adsabs/AstroCLIMB huggingface dataset:
Paper: Massive Star Formation Starts in Subvirial Dense Clumps Unless Resisted by Strong Magnetic Fields
Authors: Ke Wang, Yueluo Wang, Fengwei Xu
Figure caption: An example of the NH3 line fitting using our procedure. The black lines are mean NH3(1,1) and NH3(2,2) spectra extracted from within the clump size of HMSC G022.5309-0.1927. The red lines show the best-fit model. The fitted parameters and their uncertainty are printed on the top right corner of the plot.
Paper: Massive Star Formation Starts in Subvirial Dense Clumps Unless Resisted by Strong Magnetic Fields
Authors: Ke Wang, Yueluo Wang, Fengwei Xu
Figure caption: Histograms of basic, fitted, and derived parameters of the HMSCs (Table 1): clump mass, equivalent radius, NH3-fitted velocity dispersion, kinetic temperature, NH3 abundance, derived Mach number, virial parameter, and estimated magnetic field strength (for the 43 HMSCs with α vir < 2).
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: Clouds alter the location where the atmosphere emits. In this case, the dayside atmospheric temperature/pressure profile of an idealized terrestrial planet is only 50 K hotter (at all pressures) than the nightside of the same planet. However, the nightside of the planet is cool enough to form clouds in the upper atmosphere. The dayside emission height will depend on the atmospheric composition and resulting gas-phase opacity. In the most extreme case where the atmospheric gases are optically thin, the dayside emission height will be at the planetary surface. However, the nightside emission height will be at the top of the cloud deck if the clouds are optically thick.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: The observed contrast in dayside/nightside brightness temperature as a function of actual day/night temperature contrast for a 10 bar atmosphere with an N2- or O2-dominated atmosphere (observed at either 3–4 or 4–5 μm) and a CO2-dominated atmosphere observed at two different infrared wavelength ranges. For our fiducial temperature profile structure, the observed day/night brightness temperature contrast remains roughly constant for actual atmospheric temperature contrasts greater than 10 K. For temperature contrasts less than 10 K (gray region), the observed brightness temperature contrast depends on the efficiency of cloud formation on the dayside given a very marginal condensable supersaturation and thus requires more detailed microphysical modeling to reach robust conclusions.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: The dayside/nightside temperature contrast as a function of atmospheric composition as seen in observations averaged over 3–4 μm (top left), 4–5 μm (top right), 11–14 μm (bottom left), and 13–15 μm (bottom right). All atmospheres show dayside/nightside temperature contrasts that are enhanced compared to the true difference in dayside/nightside temperature (i.e., 50 K). The N2- and O2-dominated atmospheres show the most extreme observed dayside/nightside temperature contrast—equivalent to the difference in temperature from the top to the bottom of the atmosphere.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: The condensation sequence for a solar composition atmosphere where dashed lines indicate the condensation curves for a variety of typically assumed condensable species. The model planet atmosphere day (red) and night (blue) temperature profiles are shown. In the case of a primordial solar composition atmosphere there may exist a favorable region of temperature phase space where we do not expect significant opacity from condensational clouds (at ∼400–800 K). However, given the presumed diversity of terrestrial atmospheres, such a favorable region may be unlikely to exist.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: The atmospheric flux from the planetary dayside (red) and nightside (blue) for a host of atmospheric compositions for the case of a 10 bar atmosphere (top) and 1 bar atmosphere (bottom). In most cases (except for an N2- and O2-dominated atmosphere) the dayside emission exhibits atmospheric features, while the nightside emission resembles a blackbody emitting at a low temperature). In all cases nightside clouds give rise to significant dayside/nightside temperature contrasts.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: Same as Figure 6 but for the 1 bar atmosphere case. In the case of a 1 bar planetary atmosphere, the dayside/nightside temperature contrast is exaggerated as compared to the 10 bar case.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: The height of the cloud deck alters the nightside emission height and thus the observed nightside brightness temperature. Here we vary the location of a gray cloud deck that extends over 1 dex of atmospheric pressure. Clouds present in the upper atmosphere give rise to low observed brightness temperatures.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: Spatially inhomogeneous nightside clouds can mimic atmosphere-free terrestrial planets. (a) A cartoon picture of a terrestrial planet without an atmosphere. The observed brightness temperature comes from thermal flux from the hot dayside surface and cold nightside surface. This may appear similar to (b), the case where the planet hosts a substantial optically thin atmosphere and an optically thick layer of nightside clouds. Both the dayside and nightside of the planet are similarly hot, and the observed brightness temperature again originates near the surface of the dayside; however, the emission from the nightside arises from above the optically thick cloud deck. In this picture, the observed day/night brightness temperature contrast can be much larger than the intrinsic day/night temperature contrast.
Paper: Nightside Clouds on Tidally Locked Terrestrial Planets Mimic Atmosphere-free Scenarios
Authors: Diana Powell, Robin Wordsworth, Karin Öberg
Figure caption: Even in the most optimistic case of an optically thin atmosphere (τ = 0.1), GCM predictions from D. D. B. Koll (2022) for dayside and nightside brightness temperatures for TRAPPIST-1b and LHS 3844b are inconsistent with observations. This is particularly true in regards to LHS 3844b, where no nightside emission was detected from the planet.
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: Profiles of ((a)–(b)) Pedersen conductivity (σ p), ((c)–(d)) neutral wind velocities, and ((c)–(d)) ﹩\tfrac{{{\boldsymbol{\sigma }}}_{{\boldsymbol{p}}}{({\boldsymbol{U}}\times {\boldsymbol{B}})}_{{\boldsymbol{x}}}}{{{\boldsymbol{\Sigma }}}_{{\boldsymbol{p}}}}﹩ (positive eastward) in the equatorial region (1.°25N) at 12 LT. First column: MP effects (blue line) and no-flare (gray line) conditions at MP peak. Second column: ELP effects (blue line) and no-flare (gray line) conditions at ELP peak.
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: Redshifts and stellar masses for the galaxies in our sample in red. Our galaxies have 1.5 < z < 3 and log(M */M ⊙) ∼1010–1012. The black dots show the CEERS AEGIS field galaxies (G. B. Brammer et al. 2012; R. E. Skelton et al. 2014).
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: Comparison of galaxy images in the F150W and F444W filters produced by JWST. The white ellipse shows the effective radius of each galaxy’s fits. Each galaxy’s PSF FWHM is also shown. While the bulges of these 1.5 < z < 3 galaxies appear small in the F150W, we see their dominance when looking at the F444W image.
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: Top: the radial profile of the intensity in Band 7 (blue) and Band 3 (orange). The beam size is 0.″073 × 0.″066 for both wavelengths, which corresponds to 0.″113 × 0.″069 after deprojection. The dashed line represents the Band 3 profile scaled to match the peak intensity of Band 7 for comparison of the radial morphology. The shaded area represents the uncertainties, calculated as the rms noise level divided by the square root of the number of independent data points. The Gaussian in the upper right corner shows the major and minor axes of the beam after deprojection. Bottom: the radial profile of the spectral index. The error bar in the lower right corner indicates the 1σ error range due to the absolute flux calibration uncertainty. The shaded region shows the uncertainties propagated from the uncertainties of the radial profiles.
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: Images of PDS 70. Left: Band 3; middle: Band 7; right: spectral index between Band 7 and 3. The intensity is shown in brightness temperature using the Rayleigh–Jeans approximation. The peak brightness temperature in Band 7 of 4.2 K using the Rayleigh–Jeans approximation corresponds to 10.4 K in the full Planck brightness temperature. The contours in the left panel show 5, 10, 15, and 20 times the rms noise level, and the contours in the middle panel show 5 times the rms noise level.
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 azimuthal intensity profile along the ring in Band 7 (blue) and Band 3 (orange). The images are smoothed to be a circular beam with a size of 0.″12 after deprojection. The error bar in the upper left indicates the 1σ rms noise level.
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: Distribution of the spacing of any two spikes above 78 Jy in Figure 2 in T. H. Hankins et al. (2003).
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 full data set (a) and from the visually selected type III burst subset (b) for unweighted (blue) and weighted (orange) fits, at the five considered frequencies. Red (a), blue, and orange (b) full lines represent the empirical probability density function, P emp(τ), estimated using the KDE approach and constructed from the histogram.
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: Light curves of the radio flux density measured by SO/RPW/HFR at five frequency channels during a type III burst on 2023 November 26. Red lines show the results of the decay time fitting.
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: (a) Scatter plot of the decay times from the original data set at higher time resolution (x-axis) and reduced resolution (y-axis) for the five considered frequencies. The blue line represents the linear fit on the data, and the red line is the bisector. (b) Decay times for the five considered frequencies obtained as the median value from the observed distributions. Red: full time resolution data set; black: data set with time resolution reduced to 3.5 s; green: PSP data set with 3.5 s resolution. Error bars represent the standard error. The black, red, and lime lines correspond to the power-law fit on the respective five data points. The blue dashed line shows the power-law function from Equation (1).
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: (a) Decay times for the five considered frequencies obtained as the median value from the observed distributions. Error bars represent the standard error. The dashed line shows the power-law function from Equation (1). (b) Median decay time values from the weighted fits on the type III bursts from the selected subset in the frequency range of 3–13 MHz (shaded region), superimposed on the data shown in Figure 10 of E. P. Kontar et al. (2019) and the newly added data from N. Chrysaphi et al. (2024). Error bars represent the standard error obtained from the observed distributions. The new best-fit function is also printed.
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: Example of the HFR frequency sweep as a function of time for the receiver configuration described in the main text. Time is measured in seconds from the beginning of the sweep.
Paper: The Discovery of Three Pulsars in the Globular Cluster M15 with FAST
Authors: Yuxiao Wu, Zhichen Pan, Lei Qian, Scott M. Ransom, Ralph P. Eatough, BoJun Wang, Paulo C. C. Freire, Kuo Liu, Zhen Yan, Jintao Luo, Liyun Zhang, Minghui Li, Dejiang Yin, Baoda Li, Yifeng Li, Yinfeng Dai, Yaowei Li, Xinnan Zhang, Tong Liu, Yu Pan
Figure caption: The lower panel shows the polarization-calibrated pulse profile of PSR M15C measured at FAST in 2019—MJD 58829 (the black, red, and blue lines represent total intensity, linear polarization, and circular polarization, respectively). Measurements of the polarization position angle are shown in the upper panel.
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: Light curves of the radio flux density measured by SO/RPW/HFR during a type III burst. Red lines show the results of the decay time fitting.
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: Decay time as a function of the radial distance for the five considered frequencies.
Paper: Magnetic Field Geometry of the Gamma-Ray Binary PSR B1259–63 Revealed via X-Ray Polarization
Authors: Philip Kaaret, Oliver J. Roberts, Steven R. Ehlert, Douglas A. Swartz, Martin C. Weisskopf, Ioannis Liodakis, M. Lynne Saade, Stephen L. O'Dell, Chien-Ting Chen
Figure caption: IXPE and Swift X-ray light curves in the 2–6 keV band. The vertical dashed–dotted line shows when the pulsar crosses the stellar disk. The vertical dotted lines show the start and end of the IXPE observation.
Paper: Magnetic Field Geometry of the Gamma-Ray Binary PSR B1259–63 Revealed via X-Ray Polarization
Authors: Philip Kaaret, Oliver J. Roberts, Steven R. Ehlert, Douglas A. Swartz, Martin C. Weisskopf, Ioannis Liodakis, M. Lynne Saade, Stephen L. O'Dell, Chien-Ting Chen
Figure caption: Orbital motion of B1259−63. The pulsar moves clockwise around the orbit shown as the solid curve. Marked along the orbit, in time order, are periastron (circle), start of IXPE observation (diamond), and observation end (square). The star shows the system barycenter. The X-ray EVPA is shown as the solid orange line radiating from the barycenter, with its uncertainty shown as the two dashed orange lines. The two black dotted lines show the position angle of the pulsar and, thus, the shock cone at the start and end of the IXPE observation.
Paper: Magnetic Field Geometry of the Gamma-Ray Binary PSR B1259–63 Revealed via X-Ray Polarization
Authors: Philip Kaaret, Oliver J. Roberts, Steven R. Ehlert, Douglas A. Swartz, Martin C. Weisskopf, Ioannis Liodakis, M. Lynne Saade, Stephen L. O'Dell, Chien-Ting Chen
Figure caption: Contour plots of the PD and angle without correction for background. The × marks the measured values. The contours show the 68.27%, 95.45%, and 99.73% confidence intervals for χ 2 on 2 degrees of freedom.
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: Group velocities of LCP and RCP waves recorrected by relativistic effects of nanoshots. (a) a 0 = 10,000. Blue lines are selected paths (starting from r 0 = 200, 300, 400, and 450 km) inducing the 21 μs delay for LCP and RCP waves. Vertical dashed lines mark the starting points. The path length is shown also. (b) a 0 = 1000. The 21 μs delayed paths start from r 0 = 800, 900, 1000, and 1100 km. (c) a 0 = 450. The 21 μs delayed path starts from r 0 = 1349 km and ends at the light cylinder r  lc  ≈ 1579 km. The second path is from r 0 = 1000 km to r  lc . (d) a 0 = 100. Both nanosecond-delayed paths end at r  lc .
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: Labeled nanoshot pairs ﹩(i,i^{\prime} )﹩ in the original Figure 2 in T. H. Hankins et al. (2003).
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: (a) Group velocities for LCP and RCP waves at ω  pe /ω 0 = 1. The transmission distance required to produce a 21 μs L–R delay is determined by the ratio v  g,R /v  g,L . (b) Parameter curves for v  g,R /v  g,L  = 0.9, 0.99, and 0.995.
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: (a) Group velocities of LCP and RCP waves in the electron plasmas along the magnetic field at ω  B /ω 0 = 5. (b) The critical value ω  pe /ω 0 for v  g,L  = v  g,R .
Paper: Mechanism of Circular Polarization in Giant Pulses and Fast Radio Bursts
Authors: Hui-Chun Wu
Figure caption: (a) Group velocities of RCP waves with the frequencies ω 0 and 1.03ω 0 at the end of all the 21 μs delayed paths in Figure 3. They are plotted as a function of the path-starting position r 0. (b) The time delay of RCP waves at ω 0 and 1.03ω 0 as a function of ratio of their velocities at the path end given in (a).
Paper: The Discovery of Three Pulsars in the Globular Cluster M15 with FAST
Authors: Yuxiao Wu, Zhichen Pan, Lei Qian, Scott M. Ransom, Ralph P. Eatough, BoJun Wang, Paulo C. C. Freire, Kuo Liu, Zhen Yan, Jintao Luo, Liyun Zhang, Minghui Li, Dejiang Yin, Baoda Li, Yifeng Li, Yinfeng Dai, Yaowei Li, Xinnan Zhang, Tong Liu, Yu Pan
Figure caption: M15I detections, on MJD 59144 (left) and MJD 59933 (right). These pulsar candidates’ heuristic plots were generated with the PRESO PREPFOLD routine. Starting clockwise from the bottom left, the first panel shows the pulse profile as a function of observing time through 128 subintegrations represented in gray scale, as well as the reduced χ 2—a measure of the profile significance—also as a function of time. White banding are subintegrations excised due to radio frequency interference (RFI). On the top left is the integrated pulse profile. To the right are the various discovery parameters in the topocentric and barycentric reference frames. The three panels on the right show the results of the period and period derivative optimization process. The lower middle panel shows the reduced χ 2 as a function of trial DM, and the grayscale panel in the middle shows the pulse profile as a function of observing frequency across 128 subbands where subbands excised due to RFI are visible as white bands.
Paper: The Discovery of Three Pulsars in the Globular Cluster M15 with FAST
Authors: Yuxiao Wu, Zhichen Pan, Lei Qian, Scott M. Ransom, Ralph P. Eatough, BoJun Wang, Paulo C. C. Freire, Kuo Liu, Zhen Yan, Jintao Luo, Liyun Zhang, Minghui Li, Dejiang Yin, Baoda Li, Yifeng Li, Yinfeng Dai, Yaowei Li, Xinnan Zhang, Tong Liu, Yu Pan
Figure caption: Average pulse profiles (left) and timing residuals for the pulsars in M15 (right; the MJD of the timing residuals spans from 58350 to 60500). In all profiles, the uncalibrated peak flux density is normalized to unity. The Y-axis of the residual plot is in units of pulse phase. To obtain better timing solutions for the new pulsars and M15G, we used TOAs from the most recent observation data. For the other pulsars, their timing solutions are already well established, so we did not include the newest data (observations after MJD 60000) for them. The profile of M15G appeared notably complex upon its discovery. In our study, we were able to derive a timing solution for M15G according to these detections.
Paper: The Discovery of Three Pulsars in the Globular Cluster M15 with FAST
Authors: Yuxiao Wu, Zhichen Pan, Lei Qian, Scott M. Ransom, Ralph P. Eatough, BoJun Wang, Paulo C. C. Freire, Kuo Liu, Zhen Yan, Jintao Luo, Liyun Zhang, Minghui Li, Dejiang Yin, Baoda Li, Yifeng Li, Yinfeng Dai, Yaowei Li, Xinnan Zhang, Tong Liu, Yu Pan
Figure caption: X-ray image of M15 in the energy range 0.2–20 keV from Chandra archival data. The blue triangles show the positions of known X-ray sources, while the red stars indicate the positions of the known radio pulsars. The large green circle and smaller green circle indicate the half-light radius and core radius of M15, respectively (W. E. Harris 1996).
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: The (a) X-ray flux in the wavelength band of 0.1–0.8 nm and EUV flux at 33.5 nm, (b) EEJ calculated from the differential geomagnetic horizontal (H) component between A11 (geographic 1.°45S, 48.°45W, geomagnetic 0.°44N) and KOU (geographic 5.°21N, 52.°73W, geomagnetic 8.°62N), and (c) and (d) simulated height-integrated zonal current densities (Jx, positive eastward) at A11. The vertical gray dashed lines indicate the flare onset (11:53 UT) and ELP peak (13:53 UT). MP = the flare MP; ELP = the EUV late phase.
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 WI, field-aligned integral Pedersen conductance (ΣP), VN (northward positive), and UN (eastward positive) at local noon. The first to third columns are the results with the entire flare effect, MP effect, and ELP effect, respectively. Dashed lines denote the flare onset (11:53 UT) and ELP peak (13:53 UT).