adsabs/AstroCLIMB huggingface dataset:
Paper: No Evolution in the Half-mass Radius of Milky Way–type Galaxies over the Last 10 Gyr
Authors: Maryam Hasheminia, Moein Mosleh, Sandro Tacchella, S. Zahra Hosseini-ShahiSavandi, Minjung Park, Rohan P. Naidu
Figure caption: (a) SFH of (i) MW-type galaxies derived by applying the MSI method to the SFR–M ⋆ relation of Sp14 (red line); (ii) the MW from Sn15 (blue line); and (iii) MW-like galaxies in the IllustrisTNG (TNG50) simulation (green line). (b) Corresponding SMGHs with a final stellar mass of M *,0 = 1010.7 M ⊙. The SMGH of the MW of Sn15 is in good agreement with Kruijssen et al. (2019), which is shown in gray. (c) Tracks of the MW-type galaxies (red line), the MW (blue line), and the TNG MW-like galaxies (green line) in the SFR–M ⋆ plane. The yellow circles and cyan squares are the median values of the M ⋆-selected MW-type and MW progenitors at the different redshifts (indicated with the labels). The dashed gray lines indicate the SFR–M ⋆ relation of Sp14. The large gray circle is the M ⋆ and SFR of the MW estimated by Licquia & Newman (2015).
Paper: No Evolution in the Half-mass Radius of Milky Way–type Galaxies over the Last 10 Gyr
Authors: Maryam Hasheminia, Moein Mosleh, Sandro Tacchella, S. Zahra Hosseini-ShahiSavandi, Minjung Park, Rohan P. Naidu
Figure caption: Evolution of the median circularized half-mass size r 50 (panel (a)), half-mass semimajor axis size r e,SMA (panel (b)), and central stellar-mass density Σ1 (panel (c)) as a function of mass. Lines and symbols are the same as in Figure 2. The gray solid line in panel (a) indicates the size–mass relation of Mosleh et al. (2020) for SFGs at 0.3 < z < 0.7, while the dashed navy and dashed–dotted dark-red lines in panel (c) mark the Σ1–M * relation for SFGs and QGs. The small beige circles in panel (b) show the size–mass evolution when adopting the size measurements of Suess et al. (2019a). MW-type progenitor galaxies exhibit a steeper evolution in the Σ1–M * plane than SFGs, i.e., they have a faster central mass buildup than SFGs, consistent with the r 20 evolution.
Paper: Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi, Benjamin D. G. Chandran, Stuart D. Bale, Marco Velli
Figure caption: 8 hr long time interval I of Wind observations. Panels from top to bottom correspond to (a) and (b) histograms of the ϕ and θ angle, respectively, (c) the normalized radial component of the magnetic field −B  R /∣ B ∣ (blue line) and the bulk flow V (purple line), (d) the azimuthal angle ϕ (black) and the polar angle θ (green), respectively, and (e) the magnitude of the magnetic field vector ∣ B ∣ (blue) and the Alfvén speed V  A  (brown).
Paper: Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi, Benjamin D. G. Chandran, Stuart D. Bale, Marco Velli
Figure caption: Sketch describes how the radial-field component B  x /∣B∣ and the fluctuating bulk velocity Δ V  1 = −Δ B  1 and Δ V  2 = −Δ B  2 (orange vectors) add to the local mean bulk velocity  V  0 (Green vector) during the oscillation of the instantaneous magnetic field vector  B  1 and  B  2 (black vectors) around the local background magnetic field vector  B  0 for the case (a) where  B  0 is nearly radial and for case (b) where  B  0 is nearly perpendicular to the radial direction (of the bulk flow direction). Here ΔB 1 and Δ B  2 are normalized to velocity units.
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Energetics and reconnection rate during the LFP–current sheet interaction. We display the measured reconnected energy and the energy stored in the emerging high-frequency FMS waves (a). The reconnection velocity measured for different pulse amplitudes is shown in panel (b).
Paper: Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi, Benjamin D. G. Chandran, Stuart D. Bale, Marco Velli
Figure caption: 8 hr long time interval II of PSP measurements. Panels from top to bottom correspond to (a) and (b) histograms of the ϕ and θ angle, respectively, (c) the normalized radial component of the magnetic field B  R /∣ B ∣ (blue line) and the bulk flow V (purple line), (d) the azimuthal angle ϕ (black) and the polar angle θ (green), respectively, and (e) the magnitude of the magnetic field vector ∣ B ∣ (blue) and the Alfvén speed V  A  (brown).
Paper: Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi, Benjamin D. G. Chandran, Stuart D. Bale, Marco Velli
Figure caption: Interval III of Wind measurements. Panels from top to bottom correspond to (a) and (b) histograms of the ϕ and θ angle, respectively, (c) the normalized radial component of the magnetic field −B  R /∣ B ∣ (blue line) and the bulk flow V (purple line), (d) the azimuthal angle ϕ (black) and the polar angle θ (green), respectively, and (e) the magnitude of the magnetic field vector ∣ B ∣ (blue) and the Alfvén speed V  A  (brown).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Schematic impression of the simulation setup (bottom) and its global astrophysical context (top). The simulation domain mimics a segment of the striped magnetar wind, located in the vicinity of the light cylinder. An LFP emerging close to the magnetar propagates outwards and collides with a Harris-type current sheet of the striped wind. We model their subsequent interaction in a moving window, tracking the propagation of the fast pulse at the speed of light through a system of infinite length (and energy supply).
Paper: Features of Magnetic Field Switchbacks in Relation to the Local-field Geometry of Large-amplitude Alfvénic Oscillations: Wind and PSP Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Nour E. Raouafi, Benjamin D. G. Chandran, Stuart D. Bale, Marco Velli
Figure caption: Panels from top to bottom correspond to the measured bulk flow V (purple line) and the bulk flow V* reconstructed from changes in the magnetic field ΔB for intervals I, II, and III. The horizontal dashed line represents the mean bulk flow  V  0 considered for the reconstruction of V*.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Each column of panels represents a batch of 40 realizations of a halo model and initial conditions. The initial set of GC masses is taken to match the observed set of 33 GCs in Danieli et al. (2022), correcting only for continuous mass loss. The initial radial distribution is Sérsic with n = 0.61, with a half-light radius that is different for each halo model. Left column: the Stars model. Middle column: the Burkert model. Right column: the NFW model. Top row: the mean projected radius of GCs in different mass bins. The filled points are data from Danieli et al. (2022; see discussion in 3 and Figure 2). Points with error bars are simulation results including 68% confidence intervals. Horizontal orange lines show the ﹩\left\langle {r}_{\perp }\right\rangle ﹩ of the initial GC distribution (common to all mass bins). The corresponding initial Sérsic radius is R  e  = 4.5, 2.6, and 2.5 kpc for Stars, Burkert, and NFW, respectively. For comparison, the stellar body of UDG1 is best fit with R  e  ≈ 1.9 kpc, such that ﹩\left\langle {r}_{\perp }\right\rangle \approx 2.1\,\mathrm{kpc}﹩. The shaded gray region at r ⊥ < 0.5 kpc is to remind the reader that the predictions of the simulations are least robust in this area, notably because the mass in GCs may not be negligible with respect to the halo enclosed mass (see the text for more details). The dashed purple line is an adaptation of Equation (2) using ﹩{\tau }_{\mathrm{core}}^{(0)}={\tau }_{\mathrm{DF}}(r,{V}_{\mathrm{circ}}(r)){| }_{r={R}_{e}}﹩, ﹩{\left\langle {r}_{0,\perp }\right\rangle }_{\mathrm{core}}﹩ calculated using the initial GC distribution. Bottom row: the average number of GCs per mass bin, with big blue points representing the data and medium orange points the initial condition corrected for GC mass loss (by construction for this run, the initial condition is aligned with the data). The small blue points with error bars represent simulation results with the symmetric error estimate ﹩{\sigma }_{N}=\sqrt{\left\langle {N}_{\mathrm{GC}}^{2}\right\rangle -{\left\langle {N}_{\mathrm{GC}}\right\rangle }^{2}}﹩.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Red circles with numbers: circle position along the y-axis shows the average projected distance ﹩\left\langle {r}_{\perp }\right\rangle ﹩, for GCs belonging to luminosity bins (x-axis) marked by vertical dashed lines. Numbers indicate the number of GCs per bin. The luminosity bins are equispaced in log scale. We assume distance D = 26.5 Mpc. Blue circles show the unbinned data, comprised of the m  V  < 25.0 mag objects inside r < 2r eff in Figure 1. Fainter objects (with significant background contamination) are not shown here; in Appendix D we find that the faint object population yields ﹩\left\langle {r}_{\perp }\right\rangle \sim 2\div2.5\,\mathrm{kpc}﹩, consistent with the pattern of the m  V  < 25.0 mag sample.
Paper: Isotropization and Evolution of Energy-containing Eddies in Solar Wind Turbulence: Parker Solar Probe, Helios 1, ACE, WIND, and Voyager 1
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Sohom Roy, Joshua Goodwill, Francesco Pecora, Jake Jarosik, William H. Matthaeus, Tulasi N. Parashar, Riddhi Bandyopadhyay
Figure caption: Correlation lengths observed by PSP and Helios 1 (left), ACE and WIND (middle), and Voyager 1 (right), vs. heliocentric distance. (Top) Results for individual intervals. (Bottom) Binned averages with bars representing standard deviation about mean. Blue circles, red triangles, and black squares represent parallel, perpendicular, and all intervals, respectively. Helios 1 data represented by three turquoise crosses (﹩{\lambda }_{C}^{\parallel }﹩) and stars (﹩{\lambda }_{C}^{\perp }﹩) are extracted from Ruiz et al. (2011). PSP data to left and right of the vertical dashed line at 0.3 au represent 1 hr and 3 hr interval sizes, respectively. Columns at ∼1 au represent number density (darker shades = larger counts) of 1 day intervals for ACE and WIND grouped as ﹩{\lambda }_{C}^{\parallel }﹩ (left, blue) and ﹩{\lambda }_{C}^{\perp }﹩ (right, red). Statistics of these distributions are in Table 1. Power-law fits for λ  C , ﹩{\lambda }_{C}^{\parallel }﹩, and ﹩{\lambda }_{C}^{\perp }﹩ are in Table 2.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Left: reproduction of V-band data obtained in Danieli et al. (2022) using the Hubble Space Telescope WFC3/UVIS camera, containing UDG1 and a nearby field (postselection criteria described in Danieli et al. 2022). Circles represent 2r eff and 3r eff of the stellar light profile, with r eff the Sérsic radius. Right: a scatterplot of objects from the left panel, divided into magnitude bins. The magnitude bins for objects at m  V  < 25.0 mag are relatively clean from background contamination. In comparison, contamination is significant for the bin 25.0 < m  V  < 26.5 mag. In our main analysis, we primarily use the r < 2r eff data of the m  V  < 25.0 mag bins. We present a preliminary analysis of the 25.0 < m  V  < 26.5 mag bin in Appendix D, showing that the faint objects also exhibit radial clustering above the background, comparable to the stellar body.
Paper: Isotropization and Evolution of Energy-containing Eddies in Solar Wind Turbulence: Parker Solar Probe, Helios 1, ACE, WIND, and Voyager 1
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Sohom Roy, Joshua Goodwill, Francesco Pecora, Jake Jarosik, William H. Matthaeus, Tulasi N. Parashar, Riddhi Bandyopadhyay
Figure caption: Ratios of ﹩\langle {\lambda }_{C}^{\parallel }\rangle ﹩/﹩\langle {\lambda }_{C}^{\perp }\rangle ﹩ for PSP (blue circles), Helios 1 (red triangles), and ACE/WIND (black square). Points represent radially binned averages of results presented in Figure 2. The statistics of the distribution from ACE/WIND are given in Table 1. Error bars represent standard error of the mean, ﹩\sigma /\sqrt{n}﹩, where σ is standard deviation and n is number of samples. We also compute an average ratio ﹩\langle {\lambda }_{C}^{\parallel }\rangle ﹩/﹩\langle {\lambda }_{C}^{\perp }\rangle \approx 0.97﹩ over all Voyager data out to 10 au, with 0.17 standard error.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: The data from Figure 2, overlaid with the simple dynamical friction model captured by Equation (2). The results are shown with three different choices of binning in GC mass. Point size indicates the amount of GCs per bin. (The last two points on the right should overlap; their position was slightly displaced for clarity.)
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: An example where the observed GC mass function is slightly modified: the most-massive GC, of mass ∼15 × 105 M ⊙, is traded in the initial GC mass function by one GC with half the mass, and two GCs with one-quarter of the mass. This shows how this massive GC may have been the result of mergers. Additionally, three light GCs with m ⋆ ∼ 1.75 × 105 M ⊙ were added to compensate for loss due to the selection of data r ⊥ < 3.8 kpc. Indeed with this addition the simulation is a better fit to the data in the first data point.
Paper: Dynamical Friction in Globular Cluster-rich Ultra-diffuse Galaxies: The Case of NGC5846-UDG1
Authors: Nitsan Bar, Shany Danieli, Kfir Blum
Figure caption: Properties of mass models that we use. Top left: mass density as a function of radius. Top right: expected line-of-sight velocity dispersion of the observed distribution of stars in Danieli et al. (2022) assuming isotropic velocity dispersion. Bottom right: the dynamical friction time evaluated with the velocity of a circular orbit for m ⋆ = 5 × 105 M ⊙, with Coulomb logarithms as described in Section 4.1.1. Bottom left: the enclosed mass of different models with a rough comparison to GCs mass profile, deprojected via the approximation r = 1.25 × r ⊥ (see Equation (C3)).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Dynamic spectra and power for different pulse amplitudes (top two rows; Section 3.2.2), L  y  extensions (bottom leftmost panels; Section 3.2.1), and cooling parameters (bottom right panels; Section 3.2.3). The parameters of each model are given in the respective power plots on top of the dynamic spectra. Gray contours stacked in the spectra indicate differences by a factor of 10; red contours denote 90% of the maximum energy. The frequency is normalized to the peak frequency ﹩{\omega }_{\max }﹩ of the reference case with ﹩{ \mathcal A }=20﹩, κ ≈ 30, and ﹩{ \mathcal C }=\infty ﹩. 1D outlines on top of the spectra denote the corresponding power of the fast-wave signal (black solid line for total energy, black dotted line for the ﹩\omega /{\omega }_{\max }\in [1,2]﹩ band).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Selected representative plasmoids extracted from the simulation data at t = 4t p for different cooling strengths (as indicated). We analyze the particle Lorentz factor measured in the rest frame of the pulse plasma (panel a, top row) and the plasma density (panel a, bottom row). In panel a, we indicate locations where ﹩n^{\prime} /{n}_{0}={10}^{2}﹩ by a black contour in each panel, and locations with ﹩B^{\prime} /{B}_{{\rm{u}}}=10﹩ by cyan contours. The inset colored bars (panel a, bottom row) denote the size of the noncooled reference plasmoid (magenta), and the extent of each plasmoid (green), respectively. The size of characteristic plasmoids decreases with increasing strength of synchrotron cooling. Panels (b) and (c) show 1D outlines of selected quantities along the y = 10d u coordinate (see panel a). First, we compare the magnetic field strength for different cooling strengths (b). The maximum magnetic field strength scales with approximately ﹩{{ \mathcal C }}^{-1/2}﹩. Finally, we repeat the comparison for the pressure term ﹩\left\langle \gamma \right\rangle n^{\prime} ﹩ in (c) and find a scaling with approximately ﹩{{ \mathcal C }}^{-1}﹩.
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Comparison of dynamic spectra for a varying supply of upstream flux. Panel (a) shows an ﹩{ \mathcal A }=20﹩ reference case for a system of infinite length (﹩{ \mathcal F }\gt 1﹩, see Figure 5). Panel (b) shows an adaptation of the standard setup to a finite flux reservoir (﹩{ \mathcal F }=0.5﹩; Appendix E). We provide an animation of this simulation as supplementary material (Mahlmann et al. 2022).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Illustration of different macroparticle merging algorithms at the example of an initial charge-neutral particle cloud with trajectories that intersect in one cell, triggering merger events. We display the merging particles (magenta colored dots) as well as the local charge density ﹩| \mathrm{div}{\boldsymbol{E}}| ﹩ (blue color density) at three different times. After the particle cloud approached the common intersection cell (a) and particles are merged consecutively (b), different numerical techniques show different qualities of conserving charge neutrality (c)/(d)/(e). Merged superparticles can be randomly positioned (c), positioned at the center of mass (COC) of precursor particles (d), or injected at the COC with a correction of their displacement in the current (e).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: High-frequency FMS wave spectra with powers binned along the propagation direction (k  x ) for different amplitudes ﹩{ \mathcal A }﹩ (panel a, Section 3.2.2), and different cooling parameters ﹩{ \mathcal C }﹩ (panel b, Section 3.2.3). The inset in (a) shows the peak energy as a function of wave amplitude. The vertical lines in (b) indicate an inversely proportional scaling of the frequency with ﹩{ \mathcal C }﹩ (see Equations (10) and (23)).
Paper: Electromagnetic Fireworks: Fast Radio Bursts from Rapid Reconnection in the Compressed Magnetar Wind
Authors: J. F. Mahlmann, A. A. Philippov, A. Levinson, A. Spitkovsky, H. Hakobyan
Figure caption: Time and length scales of the LFP–current sheet interaction in 1D-PIC simulations (using a setup as described in Section 3.1). We verify the scaling derived for the LFP–current sheet interaction time (panel a, see Equation (5)) as well as the layer thickness (panel b, see Equation (15)). We show the validity of the assumption ﹩a^{\prime} \gt {\rho }_{{\rm{u}}}{\sigma }_{{\rm{u}}}﹩ that implies the presence of sufficient charge carriers in the reconnection layer.
Paper: Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath
Authors: Yingjie Zhang, Tianran Sun, Chi Wang, Li Ji, Jennifer. A. Carter, Steve Sembay, Dimitra Koutroumpa, Ying D. Liu, Guiyun Liang, Wenhao Liu, Wei Sun, Xiaowei Zhao
Figure caption: Solar wind data: (a) proton temperature and expected temperature (red), (b) proton density and velocity (red), (c) ratio of O7+ to O6+, and (d) average iron charge states. XMM-Newton data: (e), (f), (g) 2.5–8.5 keV light curves and GTIs (red), (h), (i) orbital positions during GTIs (solid lines with arrow), line of sight (dashed lines), and calculated average positions for magnetopause and bow shock (Shue et al. 1997; Khan & Cowley 1999) (gray lines). Black arrows: interplanetary shock. Vertical lines: GTI boundaries (blue) and estimated ICME leading edge (orange dashed).
Paper: Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath
Authors: Yingjie Zhang, Tianran Sun, Chi Wang, Li Ji, Jennifer. A. Carter, Steve Sembay, Dimitra Koutroumpa, Ying D. Liu, Guiyun Liang, Wenhao Liu, Wei Sun, Xiaowei Zhao
Figure caption: A schematic diagram (not to scale) of magnetospheric SWCX soft X-ray emissions during the successive impact of an ICME-driven sheath (top) and ICME (bottom) on Earth. Magnetospheric SWCX emissions (bright magenta) were observed remotely by XMM-Newton, for which the line of sight is represented by dotted lines. Solar wind protons (small white spheres) and high-state ions (colored spheres) were observed in situ by ACE.
Paper: Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath
Authors: Yingjie Zhang, Tianran Sun, Chi Wang, Li Ji, Jennifer. A. Carter, Steve Sembay, Dimitra Koutroumpa, Ying D. Liu, Guiyun Liang, Wenhao Liu, Wei Sun, Xiaowei Zhao
Figure caption: Top: (a), (b), (c) fitted X-ray flux for SWCX emissions measured in units of 10−8 erg cm−2 s−1 sr−1. Half-hourly average solar wind proton data: (d) flux, (e) density, and (f) velocity. Vertical orange dashed line: estimated ICME leading edge. Bottom: SWCX spectral model fitted to the background-subtracted pn spectrum (similar for MOS, not shown here), extracted from the interval centered at 7:00 UT (left) and 10:00 UT (right). The ion emission lines are represented by Gaussian lines, where N, Fe, and Si are in black. The cosmic background is represented by the black curve, and the sum of all models is represented by the red curve. The best-fit reduced chi square is 1.054 (left) and 1.226 (right).
Paper: Solar Wind Charge Exchange Soft X-Ray Emissions in the Magnetosphere during an Interplanetary Coronal Mass Ejection Compared to Its Driven Sheath
Authors: Yingjie Zhang, Tianran Sun, Chi Wang, Li Ji, Jennifer. A. Carter, Steve Sembay, Dimitra Koutroumpa, Ying D. Liu, Guiyun Liang, Wenhao Liu, Wei Sun, Xiaowei Zhao
Figure caption: Left panel: ratios of each ion to oxygen ions (bottom) and ratios of oxygen ions to solar wind protons (top) as measured by ACE. Middle panel: calculated alphas for each ion (bottom) and sum of calculated alphas (top). Right panel: fitted X-ray fluxes for each ion line emission (bottom) and for the total SWCX emission (top). Vertical orange dashed line: estimated ICME leading edge.