adsabs/AstroCLIMB huggingface dataset:
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Parallel electron distribution function (EDF) at different times in the PIC simulation for a core–strahl plasma. Panel (a) represents the total EDF consisting of a Maxwellian for the core and a shifted Maxwellian for the strahl of (relative) density ns0 = 0.05 and a drift velocity of Vs/Ve = 4.0. An electron thermal velocity of Ve = 0.05c was taken. Panel (b) displays the distribution function of only the strahl electrons. After a weak beam configuration at the beginning, a plateau is formed which survives up to the final simulation time of ωet = 7344.
Paper: Particle Acceleration and Transport in the Large-scale Current Sheet under an Erupting Magnetic Flux Rope
Authors: H. Wu, Y. Guo, R. Keppens, C. Xia, Y. Su, X. L. Kong, M. D. Ding
Figure caption: Schematic illustration of mini flux ropes with different chiralities within a fixed-current-and-background magnetic field framework. The upper panel shows a dextral mini flux rope with left-handed twisted field lines and negative magnetic helicity, while the bottom panel shows a sinistral one with right-handed twisted field lines and positive magnetic helicity.
Paper: Particle Acceleration and Transport in the Large-scale Current Sheet under an Erupting Magnetic Flux Rope
Authors: H. Wu, Y. Guo, R. Keppens, C. Xia, Y. Su, X. L. Kong, M. D. Ding
Figure caption: Spectrum of electrons precipitated on the bottom boundary at t = 4.4 t0. (a) Spectrum of the total electron population. (b) Spectra corresponding to those that end up as the five electron sources, colored to match Figure 4.
Paper: Particle Acceleration and Transport in the Large-scale Current Sheet under an Erupting Magnetic Flux Rope
Authors: H. Wu, Y. Guo, R. Keppens, C. Xia, Y. Su, X. L. Kong, M. D. Ding
Figure caption: Histogram of parallel energy changes from all trajectory points in Figure 4. The blue solid line and circles represent the parallel-electric-field term, the orange dashed line and squares indicate the magnetic-field-gradient term, and the green dashed–dotted line and triangles show the curvature acceleration term.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: (Top) Electron core–strahl distribution function, (middle) real, and (bottom) imaginary part of ω/ωe vs. kc/ωe. The propagation angle is θ = 5°. The ratio between cyclotron and plasma frequency is G = Ωe/ωe = 0.1.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: (Left) Electric and magnetic field components vs. time at x = 2000 λe in the PIC simulation with the strahl electrons: (a) Ex(t), (b) Ey(t), (c) Ez(t), E0 = cB0, (d) By(t) and (e) Bz(t); (right) spatial profiles of the magnetic field component Bz and the associated wavenumber power spectrum at ωet = 7000: (f) Bz(x) over the whole simulation box, (g) Bz(x) in high resolution indicating a superposition of large- and small-scale variations, (h) wavenumber power spectrum |Bz(k)/B0|2 showing two peaks which belong to the Fundamental F (ω = ωe, kλe ∼ 0.3) and the Harmonic H (ω = 2ωe, kλe ∼ 1.7).
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Spectra of Bz in the PIC simulation with the strahl electrons. (a) Spectrum vs. frequency ω/ωe and wavenumber kλe. The Fundamental F (ω = ωe, kλe ∼ 0.3) and the Harmonic H (ω = 2ωe, kλe ∼ 1.7) are clearly marked as bright spots. (B) Frequency power spectrum showing F and H as pronounced peaks of nearly the same intensity. (c) Power spectrum in the frequency range up to 1Ωe. The peak at ω ∼ 0.5Ωe indicates the existence of a whistler wave, which is simultaneously excited together with the two high-frequency modes.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Power spectra of the electromagnetic field components (a) By, (b) Ez, and (c) Ex vs. the (normalized) wavenumber kλDe (λDe: Debye length) at ωet = 7344. F and H mark the Fundamental (ω ∼ ωe) and Harmonic (ω ∼ 2ωe) at kλDe ∼ 0.015 and kλDe ∼ 0.085, which corresponds to kλe ∼ 0.3 and kλe ∼ 1.7, respectively. The second harmonic H is generated by nonlinear currents.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Left: temporal evolution of the electric and magnetic fields at x = 2000 λe in the PIC simulation with the core electrons carrying the initial current. (a) Ex (t), (b) Ey(t), (c) Ez (t), (d) By(t), and (e) Bz (t). Right: associated frequency power spectra.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: (a) Temporal evolution of EDF, (b) the initial EDF in the V|–V⊥ plane, and (c) the EDF showing the tail heating at ωet = 3672 in the PIC simulation without the strahl electrons. The black curve in panel (a) shows the initial distribution, which is shifted relative to the ions by the velocity Vd = 1Ve.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Hodogram Ey over Ex, (a) obtained from the temporal evolution in Figure 4, (b) obtained from the electric field measurements by F. S. Mozer et al. (2024) during the type III burst on 2023 March 21. The red curve represents one period of the wave. The gray line shows the magnetic field direction.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Spatial profile of the magnetic component Bz (left) and associated wavenumber power spectra at three times: (a) ωet = 370, (b) ωet = 730, and (c) ωet = 3670 in the PIC simulation with the core electrons carrying the initial current.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Power spectra of the electromagnetic field components (a) By, (b) Ez, and (c) Ex in high resolution in the wavenumber range 0 ≤ kc/ωe ≤ 1. The hot spots in By and Ez at (ω ∼ ωe, kc/ωe ∼ 0.3) mark the coupling point between the current-driven Langmuir wave and the electromagnetic L wave, see also Figure 2.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Temporal evolution of the electric and magnetic field energy in the PIC simulation with the strahl electrons. (a) Electric field energy, (b) magnetic field energy. The three components of E and B are marked by red (x), green (y), and blue (z), respectively. The total energy is marked by the black curves.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: The Hα region of our optical spectra of SU Aur. The wavelength and normalized flux of each spectrum is shown, with the vertical spacing and color according to the time. The psuedocontinuum for each spectrum is underplotted in gray. The Hα profile changes significantly over the 9 days covered by the observations, with increasing self-absorption and a changing ratio of red wing to blue wing flux. The time covered by the X-ray observations is shaded in blue. One high-resolution spectrum was taken just before the X-ray observations started and one during the quiescent period. A .fits file containing the spectral data and observation information for all spectra shown in this figure is available.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Spectra of Bz in the PIC simulation with the core electrons carrying the initial current. (a) |Bz(ω,k)|2 indicating the fundamental (F), the second harmonic (H), and the whistler wave; (b) frequency power spectrum |Bz(ω)|2 in the interval 0 ≤ ω ≤ 6ωe; (c) power spectrum in the range of whistler waves, ω ≤ 1Ωe.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: Spatial profile of Bz at higher resolution in the PIC simulation with the core electrons carrying the initial current, showing the amplitude oscillation caused by the superposition of the fundamental (F) and the second harmonic (H) of nearly equal amplitudes and wavenumbers kc/ωe ∼ 0.3 and kc/ωe ∼ 1.7, respectively. See also Figure 4(g) for comparison.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: XMM-Newton lightcurves of SU Aur. Top: EPIC lightcurves for 2002 data, binned to 600 s intervals. Bottom: EPIC lightcurves for 2012 data, binned to 400 s intervals. In both, the combined, soft, and hard lightcurves are shown in blue circles, orange diamonds, and green squares, respectively. Dotted black lines show the times at which we split the data into the flare and quiescent time intervals for each.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: X-ray lightcurves for AB Aur binned to 5 ks. The combined, soft, and hard lightcurves are shown in blue circles, orange diamonds, and green squares, respectively. AB Aur did not flare during either observation. Top: XMM-Newton/EPIC data from 2002. Bottom: XMM-Newton/EPIC data from 2012.
Paper: Particle-in-cell Simulation of Current-driven Solar Type III Radiation and Whistler Waves in a Core–strahl Plasma: Relevance to PSP and Other Space Observations
Authors: Konrad Sauer, Kaijun Liu
Figure caption: (a) Spatial variation of the electron density and (b) related wavenumber spectrum at ωet = 3672. The density disturbance is about 3%. The wavenumber spectrum has a maximum at kλe ∼ 3 and then decreases due to the onset of Landau damping.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: Chandra lightcurves of SU Aur. The combined, soft, and hard lightcurves are shown in blue, orange, and green, respectively. Regions extracted in the quiescent spectrum are highlighted in blue, while regions extracted for the flare spectrum are highlighted in red.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: Exposure time and detected photons for SU Aur and AB Aur in XMM-Newton slew observation ObsID 9241600003.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: The initial corona with a Gibson–Low flux rope configuration of the CME at time t = 0. Panels (a), (b), and (c) show the SC component of the AWSoM model with the solar surface and flux rope colored to show the radial magnetic field Br, and the 3D coronal magnetic field lines are shown in grayscale. Panel (d) shows the IH component with the inner boundary at r = 20 R⊙ colored to show Br, and the field lines are integrated with only the horizontal magnetic components on the equatorial (x−y) plane. In all images, the solar wind speeds is shown on the solar equatorial (x−y), with the sequence successively zooming out above the equatorial plane to show the development of the slow and fast streams and the CIR in the path of the CME.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: Hydrogen Balmer series lines observed in the optical spectra of AB Aur. Top row: TRES spectra. Spectral orders were continuum-corrected using a combination of polynomial fits. Bottom row: FAST spectra. Spectra are colored based on the time they were taken. We see no changes in the Hα profile across the 5 day period covered by the FAST spectra. A .fits file containing the spectral data and observation information for all spectra shown in this figure is available.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: Long-term lightcurve of SU Aur and AB Aur. See Sections 3.4 and 4.3 for data sources.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: SU Aur. The best-fit single-absorption model (model B) to the 2002 and 2012 EMOS data. Wavelengths of significant atomic species emission lines are shown with dashed and dotted lines. Errors shown are statistical and do not include systematic uncertainties. The inset plot shows a zoomed-in region around the Fe lines.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: SU Aur. Comparison of the best-fit model spectra for model configurations B, C, and D. The EMOS 1 data from 2002 are shown, with error bars showing statistical errors, not including systematic uncertainties. The differences between the models are small and within the uncertainties.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: RGS spectra showing the O VIII (top) and Ne X (bottom) Lyα and β lines. The RGS data are plotted with markers, with our model fit overplotted as a solid line in a corresponding color.
Paper: A Tale of Two Stars: X-Ray and Ground-based Observations of Two Diverging Stars in Taurus–Auriga
Authors: Mackenna L. Wood, Hans Moritz Günther, P. C. Schneider, Scott J. Wolk
Figure caption: X-ray spectra from AB Aur showing a global fit to EMOS and EPN data for the 2002 and 2012 data.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: Close-up of flux rope cluster formed by reconnection seen at time t = 60 hr. Panels (c) through (h) show the equatorial plane colored to represent the values of Bz, proton bulk speed, B magnitude, proton density, and proton and electron temperature, respectively. The magnetic field lines are once again integrated on the plane. The locations of a forward and a reverse shock are shown with curved lines and labeled. The radial line passing through the system shows where data are extracted from the model and shown with line plots. The top-left panel shows the magnetic field components plotted as functions of x with the same scale applied in the 2D images below. The top-right panel shows radial velocity, proton density, and log10 proton temperature. The plots show the system of flux ropes compressed between a forward and a reverse shock, which are delineated by curved lines on the 2D plots. At this scale we see the flux rope system captured between the CME-driven forward and reverse shocks. Solid black lines connect cospatial locations in the line plots and 2D plots at forward and reverse shocks and flux rope boundaries. Note the dagger-like high-velocity jet that cuts off the CME cusp, giving rise to two of the largest flux ropes in the cluster.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: Demonstration of SWIFT constellation measurements taken at 1 au in a tetrahedral configuration with 1 R⊙ sides centered on the radial line shown in Figure 6. The panels show (a) the magnetic field magnitude (∣B∣), individual spacecraft shown in shades of blue, the average shown in black, (b) the field components from SWIFT 1, (c) the plasma speed (∣V∣) and proton density (np) from SWIFT 1, (d) the total electric current density (|J|), individual spacecraft shown in shades of blue, the one evaluated with the curlometer technique from the magnetic fields shown in red (M. W. Dunlop et al. 2002), (e) the curlometer current density components colored as in panel (b), (f) the ratio of the magnetic field divergence and curl, (g) the ratio between the total magnetic forces (∣J × B∣) and ion pressure gradient forces (∣∇Pi∣), and (h) the BZ component extracted as a time series and along a corresponding spatial line at time t = 60 hr.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: Flux rope formation on the equatorial plane. Panel (a) shows a current sheet at t = 15 hr, while panels (b), (c), and (d) zoom in by a factor of 10 to show reconnection forming a magnetic island at time t = 22 hr. Panels (a) and (b) show Bz, while panels (c) and (d) show the proton density and plasma speed (in the frame of the Sun), respectively. Magnetic field lines are shown in black integrating only the x- and y-components. The CME flux rope collides with the CIR, causing it to elongate and form a cusp, which deflects in the direction of the CIR. The cusp compresses and necks off, forming a current sheet where reconnection spawns multiple mesoscale magnetic flux ropes. A smaller white box in panels (b), (c), and (d) shows the location of current sheet formation where reconnection will give rise to the mesoscale flux rope cluster. The interior white box frames the first flux rope as it begins to form. Note panels (c) and (d) show respectively the dense plasma of the CME cusp and the flow field that gives rise to shock formations encompassing the mesoscale flux ropes.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: Images of the velocity field in the frame of the mesoscale flux rope cluster at t = 60 hr. The full complexity of the enveloping flow is revealed in four panels. Panel (a) shows the magnitude of the shifted velocity (Vc) confined on the equatorial plane (x- and y-components only) with colored contours, while velocity streamlines are shown in white. Panel (c) shows color contours of Vz also with velocity streamlines. Panels (b) and (d) show the Alfvén Mach numbers of the Vc and Vz flows, respectively, with magnetic streamlines shown in white. The Alfvénicity of the flows is high, with Mach numbers between 0.8 and 0.9 over much of the flux rope cross sections. Flows in the x–y plane with Mach numbers greater than 1 driven by the reverse shock surround the flux ropes.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: The Bz component of the magnetic field shown on the equatorial plane of the IH component 60 hr after CME initiation. The top panels show the IH domain extending to 250 R⊙, revealing Bz over the entire CME as well as the CIR and shock-enhanced Bz appearing as an arc ahead of the CME ejecta. Panel (a) shows the location of mesoscale flux ropes at the nose of the CME, enclosed in the black box. Panel (b) shows the same region overlaid with the block-adaptive grid. Four levels of refinement are visible in a broad wedge covering the path of the CME. Three additional levels are so dense they saturate and appear solid black. Panel (c) zooms in by a factor of 10 to show a flux rope cluster forming off the nose of the CME, bounded by a forward shock and CIR to the right and a reverse shock to the left. Panel (d) zooms in by a factor of 50 to show a close-up of the mesoscale flux rope cluster, where the grid is shown at 1/16 R⊙. The formation and evolution of these flux ropes is the focus of our paper.
Paper: High-resolution Simulation of Coronal Mass Ejection–Corotating Interaction Region Interactions: Mesoscale Solar Wind Structure Formation Observable by the SWIFT Constellation
Authors: W. B. Manchester, Nishtha Sachdeva, Emilia Kilpua, Matti Ala-Lahti, Shirsh Lata Soni, Zhenguang Huang, Hongfan Chen, Aniket Jivani, Bart van der Holst, Adam Szabo, Mojtaba Akhavan-Tafti
Figure caption: 3D close-up views of the mesoscale flux ropes. Panel (a) shows a comprehensive view of the system looking toward the flux rope cluster from the +x-direction, with the inner IH inner boundary seen in the background colored with Bz. Fully 3D field lines are shown colored by Bz viewed from above the equatorial plane, also colored with Bz. Panel (b) shows a close-up of the leading flux ropes in the cluster with a translucent iso-surface for Np = 100 cm−3, which is largely contained in the +Bz flux rope. Panel (b) is viewed in the +y-direction, while panels (a) and (c) show the system from an oblique angle above the equatorial plane. Panel (c) also shows 2D magnetic field lines in white confined to the equatorial plane formed by integrating only the x- and y-components of B.