adsabs/AstroCLIMB huggingface dataset:
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Electron temperature shown on the solar surface (R = 1.05 R⊙) at t = 0, 5, 10, 15, and 20 minutes post-eruption. The white lines represent the magnetic field lines in the flux rope.
Paper: Magnetic Field Configuration of a Quiescent Prominence Revealed by Large-amplitude Longitudinal Oscillations in End-view Observations
Authors: Jun Dai, Ayumi Asai, Dechao Song, Ye Qiu, Zhe Xu
Figure caption: Axial direction of the prominence and the velocities of the oscillation. Panel (a) gives an Hα line-center image in 6562.82 Å observed by CHASE on 2023 December 1 at ∼12:00 UT. The blue contour outlines the profile of the prominence when it was on the solar disk. The blue solid dots in panel (b) represent the extracted location of the prominence spine from panel (a), and have been rotated to the center of the solar disk (corresponding to the top view) in the coordinate system. The red dashed and solid lines mark the axial direction of the prominence spine and the LOS direction when they are projected on the disk, respectively. Panel (c) gives a schematic diagram showing the angles between the prominence axis and oscillatory velocities. The gray rectangle represents the POS. POS west, north, and LOS directions are taken as x-, y-, and z-axes. The blue, red, and orange solid arrows indicate the POS velocity, Doppler velocity, and 3D velocity of oscillatory materials, respectively. The Doppler velocity and the prominence axis are coplanar in the red rectangle (Plane A), which is perpendicular to the POS. The angles between the POS velocity and the y-axis and Plane A are marked as β and γ, respectively. α represents the angle between the prominence axis and the direction of the 3D velocity.
Paper: Magnetic Field Configuration of a Quiescent Prominence Revealed by Large-amplitude Longitudinal Oscillations in End-view Observations
Authors: Jun Dai, Ayumi Asai, Dechao Song, Ye Qiu, Zhe Xu
Figure caption: Panels (a1)–(b1): velocity–time plots of VPOS, VLOS, V3D. The values in panel (a1) were obtained from slice CD, while the values in panel (b1) were obtained from the simultaneous POS velocity fields and Dopplergrams of the oscillatory prominence materials. Panels (a2)–(b2): evolution of angle α and local curvature radius of magnetic dip, where the values were estimated from the velocities in panels (a1) and (b1), respectively.
Paper: Magnetic Field Configuration of a Quiescent Prominence Revealed by Large-amplitude Longitudinal Oscillations in End-view Observations
Authors: Jun Dai, Ayumi Asai, Dechao Song, Ye Qiu, Zhe Xu
Figure caption: POS velocity fields and Dopplergrams of the oscillatory prominence. Panels (a1)–(a3) give three EUV images in AIA 171 Å overlaid by simultaneous POS velocity fields of the oscillatory prominence materials. Panels (b1)–(b3) give three Dopplergrams where the black contours outline the profile of oscillatory prominence materials.
Paper: Magnetic Field Configuration of a Quiescent Prominence Revealed by Large-amplitude Longitudinal Oscillations in End-view Observations
Authors: Jun Dai, Ayumi Asai, Dechao Song, Ye Qiu, Zhe Xu
Figure caption: Elevation angle θ and azimuth angle ψ (β in Figure 3 ) of V3D in the right-hand coordinate system.
Paper: Magnetic Field Configuration of a Quiescent Prominence Revealed by Large-amplitude Longitudinal Oscillations in End-view Observations
Authors: Jun Dai, Ayumi Asai, Dechao Song, Ye Qiu, Zhe Xu
Figure caption: 3D geometry of magnetic dips supporting OS2 and OS1 obtained from velocities. POS north, east, and LOS directions are taken as POS y-axis, POS x-axis, and LOS. Blue dotted lines represent the motion trajectories (the geometry of magnetic dips) of OS2 and OS1.
Paper: Identification of Large-scale (>100 kpc) Radio Jets in Narrow-line Seyfert 1 Galaxies
Authors: S. Umayal, Vaidehi S. Paliya, D. J. Saikia, C. S. Stalin, S. Muneer, Maheswar Gopinathan
Figure caption: Distributions of (a) redshift z, (b) bolometric luminosity, and (c) radio-loudness parameter are shown in the upper panels, while those of (d) absolute B magnitude, (e) mass of BHs, and (f) Eddington ratio are shown in the lower panels. The radio-detected NLSy1 sources plotted in gray do not include the >100 kpc NLSy1s.
Paper: Identification of Large-scale (>100 kpc) Radio Jets in Narrow-line Seyfert 1 Galaxies
Authors: S. Umayal, Vaidehi S. Paliya, D. J. Saikia, C. S. Stalin, S. Muneer, Maheswar Gopinathan
Figure caption:  Total intensity maps of all the 34 NLSy1 sources, with projected sizes of at least 100 kpc. The background gray images are the Pan-STARRS r-band images, while the contours are the radio images from VLASS (red), FIRST (green), LOFAR 6″ resolution (orange), LOFAR 20″ resolution (blue), and RACS-low (violet). The contour levels are at 3﹩\sigma \times [-({\sqrt{2}}^{m}),{(\sqrt{2})}^{n}]﹩ with m = 0 and n = [0, 1, 2, 3, 4, 5,...] mJy beam−1. The dashed contours represent negative values. The lower left corner of each image shows the beams of the different surveys. The names of the sources are given in the respective panels.
Paper: Predicting Stellar Parameters of Massive Stars from Light Curves with Machine Learning
Authors: Rachel C. Zhang, Kaze W. K. Wong, Gonzalo Holgado, Matteo Cantiello
Figure caption: Workflow setup to perform each of the prediction tasks. This flowchart visually differentiates the two main models tested (MLP, CNN), highlighting how each processes inputs to predict stellar parameters. Models trained to directly predict Teff and ﹩{\mathrm{log}}_{10}g﹩ are denoted with a “1” (e.g., MLP1, CNN1), while models trained to directly predict Teff and ﹩{\mathrm{log}}_{10}{\mathscr{L}}﹩ are labeled with a “2” (e.g., MLP2, CNN2).
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: The figure presents the variation of heating and cooling rates with Ti. Here, ﹩{Q}_{{\rm{vis}}}^{+}﹩ is the total heating rate, while ﹩{Q}_{{\rm{adv}}}^{-}﹩, ﹩{Q}_{w}^{-}﹩, ﹩{Q}_{{\rm{rad}}}^{-}﹩, and ﹩{Q}_{{\rm{tot}}}^{-}﹩ represent the advective, outflow, radiative, and total cooling rates, respectively.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: The thermal equilibrium solution for an accretion disk with MBH = 10M⊙ and α = 0.1 is shown in the figure. This figure reveals the influence of the magnetic field strength on the disk’s topological structure.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: The radial distribution of the advection solution as a function of α for ξ = 1 is shown in the figure.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: The figure shows the variation of heating and cooling rates with Ti for M = 106M⊙ and α = 0.8. All quantities have the same definitions as in Figure 2.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: The figure shows thermal equilibrium solutions for different black hole masses at ξ = 1, α = 0.1, and R = 50Rg.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: For α = 0.1, thermal equilibrium solutions for different black hole masses are presented in the left (ξ = 0) and right (ξ = 1) panels. In the left panel, the solid and dashed red lines coincide.
Paper: Magnetized Accretion Flows: The Key Roles of Viscosity and Black Hole Mass
Authors: Wen-Biao Wu
Figure caption: Thermal equilibrium solutions are plotted for different α and MBH at R = 50Rg. Blue and red curves represent cases with α = 0.1 and α = 0.8, respectively. In the figure, the solid and dashed red lines coincide.
Paper: Magnetic Flux Cancellation in the Solar Atmosphere through 3D Realistic Numerical Modeling
Authors: Fernando Moreno-Insertis, Viggo H. Hansteen, Daniel Nóbrega-Siverio
Figure caption: Result of the synthesis of the Ca II 854.2 nm, Ca II K, Mg II k, and Mg II 279.9 nm lines in the vicinity of the cancellation site. The top row shows, from left to right: the density at 1 Mm; filtergrams of the Ca II 854.2 nm line at 0.04 nm from line center near the k2r peak; the formation height at this wavelength; and the line spectra along the cut y = 10.8 Mm (shown by the green dashed line). The red dashed line is placed at line center, while the red dotted line shows the wavelength plotted in the second column. The second and third rows show the same quantities for the Ca II K and Mg II k lines, but at 0.02 nm from line center, with the downflow speed and temperature at 1 Mm replacing the density in the left column. Finally, the fourth row shows these quantities for the Mg II 279.9 nm line, with the vertical magnetic field Bz at a height of 1.0 Mm being shown in the left column. The black arrow in the vertical velocity figure shows the location of the “ridge” discussed in Section 3.4.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Properties of PRFLs, including the shear angle with the PIL (a), twist parameter α (b), and height z﹩{}_{{\rm{\max }}}﹩ (c) of unique model loops against the time when loops are observed. In each panel, the data points are plotted in color circles, with the color indicating the twist value, given in the color bar in Figure 6. The area of the circle is proportional to the number of repeat observations for each unique loop, and the vertical bar of the same color indicates one-half of the standard deviation of the measurements of the repeat loops. The thick solid black line shows the median value within a 4 minute window, and the thick dashed black lines show the quartiles of the values in the window. (d) Twist parameter α against the time of the footpoint brightening (see Section 2 for definition) in both positive and negative magnetic fields. The median and quartiles of α values within every 4 minutes are plotted in thick black/gray lines for the positive/negative footpoint timing.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Plot of time delays Δt+ and Δt−. The central scatter plot shows Δt− and Δt+ for each reference loop as a cross: red for 304 Å, and blue for 171 Å. Vertical and horizontal dashed lines of matching color show the medians. A broken black line indicates Δt+ = Δt−, and dashed diagonals above and below it mark off the central quartiles of the distribution. Normalized histograms of each delay are plotted along the side and top in matching color for each wavelength.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Top panels: distribution of vertical electric currents averaged for 72 minutes before (a) and after (b) the flare, respectively. Bottom panels: distribution of 〈α〉 averaged for 72 minutes before (c) and after (d) the flare. The black contours denote the flare ribbons, the same as in Figure 1(f). The maps are casted in CEA coordinates of heliographic longitudes and latitudes.
Paper: Observation and Modeling of Shear Evolution of Post-reconnection Flare Loops
Authors: Drake Osaben, Jiong Qiu, Dana W. Longcope
Figure caption: Distribution of α at z = 0 for all best-fit model loops (open circle) and for the consolidated loops (filled circle), superimposed on a magnetogram of the radial component of the photospheric magnetic field in helioprojective coordinates (AIA image plane). The orange curve outlines the PIL of the radial magnetic field.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Predicted trend of total water abundance (number ratio) vs. orbital period. The blue line corresponds to pebble accretion with perfect dust trap with Stokes number = 0.01 and the highest Σ0 whereas the yellow line corresponds to pebble accretion with no dust trap at the highest Σ0. In both cases, a discontinuity appears at our adopted iceline since inside the iceline, solid pollution does not bring additional water and the total atmospheric water content is that of stellar value.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Measured water abundance from simulated Ariel retrievals vs. orbital period using MCS planet data under pebble accretion with perfect dust traps (left) and without a dust trap (right), assuming high-eccentricity migration occurs for Jupiter-mass exoplanets that were originally at a > 1 au. These are the targets predicted to be observable to Tier 2 within a year. The red points are the assigned true water abundance whereas the blue points are the simulated data accounting for uncertainties. Black points are the weighted average of the hot (left-most point) and warm Jupiters (right-most black point). High-eccentricity migration predicts hot Jupiters to appear significantly more water-enriched than warm Jupiters and the amount of such an excess is expected to be detectable by Ariel.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Predicted atmospheric metallicity under pollution by disk-induced migration with respect to the final orbital period of planets. Blue lines correspond to massive disks with Σ0 at the 99th percentile while red lines correspond to that of typical MMEN (F. Dai et al. 2020). Varying levels of transparency correspond to fdep with 1 being no gas depletion. Planets are halted either after 10 Myr or once they reach 10 days, which we set to be the inner edge of the protoplanetary disk. Even the highest metallicity falls below the assumed stellar value 0.02 by roughly 2 orders of magnitude, much more than the order unity numerical coefficient we ignored in the torque calculation.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Measured water abundance from simulated Ariel retrievals vs. orbital period using targets from the MCS under pebble accretion. The uncertainties on the retrieved water abundance, shown here in gray, are drawn from Q. Changeat & K. H. Yip (2022) as described in the text. The transit targets represent the 431 easiest-to-observe Jupiters (M > 0.3Mjup) that can be observed to Tier 2 signal-to-noise ratio in a cumulative observing time of 1 yr. The binned data are shown in black, but the fit shown in red is determined from the unbinned data. The uncertainty on the linear fit is shown by fainter red shading. All targets are within the iceline so a flat H2O abundance with orbital period is expected and obtained regardless of dust trapping.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Predicted trend of metallicity with orbital period under local planetesimal accretion. The blue lines correspond to highest Σ0 (99th percentile) while the red lines illustrate Σ0 of F. Dai et al. (2020). Solid lines show 1 Myr evolution while dotted lines show 10 Myr evolution. The gray lines signify the total available mass budget within the feeding zone.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Same as Figure 2 but for pebble accretion. The top panel corresponds to no dust trapping while the bottom panel corresponds to perfect dust traps (i.e., local accretion) where different colors correspond to varying Stokes number.
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Metallicity comparisons from cross-matched planets in the Mission Candidate Sample catalog (MCS; B. Edwards & G. Tinetti 2022) and the Ariel Stellar Characterisation working group’s catalog (ASC; C. Danielski et al. 2022).
Paper: Testing the Origin of Hot Jupiters with Atmospheric Surveys
Authors: Lina D'Aoust, Ben Coull-Neveu, Eve J. Lee, Nicolas B. Cowan
Figure caption: Cumulative distribution function of solid disk densities at 1 au (Σ0) calculated from protoplanetary disks in C. F. Manara et al. (2023) around stars of mass ≥1M⊙.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Multiwavelength images of Himiko (left) and CR7 (right). The origins of the relative coordinates of Himiko and CR7 correspond to (R.A., decl.) = (2h17m57﹩\mathop{.}\limits^{{\rm{s}}}﹩571, −05°﹩{08}^{{\rm{{\prime} }}}\,\,44\mathop{.}\limits^{\unicode{x02033}}816﹩) and (10h00m58﹩\mathop{.}\limits^{{\rm{s}}}﹩007, 01°﹩{48}^{{\rm{{\prime} }}}14\mathop{.}\limits^{\unicode{x02033}}930﹩), respectively (J2000.0). The gray images show the NIRCam F115W, corresponding to rest-frame UV (beam size ﹩\sim 0\mathop{.}\limits{^{\prime\prime} }07﹩). The green contours show the Hα emission (2σ, 3σ, 5σ, 10σ, 20σ, 60σ) taken with the NIRSpec-IFU PRISM (beam size ﹩\sim 0\mathop{.}\limits{^{\prime\prime} }2﹩). The red contours show the [C II] 158 μm emission (2σ, 3σ, 4σ, 5σ) obtained by the ALMA observations (beam size ﹩\sim 0\mathop{.}\limits{^{\prime\prime} }9﹩). The red crosses indicate the [C II] 158 μm peak position, where the bar scales correspond to their positional uncertainty. The blue contours show the Lyα emission (2σ, 3σ, 5σ, 7.5σ, 10σ, 15σ) taken with NB921 (beam size ﹩\sim 0\mathop{.}\limits{^{\prime\prime} }8﹩). The scale bars show 3 kpc at z = 6.6. In the figures, we do not conduct a PSF matching.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Left: JWST NIRSpec-IFU G395H images collapsed around [O III]λ5007 emission line with a range of 750 km s−1 for Himiko (top) and CR7 (bottom). Black squares show the selected region for the following moment map analysis (Figure 8). White circles show the apertures for the extracted spectrum. North is up, and east is to the left side. We can find the five and four clumps for Himiko and CR7, respectively. Right: [O III]λ4959, 5007 emission lines from the individual apertures taken with NIRSpec-IFU G395H, for Himiko (top) and CR7 (bottom). The black histograms show the spectrum, and the gray shadings show 1σ uncertainties. The red and gray lines show the total Gaussian fitting results and individual Gaussian components, respectively.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: NIRCam images of Himiko and CR7 (5″ × 5″). The F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W (F115W, F150W, F277W, and F444W) images are shown for Himiko (CR7). The scale bar is 1″ (5.5 kpc at z = 6.6). We can see the multiple components in both Himiko and CR7. The circle in the bottom right corner represents the size of the PSF FWHM. In the F277W image of CR7, we show a possible chance-projected object, indicated by the gray arrow (see Section 4.1).
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Neutrino flux averaged over the disks of the Sun, Jupiter, and Earth at d ≫ Ri.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Distributions of Lyα and Hα emission from Himiko (left) and CR7 (right). The background image represents the Lyα emission observed with NIRSpec-IFU PRISM. Only spaxels with S/N > 3 are shown. The blue and gray contours indicate the Lyα emission from NB921 and the Hα emission from NIRSpec-IFU PRISM, respectively. The contour levels and the relative coordinates are the same for Figure 3. The scale bars correspond to 3 kpc at z = 6.6. A PSF matching is not applied in the figures.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Gamma flux from the peripheral region of Jupiter (left) and east–west dependency (East at α = π/2) of the flux.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Neutrino flux from Jupiter observed from three directions θobs at ρ = 0.1, 0.9 (see Figure 6). The dashed line is the flux before including magnetic and absorption effects.
Paper: High-energy Gamma Rays and Neutrinos from the Sun, Jupiter, and Earth
Authors: Pablo de la Torre, Miguel Gutiérrez, Manuel Masip, Alejandro Oliver
Figure caption: Gamma flux from the Earth.