adsabs/AstroCLIMB huggingface dataset:
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Magnetic field configuration 28 s before the flare peak for setup (A) (left) and 14 s before the flare peak for setup (B) (right). Field lines are color-coded by twist number as in Figure 8. In addition, we show a second set of field lines that are selected based on their connectivity to the reconnection region; these field lines are color-coded by temperature. In both setups we find tether-cutting reconnection underneath the ejected flux ropes. We show cross sections through the erupting flux ropes that display the mass density. Imagery produced by VAPOR (www.vapor.ucar.edu; Li et al. 2019).
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Cross section from setup (B) along the cut indicated in Figure 1(c). All quantities shown are as in Figure 10. A MFR is present already before the eruption and carries most of the filament mass away after the eruption.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Overview of active region NOAA 12673 from HMI observation at September 6 00:00 UT. The top row shows the entire active region, while the bottom row zooms in on the central region, within the dashed box in each top-row panel, which contains the central penumbral light bridge and large Doppler shift signal of interest. Left-hand column: Continuum intensity normalized to nearby quiet-Sun mean. Middle column: Vector magnetic field map. The background gray image shows the vertical field. The red (cyan) arrows shows the horizontal field vectors in positive- (negative-) B  z  regions. The scale of field strength is plotted on the map. Right-hand column: Doppler velocity after various corrections (see Section 2.1). Redshifted (blueshifted) regions have negative (positive) LOS velocity. Note that opposite to the convention, the sign of v  l  is positive (negative) if the flow is toward (away from) observer. The dashed contours are for v  l  = ± 1 km s−1. The dotted boxes in the top row indicate the field of view of the bottom row.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Hinode/SP results for the central penumbral light bridge for the 2017-09-06T 00:02:05 raster. From top to bottom (excluding leftmost column): Maps at optical depth ﹩\mathrm{log}{\tau }_{500}=0﹩, −0.8 and −1.6. Leftmost column, from top to bottom: Intensity maps for the continuum, line core at 630.25 nm, and line core at 630.15 nm. From left to right (from the second column): temperature, Doppler velocity (saturated at ±4 km s−1), magnetic field strength, and inclination. Zero degrees inclination is toward the observer. The contours are for v  l  = ± 1.5 km s−1. The cross in the upper left-hand panel marks the location of the example fitting results in Figure 6. The dashed line indicates the location of the vertical slice in Figure 7. The results are from the SIR model atmosphere with multiple nodes.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Photospheric velocity field in the active region core region based on HMI data. Left-hand panel: Map of inferred  v  from DAVE4VM, shown as a comparison to the nominal result in the next panel. The background image shows the vertical velocity v  z . The arrows illustrate the horizontal velocity  v   h . Middle panel: Similar to the left-hand panel but from DAVE4VMwDV. Right-hand panel: Map of the angle θ between  v  and  B . Red color indicates the region with flows parallel or antiparallel to the magnetic field. The dashed contours are for observed Doppler velocity v  l  = ±1 km s−1, defined in the last panel of Figure 1.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Histogram of several variables in the central penumbral light bridge with fast Doppler flow (inferred ∣v  l ∣ ≥ 1 km s−1). The regions are marked by the contours in Figure 2. Left-hand panel: Observed Doppler velocity v  l  (average of 00:00 and 00:12 UT frames) and inferred vertical velocity v  z . Middle panel: Variable ﹩| {v}_{z}/{v}_{l}\,| \hat{{\boldsymbol{z}}}\cdot \hat{{\boldsymbol{\eta }}}﹩, where ﹩\hat{{\boldsymbol{z}}}﹩ is the local vertical unit vector. This illustrates the relative contribution of v  z  to the observed v  l . Right-hand panel: Angle between  v  and  B .
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Scatter plot of the cosine of magnetic inclination ﹩\cos \gamma ﹩ and LOS velocity v  l  inside the light bridge for pixels with continuum intensity greater than 30% of a nearby quiet Sun. Points above and below the v  l  = 0 line come from the blueshifted and redshifted regions, respectively. The blue-dashed lines illustrate the expected patterns if the observed v  l  is due to a 5 km s−1 and 15 km s−1, field-aligned flow in the redshifted light bridge. The red line is the best fit for pixels with v  l  < −1.5 km s−1. The pink shade illustrates the 95% confidence interval, which is about twice the line thickness. The slope is 9.6 km s−1. The blueshifted points appear to lack a clear linear relation.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Example of SIR fitting of Hinode/SP observation. The four panels are for Stokes I, Q, U, and V, normalized by quiet-Sun continuum intensity I 0. Black curves show the observed Stokes profile in the light bridge for the point marked by the white×in Figure 4. Blue and red lines are for SIR fitting with one and multiple nodes, respectively. The two vertical dotted lines indicate the reference line-center wavelengths.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: A vertical slice through the light bridge along the dashed line in Figure 4. The x-axis shows the spatial extent. The y-axis shows the logarithm of optical depth, limited between ﹩\mathrm{log}{\tau }_{500}=0﹩ and −2. From top to bottom: Temperature, Doppler velocity, and inclination with respect to the LOS. The black-dashed lines indicate the approximate boundary of the light bridge, where the continuum intensity is greater than 30% of the quiet Sun.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Comparison of observed and inferred Doppler velocities from HMI. Only the central region is shown. Left-hand panel: Averaged HMI v  l  map for 00:00 and 00:12 UT. Middle panel: v  l  from DAVE4VM. Right-hand panel: v  l  from DAVE4VMwDV. The dashed contours are for observed v  l  = ±1 km s−1.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: The Doppler velocity maps inferred from Hinode/SP observation at optical depth ﹩\mathrm{log}{\tau }_{500}=0.0﹩, ﹩\mathrm{log}{\tau }_{500}=-0.8﹩ and ﹩\mathrm{log}{\tau }_{500}=-1.6﹩. The black lines are the PILs for the LOS magnetic field B  l  at each depth.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Scatter plots of the velocities inferred using five-point stencil and the Schall operator for numerical differentiation. The four panels are for the v  x , v  y , v  z , and v  l  component, respectively. The slope of a linear fit and the Pearson correlation coefficient r are noted for each case.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Maps of the standard deviations for v  x , v  y , and v  z  from the Monte Carlo sample, from left to right. Black-dashed contours mark the region with ∣v  l ∣ > 1 km s−1.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption:  L-curve displaying the trade-off between the two loss functions L 1 and L 2 in DAVE4VMwDV, for the HMI observations of active region NOAA 12673. The values next to the black dots represent the weighting λ of each test.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: Scenario to explain the persistent convergent flows near the PIL from Lites et al. (2002). The magnetic field flux tubes interlace and bend downward near the PIL seen from LOS. The oppositely directed Evershed flows converge upon the PIL and return to the interior.
Paper: Large Photospheric Doppler Shift in Solar Active Region 12673. I. Field-aligned Flows
Authors: Jiayi Liu, 嘉奕 刘, Xudong Sun, 旭东 孙, Peter W. Schuck, Sarah A. Jaeggli, Brian T. Welsch, C. Quintero Noda
Figure caption: BIC maps of SIR fitting for the Hinode/SP scan at 00:02:05 UT. Left-hand panel: BIC map in logarithmic scale from inversion with multiple nodes (with gradient). Middle panel: Same as left-hand panel but for single-node inversion (without gradient). Right-hand panel: The ratio of BIC between multi-node and single-node inversions.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: The contribution to the gamma-ray flux from NGC 1068 (panel (b)) and the background gamma-ray intensity (panel (a)) by the internal shocks for models M1 (solid black), M2 (black dashed line), and M3 (black dotted line). In panel (a), solid points represent the intensity observed by Fermi-LAT (red, Ackermann et al. 2015), COMPTEL (teal, Weidenspointner et al. 2000), SMM (brown, Watanabe et al. 1997), Swift BAT (cyan, Ajello et al. 2008), and RXTE (purple, Revnivtsev et al. 2003). Thin solid, dashed, and brown dotted lines represent the intensities predicted by models for Seyfert galaxies (Gilli et al. 2007), blazars (Giommi & Padovani 2015), and star-forming galaxies (Lacki et al. 2014), presented in De Angelis et al. (2021). In panel (b), the red, blue, and purple points represent the observed gamma-ray intensities adopted from Ajello et al. (2017); Abdollahi et al. (2020), and Acciari et al. (2019), respectively. The sensitivities for future telescopes in ∼MeV bands are presented by colored dashed lines.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Trace-back time (the time when an ejected star reached its birthplace) vs. current separation between runaway/walkaway stars and their birthplaces. Left: runaway/walkaway candidates born in IC 348 collected from Kounkel et al. (2022b; gray points), and in our study (colored symbols). V701 Per has three possible birthplaces, shown separately. LRL 170 and LRL 92 are currently within the central region of IC 348, with their trace-back times set to 0.01 Myr. The cyan horizon line represents the radius containing half of IC 348’s members. Yellow and green diagonals show the projected velocity of 30 km s−1 and 5 km s−1 at 325 pc, separately. Right: same as the left panel, but for candidates born in the Mestor and Heleus subgroups within the Perseus cloud.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: The spectral energy distribution for nonthermal emission from internal shocks of the jet for models M1 (solid), M2 (dashed line), and M3 (dotted line).
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Proper motion deviation ﹩{\rm{\Delta }}\mu =\sqrt{{({\rm{\Delta }}{({\mu }_{\alpha }\cos \delta ))}^{2}+({\rm{\Delta }}{\mu }_{\delta })}^{2}}﹩ (y-axis) between center of mass and center of light in binary systems in relation to the binary separation a (x-axis), assuming that the binary orbit is circular and viewed face on. Panels represent the mass combinations of binaries, with primary masses M 1 of 0.2, 0.3, 0.5, and 1.0 M ⊙ from the left column to the right column, and mass ratios M 2/M 1 of 0.2, 0.4, 0.6, 0.8, and 1.0 from the top row to the bottom row. The condition where the secondary mass is less than 0.1 M ⊙ is not included. The legend in each panel shows the luminosity of the binary.
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: The cumulative number of gamma-ray emitting sources predicted to be detectable by Fermi-LAT as a function of the luminosity distance for the fiducial model (solid black line), a model with a smaller number of accreting sBHs per AGN disk (N BH,acc = 5, orange dashed line), and that with a weaker gamma-ray luminosity (L  γ,iso = 1040 erg s−1, blue dashed line). The number of gamma-ray sources, inferred from observations, in nearby radio-quiet Seyfert galaxies for moderate and optimistic cases are shown in red and brown dotted lines.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Similar to Figure 5, but for LRL 92. Members which overlapped with LRL 92 by 1σ and 2σ are shown as blue triangles and green hexagons, respectively, with proper motion vectors pointing to past positions in a scale of 5 mas yr−1 at a vector length of 0.1.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: The cumulative distribution of temperatures of the six young proper motion outliers in this study (orange), high-confidence IC 348 members (gray), runaway stars born in the Orion Nebula cloud in McBride & Kounkel (2019; blue), and Orion stars in Kounkel et al. (2018; cyan). The temperatures are from the APOGEE measurements in Kounkel et al. (2019; IC 348) and Kounkel et al. (2018; Orion).
Paper: High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman
Figure caption: A schematic picture of emission from internal shocks in a jet launched from an sBH accreting gas in an AGN disk.
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Diagram showing that galaxies that have infallen at earlier times are quenched earlier across all of our sample redshifts (z = 0.26–1.13). The 4000 Å break (Dn4000) and the position in the projected phase space ((r proj/r 500) ×  (Δv/σ cl); Figure 3) are used as proxies for mean stellar age and cluster infall time, respectively. In each panel, different colors indicate different infall time zones separated by vertical dashed lines and the color bars on top (Section 3.2): early (red), intermediate (orange), and recent (blue) infall. Top: distribution of galaxies at all redshifts (0.26 < z < 1.13). Colored diamonds indicate the bootstrapped mean Dn4000 of galaxies in the corresponding infall time zones. The error of the mean is smaller than the symbol size. The black solid line is a linear fit to individual galaxies derived from bootstrapping with the Dn4000 uncertainties accounted for (Table 3). The dotted horizontal line indicates Dn4000 = 1.55 as the guideline used in the literature to separate star-forming (Dn4000 < 1.55) and quiescent (Dn4000 > 1.55) galaxies. The typical uncertainty of Dn4000 is marked in the bottom right of each panel. Middle: distribution of low-redshift (0.26 < z < 0.53) subsamples. Bottom: distribution of high-redshift (0.53 < z < 1.13) subsamples. Note that there is a continuous increase in the mean Dn4000 of galaxies with the infall time proxy at all redshifts (from top to bottom), as also shown in the histograms on the right. The continuous Dn4000 increase with the infall time proxy (from recent to early infall) shown in all panels suggests that galaxies become quenched as they spend a longer time in the cluster environment at all redshifts z = 0.26–1.13 (Section 4.1).
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Projected phase space diagram of galaxies stacked from 105 clusters at 0.26 < z < 1.13 (i.e., the normalized line-of-sight peculiar velocity vs. projected clustercentric radius), which shows a variety of accretion stages of cluster galaxies since infall. The white circles and gray plus signs indicate the low-redshift (0.26 < z < 0.53) and high-redshift (0.53 < z < 1.13) subsample galaxies, respectively. The phase space is color coded by different infall time zones based on the caustic lines (i.e., solid lines; Section 3.2): early infall (red), (r proj/r 500) ×  (∣Δv∣/σ cl) < 0.1; intermediate infall (orange), 0.1 < (r proj/r 500) ×  (∣Δv∣/σ cl) < 0.4; and recent infall (blue), (r proj/r 500) ×  (∣Δv∣/σ cl) >0.4. The dashed line is the escape velocity curve of a cluster assuming an NFW potential (Navarro et al. 1996) with the typical cluster mass (M 500 = 4.97 × 1014 M ⊙) and velocity dispersion (σ cl = 1052 km s−1) of our sample clusters. Comparison of the galaxies’ distribution with the escape velocity curve suggests that galaxies within the early and intermediate infall zones are likely gravitationally bound to the cluster, while galaxies within the recent infall zone are becoming gravitationally bound. This figure shows the overall accretion stages of cluster galaxies over a wide range of redshifts and illustrates how our analysis adopts the galaxies’ location in the projected phase space to statistically infer the mean infall time of galaxies based on cluster simulations (Section 3.2).
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Similar to the top panel of Figure 4 but focusing on the galaxy luminosity dependence of the environmental quenching effect (i.e., the continuous age (Dn4000) increase of galaxies since infall). The diamonds and associated error bars are the bootstrapped mean Dn4000 strength and the 1σ standard deviation of galaxies in each infall zone. Different colors indicate the different i-band luminosity bins: all (black), faint (sub-L*; orange), and bright (super-L*; blue). Note that both the faint and bright subsamples show a continuous Dn4000 increase with infall proxy. However, at all fixed infall zones, bright galaxies have larger mean Dn4000 compared to their faint counterparts. This suggests that environmental quenching impacts galaxies regardless of the galaxies’ luminosity, yet the exact age (Dn4000) depends on the galaxies’ luminosity due to an internal mass quenching (i.e., downsizing) effect at a fixed environment (Section 4.2).
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: The figure shows that galaxy luminosity (left) and redshift (right) do not show an obvious dependence on infall proxy. The red points with error bars indicate the median values and associated 1σ spread per infall proxy bin. In the left panel, the galaxy luminosity (L  i /L*) distribution is similar regardless of infall proxy, with median values consistent within 1σ. In the right panel, the redshift distribution is also consistent across all infall proxies, although the median redshift seems to slightly decrease with infall proxy within 1σ population spread. Little (or no) dependence of luminosity and redshift on infall proxy suggests that the increasing Dn4000 trend with infall time proxy (e.g., Figure 4 and Section 4.1) is not driven by either luminosity or redshift. Rather, it is most likely due to environmental quenching such that galaxies that have infallen earlier stopped star formation earlier. It is also regardless of specific galaxy luminosity (Figures 6 and 8 and Section 4.2) and redshift bins (Figure 9 and Section 4.3).