adsabs/AstroCLIMB huggingface dataset:
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: Temporal profiles of 5 minute resolution data plotted for the time period of 01:00 UT 2023 August 5 to 17:55 UT 2023 August 6. (a) Solar near-relativistic electron fluxes (cm−2 sr−1 s−1) of 53–103, 103–175, and 175–315 keV overplotted by their respective smoothed data, and (b) background-subtracted data of the smoothed electron fluxes of these energy channels.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: AIA/SDO 1700 Å images overplotted with HXI contours. The HXI contours cover the two ribbons of the flare.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Height profiles for the two STEREO map series (Interval 5) at a fixed limb angle of 68.15°. The results are shown for STEREO-A (black dots) and STEREO-B (white triangles). A model height profile for h(L) is fitted (dashed line) to the points with Carrington longitude > 220°. The shaded region is as in Figure 9. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Average limb angle of the prominence over time (Interval 5). (Top) The height of the prominence at B*, the weighted-average limb angle, is shown. (Bottom) For each detection, the average angle is calculated for the prominence using Equation (1). The hatched region denotes the approximate timing of the eruption, and is the same as in Figure 8. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: EUV filament channel, EUVI 195 Å (STEREO-B, relative time t = 108.18 hr). The results of the fixed limb angle height models (Figures 10 and 11) are marked with either a cross (AIA) or a triangle (EUVI) in the zoomed-in image. The dashed box indicates the region where intensity oscillations are observed.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Height profiles for the AIA map series (Interval 4) at fixed limb angle: (top) 60° and (bottom) 64°. A model height profile for h(L) is fitted to the top panel (dashed), and two models are fitted to the bottom panel (dashed and dashed–dotted lines). Points in light gray indicate the times and longitudes where a small filament surge affects the results: (top) 176°–181° and (bottom) 177°–180°. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Power spectra for the EUVI 195 Å intensity time series, δ I(t), in Interval 1. (Left) Fourier power spectrum (histogram mode) and Lomb–Scargle periodogram. The spectra are normalized using the variance, σ 2, of the global wavelet power spectrum. (Right) Morlet wavelet power spectrum. Increasing spectral power is indicated by increasing gray levels. Significant power is within the 95% confidence level contours and outside the hatched cone-of-influence region. The normalized global wavelet power spectrum is also shown. Dashed lines denote the global confidence level for the periodograms. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: SDO/AIA 193 Å at relative time t = 234.5 hr). The slit—also used for EUVI—is shown as a dashed box, with the alternative overlapping region shown as a blue box. The triangle and crosses are as in Figure 12.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Filament intensity in SDO/AIA (Interval 2). (Top) Averaged 193 Å intensity, I, in a rectangular region of interest and a smoothed version, I 0. (Bottom) Intensity time series δ I = (I − I 0)/I 0 for the 193 Å and 304 Å sequences. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Filament intensity in STEREO-B EUVI 195 Å (Interval 1). (Top) Averaged ROI intensity, I, and a smoothed profile, I 0. (Bottom) The profile δ I = (I − I 0)/I 0 is obtained using I and I 0 from the top panel. Time is expressed in hours from 2011 March 14 00:00 UT.