adsabs/AstroCLIMB huggingface dataset:
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Estimates of the column density with the PCM (i.e., technique of direct integration) for a point source behind a homologous spherical flow according to column density and resolution. The PCM fails to account for instrumental smoothing, and therefore cannot recover the correct column density. The disagreement grows worse with increasing column density and resolution.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Results of the performance of the two methods (SALT and PCM) in recovering the true column densities for a number simulated data generated using RASCAS (see text for details). The negative correlation between ﹩{\rm{log}}(N/{N}_{{\rm{RASCAS}}})﹩ and ﹩\mathrm{log}{N}_{\mathrm{RASCAS}}﹩ for the PCM estimates shows that the discrepancy between the recovered and true densities grows with the density, similar to the behavior observed in Figure 2.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Comparison of H I derived from three different methods: the DLA H I column density (W. Hu et al. 2023), H I derived from the PMC (X. Xu et al. 2022), and H I derived from SALT. SALT agrees more closely in magnitude with the DLA result than it does with the PCM result.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Comparison between the predicted S II 1254 Å line profile (red line) and the observed data (black line). The predicted profiles are computed using the best-fit geometrical parameters derived from the Si II fits, scaled to the oscillator strength of the line and the solar ratio of sulfur to silicon for galaxies with an uncontaminated S II line.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Comparison between PCM- and SALT-derived total hydrogen mass outflow rates. The two methods have a strong positive correlation with each other, with the galaxies clustering near the black one-to-one line.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Same as Figure 4 but for S IV 1063 Å, using the Si IV fits.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Corner plot for J1112+5503 for the Si III line fit. Blue points represent the chosen maximum likelihood values.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Box plots of difference in CNN-predicted ϕ CNN (right), γ CNN (middle), and ﹩{M}_{{\rm{A}}}^{\mathrm{CNN}}﹩ (left) and the actual values in the simulation A0 (〈M A〉 = 1.25, 〈M  s 〉 = 1.21, 〈γ〉 = 60°) with Gaussian noise introduced. The upper and lower black lines represent the deviation's maximum and minimum, respectively. The box gives ranges of the first (lower) and third quartiles (upper) and the orange line represents the median value. The amplitude of the noise varies from 10%, 50%, to 100% of the mean intensity of the maps, corresponding to SNRs of 10, 2, and 1, respectively.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Box plots of difference in CNN-predicted ϕ CNN (right), γ CNN (middle), and ﹩{M}_{{\rm{A}}}^{\mathrm{CNN}}﹩ (left) and the actual values in the simulation A0 (〈M A〉 = 1.25, 〈M s〉 = 1.21, 〈γ〉 = 60°) when spat. The upper and lower black lines represent the deviation's maximum and minimum, respectively. The box gives ranges of the first (lower) and third quartiles (upper) and the orange line represents the median value. ﹩{k}_{\min }﹩ represents the minimum wavenumber remaining in the filtered synchrotron intensity map and L box is the size of the simulation box.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: A comparison of the CNN-predicted 3D magnetic fields using the simulation 〈M A〉 = 0.79, 〈M s〉 = 0.61, and 〈γ〉 = 60°. Each magnetic field segment is constructed by the POS magnetic field’s position angle (i.e., ϕ) and the inclination angle γ. Note that the magnetic field obtained is the projection along the LOS and averaged over 132 × 132 pixels for visualization purposes. The third axis of the LOS is only for 3D visualization purposes and does not provide distance information here. The total intensity map I is placed on the POS, i.e., the x–y plane.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: 2D histograms of the CNN predictions, i.e., ϕ CNN (right), γ CNN (middle), and ﹩{M}_{{\rm{A}}}^{\mathrm{CNN}}﹩ (left) and the corresponding actual values in simulation. The dashed reference line represents the ideal scenario, where the predicted values and actual values match perfectly.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: A numerical illustration of the anisotropy in normalized synchrotron intensity map. The black streamlines represent the POS magnetic field orientation. Panel (a) 〈M A〉 = 0.26, 〈M s〉 = 0.66, and 〈γ〉 = 90°. Panel (b) 〈M A〉 = 1.21, 〈M s〉 = 0.58, and 〈γ〉 = 90°. Panel (c) 〈M A〉 = 0.26, 〈M s〉 = 0.66, and 〈γ〉 = 30°.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Comparison of the POS magnetic fields predicted by the CNN (right) using the Sino-German λ6 cm synchrotron emission data and inferred from synchrotron polarization (left). The background image is the integrated synchrotron intensity map.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Maps of CNN-predicted inclination angle γ (left panel) and Alfvén Mach number M A using the Sino-German λ6 cm synchrotron emission data. The contours represent the synchrotron intensity structures seen in Figure 8.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Histograms of CNN-predicted ϕ (left), defined north from the west, γ (middle), and M A (right). The synchrotron polarization measured ϕ is also given for comparison.
Paper: Probing Three-dimensional Magnetic Fields. III. Synchrotron Emission and Machine Learning
Authors: Yue Hu, A. Lazarian
Figure caption: Evolution of CNN’s validation loss, i.e., the mean-squared error. Two cases with an input patch size of 22 × 22 cells or 44 × 44 cells are tested.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Thermonuclear X-ray bursts from 4U 1820–30 at 1/16 s time resolution in the 0.4–12 keV range observed with NICER. The gray shaded area corresponds to the burst profile in the 3–12 keV range that is scaled up by a factor of 5 for plotting purposes. All the bursts are aligned on a relative timescale to keep peak time at zero.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: The left panel shows the light curve of Burst #11 from 4U 1820–30 with a bin size of 62.5 ms in 3–10 keV. Vertical blue dashed lines show the time interval used for the calculation of the Z 2 power spectrum for the same energy range. The inset plot refers to the power spectra in the vicinity of 716 Hz. On the right, the pulse profile generated by folding the light curve with the 716 Hz is shown, together with the best-fitting sinusoidal model (blue line).
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The beam response of three calibrators (CasA, 3C295, and CygA) in terms of frequency vs. ρ(f). The frequency spans 400 to 725 MHz with a resolution of 12.5 MHz. ρ(f) spans −24° to 24° in steps of 0.°15. The RFI channels are masked. For the three calibrators, the holography data do not fully cover the range of ρ(f) in the lower band, and hence there are empty regions that we address with zero padding.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The measurement of the geometrical factor G. The outline markers represent the Fourier transform of the beam response of CygA at different bands, which the beam response is measured per 0.°6 (a quarter of the resolution of Figure 18) for visualization purposes. The dashed line illustrates the Gaussian fitting line, and the FWHM is 16.94 m.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: The color–color diagram using NICER observations of 4U 1820–30. The persistent emission before each burst is marked with a number in occurrence order. Two colors (black and red) are considered to distinguish overlapping burst numbers.
Paper: A Comprehensive Study of Thermonuclear X-Ray Bursts from 4U 1820–30 with NICER: Accretion Disk Interactions and a Candidate Burst Oscillation
Authors: Gaurava K. Jaisawal, Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, David R. Ballantyne, Jens H. Beck, Ersin Göğüş, Diego Altamirano, Zaven Arzoumanian, Deepto Chakrabarty, Keith C. Gendreau, Sebastien Guillot, Renee M. Ludlam, Mason Ng, Andrea Sanna, Jérôme Chenevez
Figure caption: Distribution of maximum powers obtained from simulations. The Red dashed line shows the Fourier power value of 37.6 of the signal at 716 Hz found from Burst #11 in the 3–10 keV range.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Absolute ratio of the holography and beam model for the three calibrators, CasA, 3C295, and CygA.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: The beam model resulting from applying the SVD technique to the holography data of CygA.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: From top to bottom: Near-relativistic and relativistic electron intensities, energetic proton intensities, magnetic field magnitude B, magnetic field elevation angle θ, magnetic field azimuthal angle ϕ in spacecraft centered RTN coordinates, solar wind proton speed V  p , solar wind proton density N  p , and solar wind proton temperature T  p  from 2022 November 9 to 17 measured by SolO (left column), STA (mid column), and at L1 (right column). See text for the specific instruments that collected these measurements. The solid vertical lines in the second and third columns indicate the passage of stream interface (SI) of the stream interaction region (SIR) preceding the passage of the solar wind high-speed stream (HSS) seen first by STA and later at L1. Existing SolO magnetic field and solar wind plasma data do not certify the passage of the SIR although the decreasing solar wind speed profile seen by SolO during November 11–12 suggests the passage of a preceding HSS.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: SDO/AIA 211 Å images for the EUV phenomena related to the origin of the ion events #1 (left column) and #6 (right column). The top two panels are direct SDO/AIA 211 Å images prior to the estimated SRTs of the associated SEE events, with overlaid SDO/HMI line-of-sight magnetic field polarity (white and black contours). The four bottom panels are running difference images indicating the main features associated with these EUV confined eruptions.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: Time evolution of (a) 46.7–86.6 keV electron intensities measured in each one of the four EPD/EPT apertures; (b) pitch-angle coverage scanned by the four EPD/EPT apertures; (c) pitch-angle distribution color-coded according to the 46.7–86.6 keV electron intensities in the four apertures; (d) magnetic field magnitude B (black trace) and RTN components of the magnetic field vector B  r  in blue, B  t  in green, and B  t  in magenta; (e) first-order anisotropy coefficient.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: From left to right: SDO/HMI line-of-sight magnetograms, H α  images from GONG ground-based observatories, and SDO/AIA 304 Å images at the times indicated at the bottom of each panel observed prior to a sequence of (top row) three jets on November 12 and two jets (bottom row) on November 14. The yellow, green, and blue arrows and lines indicate the location of minifilaments observed prior to their eruption and were no longer observed after their eruption.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: Time evolution of (a) 46.15–85.7 keV electron intensities measured by Wind/3DP binned in eight different pitch angles; (b) the eight pitch angles used to bin the measured intensities; (c) pitch-angle distribution color-coded according to the 46.15–85.7 keV electron intensities; (d) magnetic field magnitude B (black trace) and RTN components of the magnetic field vector B  r  in blue, B  t  in green, and B  t  in magenta; (e) first-order anisotropy coefficient.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: The same as Figure B1 but for the 45–85 keV electrons measured by STA/SEPT.