respectively. Top right: example of a slow wind interval with balanced Alfvénic turbulence. The interval is 2 days, 12 hr 50 minutes long, starting on 2014 August 13, 00:11:12. Bottom left and right: the normalized PSDs of the magnetic field for the above intervals, respectively. The black dashed and dotted guidelines are for comparison to a −5/3 and −1 power law, respectively.
Paper: On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity
Authors: Mason Dorseth, Sofiane Bourouaine, Jean C. Perez
Figure caption: The start times of all the 1220 intervals created for this study. The homogeneous intervals of the three slow wind types are shown in their respective colors. Black dots represent intervals that do not fall into any of these categories.
Paper: On the 1/f Spectrum in Slow Solar Wind Turbulence: The Role of Alfvénicity
Authors: Mason Dorseth, Sofiane Bourouaine, Jean C. Perez
Figure caption: Normalized magnetic PSD for 3 day subintervals. The dark blue, red, and pink spectra correspond to days 1 to 3, 2.5 to 4.5, and 4 to 6, respectively. The guidelines are the same as those shown in Figure 3.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: Comparison of plasma density distributions for various simulations in the SCLF regime. (a) Small gap l gap ≪ R  PC  with constant curvature (same as used in Figure 2, simulation SCLFsmall from Table 1). Panel (b) shows significant decorrelation of discharges on different field lines for a small gap and artificially reduced repetition rate (simulation SCLFsmallTail). Panel (c) presents the simulation SCLFsmallCurv with the same parameters but with dipolar curvature, ρ  c  ∼ 1/θ. The inset displays the field-aligned component of the electric field, highlighting the inclined fronts of field screening. Panel (d) depicts the case of a large gap, l gap ≲ R  PC  (SCLFlarge). The right column shows plasma currents averaged along the field lines at different times for (e) small and (f) large gaps, indicating that smaller gaps more effectively sustain the twist of the magnetospheric field lines. The dotted red line in panels (e) and (f) shows the distribution of the magnetospheric current density.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: Evolution of the discharge in the 2D polar cap with a small gap, l gap ≪ R  PC , and free particle escape from the stellar surface (SCLF). The first column depicts (a) the electric field and (b) plasma density during the initial phase of the evolution, where patches occupy a large area of the polar cap. At this time, the discharge along the super-GJ field lines behaves in an almost steady-state manner. The second column illustrates a later evolutionary stage when all patches are cleared of the initial plasma, leading to a cyclic discharge. The asymmetry of clouds of produced plasma suggests the decorrelation of discharges on neighboring field lines. Lines “E” and “F” indicate the positions of 1D cuts of the z − p  z  phase space and electric field for the region of the super-GJ current (e1, e2) and (f1, f2)—for return current. In the phase-space plots, blue, red, and black circles represent the position and momentum of electrons, positrons, and pair-producing photons, respectively.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: 3D SCLF discharge in a polar cap of a 60°-inclined rotator with a marginally small gap, l gap < R  PC . Panel (a) shows a volume rendering of the density of a secondary plasma. The plane at the bottom shows the position of the stellar surface, and the color map shows the distribution of the magnetospheric current. The blue lines perpendicular to the stellar surface represent the magnetic field lines. Panels (b) and (c) show the time-averaged distribution of the plasma current. The black dashed line in panel (c) shows the position of the 1D slice in panel (b). The two lower rows show 2D slices of the plasma density (panels (d), (e), (g), and (h)) and electric field (panels (f) and (i)) through the center of the domain in two different projections. The dashed lines in each of the slices show the position of a slice in a perpendicular plane, e.g., the dashed line in panel (d) shows the position of slices in panels (e) and (f). Panels (d)–(f) in the middle row show the initial phase of the simulation, when a lot of patches are still filled with initial plasma, and the lower row (panels (g)–(i)) shows a time when all patches are cleared of the initial plasma. White dashed lines in panel (d) show the boundaries of the initial patches, white shadowed regions show initially inactive patches, and two nonshadowed regions represent initially active patches.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: Distribution of the magnetospheric current across the polar cap used in our (a) 2D and (b) 3D simulations, which mimic the currents in the magnetospheres of aligned and 60°-inclined rotators. The net current across the polar cap is zero, with outgoing and return current regions each covering roughly half of the polar cap. The colored inset in panel (a) marks the boundaries of initial high-density plasma-filled patches (see Section 2.5). In panel (b), the thick black lines represent the boundaries of super-GJ and return current regions.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: Evolution of the discharge in the 2D RS75 polar cap with small (l gap ≪ R  PC , RSsmall) and large (l gap ≲ R  PC , RSlarge) gaps. The first column shows (a) electric field and (b) plasma density distribution during the initial phase of the evolution in RSsmall, when initial patches still occupy a large area of a polar cap. The second column, panels (c)–(d), illustrates a later evolutionary stage when all patches are cleared of the initial plasma. The right column shows (e) the electric field and (f) density snapshots for a large gap, RSlarge, at a later time when the initial patches are cleared of plasma.
Paper: Coherence of Multidimensional Pair Production Discharges in Polar Caps of Pulsars
Authors: Alexander Chernoglazov, Alexander Philippov, Andrey Timokhin
Figure caption: 1D test of the curvature cooling and atmospheric particle injection in the charge-separated SCLF model: the left column shows (a) plasma density, (b) electric field, and (c) phase space z − p  z  for the super-GJ current; the right column shows the same quantities as the left column, but for the sub-GJ current. For the super-GJ current, the phase space plot (panel (c)) shows that electrons initially accelerate in almost vacuum potential (the orange dotted line shows analytical prediction) and later enter into the radiation-reaction-limited regime (indicated by the red dotted–dashed line). In the case of the sub-GJ current, extracted electrons travel at mildly relativistic speeds and maintain a state of small electric field.
Paper: Monster Shocks, Gamma-Ray Bursts, and Black Hole Quasi-normal Modes from Neutron-star Collapse
Authors: Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Close-up of the black hole (black circle) and equatorial current sheet with magnetic field lines (gray) after the collapse of a neutron star with initial rotation ν = 900 Hz. Color shows the azimuthal component E  ϕ  of the electric field normalized to the magnetic field B. The snapshot is taken at time t = 0.67 ms after the onset of collapse.
Paper: Monster Shocks, Gamma-Ray Bursts, and Black Hole Quasi-normal Modes from Neutron-star Collapse
Authors: Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: MHD waves excited in the neutron-star magnetosphere by the collapse. The rotation axis is along z, and the figure shows a cut of the magnetosphere along the plane of y = 0. The black circle at the center is the nascent black hole. Green curves show the magnetic field lines, and color shows E  ϕ /B as measured by the local normal observer. The snapshot is taken at t = 0.67 ms from the onset of collapse.
Paper: Monster Shocks, Gamma-Ray Bursts, and Black Hole Quasi-normal Modes from Neutron-star Collapse
Authors: Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Black hole ring-down of the rapidly rotating configuration, ν = 900 Hz. The ring-down in gravitational waves (GW) and in the electromagnetic field (EM) is shown using the Newman–Penrose scalars ψ 4 (ℓ = m = 2 mode) and ϕ 2 (ℓ = m = 1 mode), respectively. All quantities are measured at a radius r ≈ 75 km.
Paper: Monster Shocks, Gamma-Ray Bursts, and Black Hole Quasi-normal Modes from Neutron-star Collapse
Authors: Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Shock formation and evolution, shown with three snapshots (cuts of the magnetosphere along the vertical plane of y = 0). Color panels show thermal energy density U th (normalized to the magnetic energy density U  B ) at z > 0 and fluid Lorentz factor γ at z < 0. Lower panels show the radial four-velocity u  r  = γ v  r /c measured along two lines in the x–z plane: on the x-axis (polar angle θ = 90°, red) and on the line of θ = 25° (black).